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## (from tabmap V6.0 (2016-08-18)) 2024-05-21T12:51:56 #--------------------------------------------------------------------------- #-- B/gcvs General Catalogue of Variable Stars (Samus+, 2007-2017) #-------------------------------------------------------------------------- #---Table: B/gcvs/./gcvs_rem.dat GCVS remarks (17431 records) # GCVS A12 --- Variable star designation # Text A67 --- Text of note -------------------------------------------------------------------------------- GCVS |Text ------------|------------------------------------------------------------------- R And |SiO maser. S And |SN (NGC 224). W And |SiO maser. Z And |Outbursts, average cycle 8400d. Porb = 758.8d, it reveals itself in Z And |photometry during the low state. A quasi-period, P1, about 656d is Z And |present during the outbursts. The beat period between Porb and P1, Z And |about 5500d, is also found in the photometric data. RS And |H2O maser. RT And |P varies, current elements are given. RU And |P varies strongly. RX And |Porb = 0.209893d. RY And |OH, H2O maser. SS And |P2 = 650d, P3 = 3800d. SU And |VB A (B 12.77m, F0V:, 15"). SV And |SiO maser. SW And |[Fe/H] = -0.24. P varies, current elements are given. According to SW And |[N0037], Max = 2435249.25744 + 0.442270491d*E - 1.032 x SW And |10^{-10}E*E. SY And |d = 0.027P. TW And |P varies, current elements are given. d = 0.020P. P varies, current TW And |elements are given. TX And |Recent observations in the AAVSO database suggest type LB. UU And |The depth of MinII is 0.2m R. P varies, current elements are given. VX And |The mean brightness varies with P = 904d. WW And |The depth of MinII is 0.16m. WX And |d = 0.03P. P varies, current elements are given. WY And |[Fe/H] = -1.0. WZ And |P varies, current elements are given. Min II 11.61. XX And |P varies, current elements are given. [Fe/H] = -1.94. Blazhko XX And |effect with a 36-day period [03111]. XY And |[Fe/H] = -0.92. XZ And |P varies in a complex manner, current elements are given. ZZ And |[Fe/H] = -1.58. AB And |P varies, current elements are given. The light curve shape varies. AC And |A triple-mode pulsator. The table gives the light elements for the AC And |fundamental-mode pulsations. First overtone: Max = 2428009.45 + AC And |0.5251342d*E; second overtone: Max = 2428009.69 + 0.4210572d*E. AC And |[Fe/H] = -1.16. AD And |The depth of Min II is 0.58m. P varies, current elements are given. AE And |In the M31 galaxy. AF And |In the M31 galaxy. AG And |The data in [75119] refer to a different star. The data in [08296] AG And |probably refer to a different star. AM And |VB A (B 14.7m 17" sf). AQ And |Secondary period 346d. AR And |Porb = 0.16302d. AT And |[Fe/H] = -1.18. AW And |Identified by its number from the Harvard - Groningen AW And |Durchmusterung quoted in [01992], in 1 degree of declination from AW And |the position published by the discoverer. Not red, apparently does AW And |not vary in modern automatic surveys. BD And |P varies, current elements are given. BK And |[Fe/H] = -0.08. BL And |The depth of Min II is 0.32m. BU And |H2O maser. BX And |ADS 1671 A (B 10.86m, 20", 59{deg}). P varies, current elements are BX And |given. CC And |Multiperiodic. CE And |H2O maser. CG And |The elements in the Table correspond to maximum U-band light. CG And |During some seasons, short-period variations with a period about CG And |125 min and an amplitude up to several hundredths of a magnitude CG And |were observed. In 1973, periods of 0.09325d and 0.06737d were CG And |detected. CI And |[Fe/H] = -0.69. CN And |P varies, quadratic term -9.8*10^{-11}*E*E. CO And |d = 0.06P:. CP And |d = 0.01P:. P varies? CU And |d > 0.034P. P varies? DI And |An unusual light curve with a secondary maximum. DL And |In the region of the open cluster NGC 7686. DQ And |[M/H] = 0.00. DR And |[Fe/H] = -1.48. P varies, current elements are given. Blazhko DR And |effect with a period about 57d is possible [N0053]. DS And |d = 0.04P. In the open cluster NGC 752. dII = 0.07P. DU And |[Fe/H] = -2.11. DX And |Porb = 0.440502d. EG And |Porb = 482.57d. The light curve is modulated with a double wave EG And |during the orbital period. EL And |A twice shorter period is possible. EP And |The depth of Min II is 0.60m. P varies, current elements are given. ET And |SB1, Porb = 48.304d. EU And |H2O maser. EX And |No evidence for the secondary minimum being displaced, as claimed EX And |in [04335], in recent CCD data. P varies? EY And |OH, H2O, SiO maser. FF And |VB A (B 10.53m V, 7", 295{deg}). SB2, Porb = 2.170304d. BY-type FF And |variations: 10.35m - 10.42m V outside flares, P = 2.170d [5230]. FL And |d = 0.02P. FO And |Porb = 0.07161d. Superhumps: P = 0.07411d [N0067]. FV And |P varies? GK And |P varies? GN And |ADS 409 A (B 13.1m, 2", 6{deg}, 1948). GP And |VB A (B 12.50m, 11"). P varies, quadratic term +5.20d*10^{-13}E*E. GQ And |ADS 246 B (A = GX And). 11.04m - 11.10m V outside flares [08313]. GX And |ADS 246 A (B = GQ And). GY And |SB1, P = 272.88d. GZ And |ADS 1693 A (B 11.13m, 8", 31{deg}, 1894; C 11.91m, 14", 200{deg}, GZ And |1908; D 12.65m, 24", 285{deg}, 1908). P varies, current elements GZ And |are given. HN And |SB1, P = 106.3334d. From Hipparcos data, a photometric period of HN And |1.7237d (instead of 69.92d) was suggested in [N0078]. However, it HN And |does not represent the observations from [06992], where the derived HN And |period was 69.5d. HR And |d = 0.05P. HS And |P varies, current elements are given. HT And |In the region of the M 31 galaxy. HY And |In the region of the M 31 galaxy. HZ And |P > 100d. Red. IK And |In the region of the M 31 galaxy. IL And |d = 0.02P. IO And |In the region of the M 31 galaxy. IP And |d = 0.02P:. KM And |According to [69005], cst, 14.8m pg. KP And |The depth of Min II is 0.1m R. KV And |Superhumps: P = 0.07434d [N0087]. KX And |SB2 (Porb = 38.908d). Porb reveals itself in seasonal light curves. KZ And |ADS 16557 B (A 7.2m; B 16", 256{deg}, 1984). SB2, Porb = 3.032867d. LL And |Porb = 0.055055d. LM And |VB (QY And 14" np). LN And |ADS 16472 (B A1V, 9.88m, 7", 40 {deg}). LO And |P varies, current elements are given. LQ And |SB1, Porb = 7.413d. LR And |Epoch of Max is given. P varies, quadratic term +3.379*10^{-9}*E*E. LS And |In the region of the M 31 galaxy. LT And |In the region of the M 31 galaxy. LV And |[Fe/H] = -1.55. MP And |[Fe/H] = -1.62. MR And |[Fe/H] = -1.26. MU And |[Fe/H] = -1.57. MV And |[Fe/H] = -1.78. MX And |[Fe/H] = -1.50. MY And |[Fe/H] = -1.32. NN And |[Fe/H] = -1.35. NO And |[Fe/H] = -1.67. NQ And |[Fe/H] = -1.38. OR And |Porb = 0.1359d. OT And |MinII - MinI = 0.52P. OV And |ADS 284 B (A Sp G, 7.5" p; several additional fainter companions). PQ And |Rare outbursts in 1938, 1967, 1988. Porb = 0.071d. PT And |In the region of the M 31 galaxy. PU And |In the region of the M 31 galaxy. PX And |The elements are for eclipses. The amplitude of the eclipses is PX And |about 0.5m. PY And |SB, P = 399.6d. QR And |The elements are for eclipses. QU And |SB1. QW And |The depth of MinII is 0.44m. QX And |In the open cluster NGC 752. P varies? QY And |VB (LM And 14" sf). Variations only due to LM And are seen in QY And |ROTSE/NSVS data for combined light. QZ And |VB A (B 14" np). V0336 And |VB A (B 20" sp). V0337 And |VB A (B 14.0m, 15" nf). V0342 And |VB (A 7.86m, B 9.21m, 5", 82{deg}, 1991). V0348 And |ADS 197 (B 7.5m V, 0.2", 42{deg}, 1957). V0355 And |ADS 616 (A 7.92m Hp, F5; B 9.08m Hp, 1.4", 5.5{deg}, 1991). V0361 And |ADS 948 (A 7.84m, F0; B 11.65m, 3", 249{deg}, 1991). V0369 And |VB (9.5m V + 9.5m V, 0".1, 128{deg}, 1986.9). V0371 And |VB (ADS 1613AB: A 8.7m V, B 8.9m V, 0.2". 358{deg}, 1997; C 11.5m V0371 And |V, 0.8", 261{deg}, 1958). V0392 And |VB (A 9.3m Hp; B 11.5m Hp, 2", 75{deg}, 1991). V0393 And |P = 0.223880d is suggested in [HIP], the light curve has a large V0393 And |scatter. V0395 And |ADS 16965 (A 7.6m V; B 9.8m V, 6", 103{deg}, 1991). V0413 And |d = 0.01P. ADS 17087 (B 12.5m V, 5", 181{deg}, 1907). V0419 And |ADS 1672 (B 10.0m V, 6", 254{deg}, 1991). V0420 And |VB A (B 15.0m pg, 12" np). V0428 And |SB1, Porb = 576d. V0429 And |Multiperiodic, P1 = 195s. V0446 And |A chromospherically active giant, photometric variations with the V0446 And |rotation period. V0455 And |A single major outburst in September, 2007. Superhumps were V0455 And |observed. Porb = 0.05631d. V0466 And |A single major outburst in September, 2008. Early superhumps: P = V0466 And |0.056383d; ordinary superhumps: P = 0.05713d; late superhumps: P = V0466 And |0.056d. V0470 And |P2 = 1.93570d. V0478 And |Multiperiodic. V0484 And |Catalina data do not completely confirm the light elements [00001]. V0496 And |P varies, current elements are tabulated. V0498 And |VB A (A 10.04mV; B 10.15mV, 22", 139{deg}, 2005). Combined V0498 And |brightness is tabulated. V0500 And |A single major outburst in November, 2008. Superhumps were V0500 And |observed. V0515 And |P2 = 0.0056553d. V0521 And |Multiperiodic. V0522 And |MinII - MinI = 0.484P. V0529 And |Multiperiodic. The largest-amplitude {Delta} Scuti period is V0529 And |0.11876d. VB A (B 13.4mV, 16", 166{deg}, 1998). V0560 And |O'Connell effect. V0572 And |Early superhumps: P = 0.054868d; ordinary superhumps: P = V0572 And |0.055544d. V0604 And |Multiple. The coordinates in [80598] are wrong. V0704 And |Porb = 0.154d. V0735 And |Magnitudes in the Table can be influenced by surrounding bright V0735 And |stars. V0736 And |VB AB (AB 11.03mV; 0.1", 115{deg}, 1973; A and B estimated equally V0736 And |bright). Magnitudes in the Table can be influenced by a 10.60mV V0736 And |star BD +36 0159 (50", 252{deg}, 1999). V0744 And |Porb = 0.02608d. V0751 And |A twice shorter period is not excluded. V0762 And |Studied in [81025] (SAVS 023548+491758) but erroneously identified V0762 And |with GSC 03303-01008. V0769 And |VB B (A 16.8mV, B 16.9mV; AB 6", 37{deg}, 1998). The magnitudes in V0769 And |the Table were influenced with the companion. V0770 And |Multiperiodic. V0782 And |MinII - MinI = 0.383P. V0784 And |P1 is presented in the Table. P0 = 0.534895d; P1/P0 = 0.7465. V0787 And |P1 is presented in the Table. P0 = 0.542396d; P1/P0 = 0.7465. V0788 And |P1 is presented in the Table. P0 = 0.529664d; P1/P0 = 0.7461. V0796 And |P1 is presented in the Table. P0 = 0.470490d; P1/P0 = 0.7442. V0797 And |Additional non-radial pulsation, Pnr = 0.18776d. P1 is presented in V0797 And |the Table; Pnr/P1 = 0.9162. V0799 And |VB (A 10.3m; B 10.9m, 6", 320{deg}, 2016). The magnitudes in the V0799 And |Table are for combined brightness. V0800 And |Biperiodic, P2 = 71.2d. V0806 And |MinII - MinI = 0.494P. V0807 And |d = 0.08P. The elements in the table are for planet transits. V0807 And |Superposed DSCT oscillations: P = 0.0476d [023]. V0811 And |VB A (15.3mG; B 16.9mG, 11", 44{deg}, 2000). V0812 And |Blazhko effect? P varies? V0819 And |Multiperiodic, other periods are 0.0914017d and 0.0849941d. alf And |SB2 (P = 96.7041d). VB (interferometric, a = 0.024"). Photometric alf And |variability could not be confirmed in [N0111]. zet And |For regular ellipsoidal variations, the depth of minima are about zet And |0.07m. lam And |The tabulated elements are for brightness minima in 1996 - 2002. lam And |SB1 (P = 20.5212d). omi And |Multiple (AB 0.3", period much longer than 100d; Aa 0.05"; B SB2, P omi And |= 33.08d). Several shell events were observed. Periodic variations omi And |with varying amplitude (up to 0.1m): double wave, MinI = omi And |2429981.250 + 1.571272d*E [N0114]. A number of different omi And |photometric and spectroscopic periods were also reported. T Ant |[A/H] = -0.0. P var, nonlinear elements: Max = 2436120.756 + T Ant |5.897915d*E + 4.80d*10^{-8}E^2 [N0027]. V Ant |OH, H_2O, SiO maser. SZ Ant |From photometry in [N0002], about 12.3m V, const? [00001]. TU Ant |From photometry in [N0002], about 10.6m V, const? [00001]. WY Ant |[Fe/H] = -1.48. P var, nonlinear elements: Max = 2439139.40 + WY Ant |0.574330174d*E + 4.820d*10^{-10}E^2 [N0029]. AG Ant |[Fe/H] = -4.8. A post-AGB star. SB1. Brightness variations with the AG Ant |orbital period probably due to variations of circumstellar AG Ant |extinction. AI Ant |Slow variations with Prot (see Table), oscillations with P about 15 AI Ant |minutes, several frequencies. BU Ant |VB A (B 11.72m, 27", 36{deg}, 2000). BV Ant |MinII - MinI = 0.60P. BW Ant |Porb = 0.0303d. BX Ant |VB B (A 10.9m; AB 27", 124{deg}, 1999). In the TWA association. BY Ant |VB B (A = NSV 04876, 5.56m, B9.5V; AB 11", 226{deg}, 1999). BZ Ant |VB B (A 5.56m, NSV 04876; AB 11", 226{deg}, 1999). CE Ant |In the TWA association. CH Ant |Multiperiodic, 4 harmonics. P1 is given in the Table. CI Ant |VB A (B 13.1m, 1", 306{deg}, 1991). CN Ant |P strongly varies. The elements in the Table are for JD 2453569 - CN Ant |2454298. RS Aps |VB A (A 15.1mV; B 15.5mV, 6", 139{deg}, 1999). TY Aps |Blazhko effect? [Fe/H] = -0.95. UW Aps |VB A (A 15.4mV, B 15.7mV; AB 9", 147{deg}, 2000). VX Aps |[Fe/H] = -1.44. YZ Aps |VB (14.2m, 14.6m, 8", 207{deg}, 2000). The southern component YZ Aps |varies? AB Aps |[Fe/H] = -1.30. BE Aps |OH maser. BM Aps |VB A (B 12.2mR, 18", 137{deg}, 2000). The tabulated magnitude in BM Aps |maximum is influenced by the companion. BS Aps |[Fe/H] = -1.33. CE Aps |VB A (B 13m, 14", 125{deg}; C 14m, 199{deg}, 2000). CK Aps |[Fe/H] = -1.49. CP Aps |VB A (B 15.2m, 9", 289{deg}, 2000). It is not quite clear which of CP Aps |the components varies. CZ Aps |SiO maser. DF Aps |VB A (B 15.5mpg, 14", 308{deg}, 2000). DI Aps |Blazhko effect? [Fe/H] = -1.60. DZ Aps |Blazhko effect. EL Aps |[Fe/H] = -1.56. ER Aps |[Fe/H] = -1.39. EX Aps |[Fe/H] = -0.81. GO Aps |Type RR is not excluded. IP Aps |VB B (A 14.5mpg, B 14.7mpg; AB 10", 140{deg}, 2000). IZ Aps |VB B (A 15.4mpg, B 16.4mpg; AB 8", 300{deg}, 2000). LM Aps |Type RV is also possible. LO Aps |O'Connell effect. LU Aps |[Fe/H] = -2.06. MY Aps |L19-2. Multiperiodic, main stable modes: 192.6s and 113.8s. OZ Aps |A twice longer period is not excluded. PQ Aps |In the region of the globular cluster IC 4499; cluster non-member. PV Aps |MinII - MinI = 0.75P. QX Aps |Superposed variations with P = 74d: and an amplitude about 1m. V0347 Aps |VB A (A 13.5m; B 15.1m, 10", 79{deg}, 2000; C 5", 321{deg}, 2000). V0347 Aps |The tabulated amplitude was affected by the companions. V0367 Aps |VB B (A 11.3m; AB 8", 58{deg}, 2000). V0380 Aps |VB (several companions). V0390 Aps |Distorsion wave: P = 2.84455d. V0393 Aps |Period varies. V0394 Aps |VB A (B 7", 340{deg}, 2000). V0395 Aps |The period in the Table is that of the first overtone (P1). V0395 Aps |Fundamental mode: P0 = 0.472647d. P1/P0 = 0.74445. V0398 Aps |According to [g0009], the star is a second-overtone pulsator. V0401 Aps |P varies, the period in the Table is valid for 1990 - 1994. V0403 Aps |The period in the Table is that of the first overtone (P1). V0403 Aps |Fundamental mode: P0 = 0.477591d. P1/P0 = 0.744412. V0404 Aps |The period in the Table is that of the first overtone (P1). V0404 Aps |Fundamental mode: P0 = 0.480751d. P1/P0 = 0.74410. V0405 Aps |Blazhko effect. V0410 Aps |The period in the Table is that of the first overtone (P1). V0410 Aps |Fundamental mode: P0 = 0.473375d. P1/P0 = 0.74416. V0419 Aps |According to [g0010], the star is a second-overtone pulsator. V0419 Aps |According to [g0009], the star is a second-overtone pulsator. V0421 Aps |The period in the Table is that of the first overtone (P1). V0421 Aps |Fundamental mode: P0 = 0.496065d. P1/P0 = 0.74449. V0426 Aps |Blazhko effect? V0431 Aps |The period in the Table is that of the first overtone (P1). V0431 Aps |Fundamental mode: P0 = 0.48834d. P1/P0 = 0.74434. V0432 Aps |The period in the Table is that of the first overtone (P1). V0432 Aps |Fundamental mode: P0 = 0.474642d. P1/P0 = 0.74414. V0440 Aps |The coordinates in the Table are uncertain. V0444 Aps |The coordinates in the Table are uncertain. V0445 Aps |The period in the Table is that of the first overtone (P1). V0445 Aps |Fundamental mode: P0 = 0.480528d. P1/P0 = 0.74440. V0446 Aps |The period in the Table is that of the first overtone (P1). V0446 Aps |Fundamental mode: P0 = 0.486080d. P1/P0 = 0.74420. V0447 Aps |According to [g0009], the star can be a double-mode pulsator with a V0447 Aps |low-amplitude fundamental mode. V0448 Aps |The period in the Table is that of the first overtone (P1). V0448 Aps |Fundamental mode: P0 = 0.473993d. P1/P0 = 0.74424. V0449 Aps |The period in the Table is that of the first overtone (P1). P1 = V0449 Aps |0.358943d is equally possible. The fundamental-mode period was not V0449 Aps |determined in [g0009]. V0454 Aps |The coordinates in the Table are uncertain. V0458 Aps |According to [g0009], the star is a second-overtone pulsator. V0461 Aps |The period in the Table is that of the first overtone (P1). V0461 Aps |Fundamental mode: P0 = 0.477109d. P1/P0 = 0.74434. V0463 Aps |The period in the Table is that of the first overtone (P1). V0463 Aps |Fundamental mode: P0 = 0.480001d. P1/P0 = 0.74434. V0466 Aps |The period in the Table is that of the first overtone (P1). V0466 Aps |Fundamental mode: P0 = 0.474776d. P1/P0 = 0.74424. V0469 Aps |Blended; the coordinates in the Table are uncertain. V0470 Aps |The period in the Table is that of the first overtone (P1). V0470 Aps |Fundamental mode: P0 = 0.493508d. P1/P0 = 0.74446. V0483 Aps |The period in the Table is that of the first overtone (P1). V0483 Aps |Fundamental mode: P0 = 0.485225d. P1/P0 = 0.74501. V0488 Aps |The period in the Table is that of the first overtone (P1). V0488 Aps |Fundamental mode: P0 = 0.482485d. P1/P0 = 0.74431. V0494 Aps |Cluster non-member? V0496 Aps |P varies? V0498 Aps |P varies? V0504 Aps |P varies? [g0001]. kap 1 Aps |SB. VB A (B 11.27m, 27", 255{deg}, 2000). R Aqr |P varies, current elements are given. SiO, OH, H2O maser. Porb = 44 R Aqr |years? In a nebula, has a jet. During certain time intervals R Aqr |several years long, too faint maxima and/or too bright minima, with R Aqr |the total range within two magnitudes. V Aqr |H2O maser. Biperiodic, P1 is given in the Table, P0 = 689d. W Aqr |SiO maser. RX Aqr |H2O maser. RY Aqr |P varies, current elements are given. ADS 14862 A (B 12.65m, 4", RY Aqr |238{deg}, 1899). ST Aqr |P varies, current elements are given. SU Aqr |ADS 16318 A (B 10.7m, 5", 143{deg}, 1926). The range given is for SU Aqr |the combined brightness. SW Aqr |[Fe/H] = -1.63. SX Aqr |[Fe/H] = -1.87. TT Aqr |VB A (B 15.0m, 3", 135{deg}, 1830). TZ Aqr |[Fe/H] = -1.24. UU Aqr |The elements are for eclipses, about 1.3m V deep. Strong nova-like UU Aqr |variations (see [N0116]). VY Aqr |Rare outbursts. Porb = 0.06309d. XX Aqr |OH maser. XZ Aqr |P varies, current elements are given. The depth of MinII is about XZ Aqr |0.2m V. YZ Aqr |[Fe/H] = -1.55. AA Aqr |[Fe/H] = -2.09. AE Aqr |Porb = 0.4116556d. Short flares, flickering. Ellipsoidal variations AE Aqr |with Porb and an amplitude of 0.3m V [N0118]. Optical oscillations AE Aqr |with P = 33.076737s [08675] and an amplitude up to 0.02m are AE Aqr |considered the spin period of the white dwarf, a twice shorter AE Aqr |period was also reported. AX Aqr |[Fe/H] = -1.88. P varies, current elements are given. BB Aqr |[Fe/H] = -1.55. BG Aqr |[Fe/H] = -1.51. BH Aqr |[Fe/H] = -1.80. P varies? BN Aqr |[Fe/H] = -1.33. P varies, current elements are given. BO Aqr |[Fe/H] = -1.80. P varies? Current elements are given. BQ Aqr |d = 0.05P:. P varies? BR Aqr |[Fe/H] = -0.74. P varies? BS Aqr |P varies? Current elements are given. BT Aqr |[Fe/H] = -0.29. P varies, current elements are given. BV Aqr |[Fe/H] = -1.18. P varies? BW Aqr |DII = 0.06P, Min II - Min I = 0.478P (1983. Apsidal motion. BX Aqr |P varies, current elements are given. CF Aqr |[Fe/H] = -1.03. CH Aqr |[Fe/H] = -1.61. CP Aqr |[Fe/H] = -0.77. CV Aqr |Minor planet (52) Europa. CX Aqr |P varies, current elements are given. CY Aqr |[Fe/H] = -1.65. P varies, current elements are given. DD Aqr |P varies, current elements are given. DN Aqr |[Fe/H] = -1.66. DO Aqr |P varies. DS Aqr |[Fe/H] = -1.1. DU Aqr |The minor planet (57) Mnemosyne. The data in [00797] must refer to DU Aqr |another star. DV Aqr |A shell spectral episode was reported in [08062]. DX Aqr |ADS 15562 B (A 7.36m, K0III; B 4.0", 332{deg}, 1991). The range in DX Aqr |the Table is for combined brightness. EP Aqr |SiO, H2O maser. EZ Aqr |VB (AB a = 0.36", P = 2.20 years; A SB, P = 3.786516d). BY-type EZ Aqr |variations: Prot is about 4d [N0120]. FF Aqr |d = 0.059P. The amplitude of the distortion wave is 0.22m U. FG Aqr |VB A (B = NSV 14102, 8", 212{deg}, 1982.66). FI Aqr |P = 4.659d or 4.719d not excluded. FK Aqr |BDS 11854 A (B = FL Aqr, 24", 352{deg}, 1966). SB2 (P = 4.08322d). FL Aqr |BDS 11854 B (A = FK Aqr; B 24", 352{deg}, 1966). FO Aqr |Brightness variations reveal Porb (see Table) and Pspin = 0.014519d FO Aqr |(the spin period varies). FR Aqr |VB A (B 16.68m V, white dwarf, 14", 311{deg}, 1946). FU Aqr |Type EW with twice longer period is also possible. FV Aqr |[Fe/H] = -2.8. FX Aqr |Blazhko effect? GK Aqr |P varies, current elements are given. GR Aqr |P = 0.675601d is also possible. GS Aqr |According to [68018], P = 0.4604185d. GV Aqr |According to [N0002], P = 0.20259d. HH Aqr |Blazhko effect, P(Bl) = 68.7d ? HI Aqr |VB (a = 0.077", Porb = 19.25 yr). SB2 (P = 3.429616d). HK Aqr |Flare amplitude up to 0.6m U. HL Aqr |Rapid small-amplitude oscillations: P = 39.2s. HM Aqr |Very unusual, the depth of minima varies strongly. HV Aqr |The X-ray source 1RXS J212125.1-030936. VB A (B 5", 321{deg}, HV Aqr |1992). The light curve shape varies. HZ Aqr |Porb = 3.7569d. KQ Aqr |The X-ray source 1RXS J221038.4-240120. KV Aqr |VB AB (A 7.24m; B 8.23m, 7", 158{deg}, 1991). One deep fading on a KV Aqr |brightening trend. LL Aqr |The phase of MinII is 0.32. LY Aqr |A binary millisecond pulsar with radio eclipses. LZ Aqr |Orbital-period modulation during the bright stage: Min = LZ Aqr |2451022.782 + 0.24820d * E [N0131]. OV Aqr |A twice longer period is not excluded. QT Aqr |Porb = 0.074665d. QU Aqr |Porb = 0.08330d. QV Aqr |VB A (B 19.1mg, 4", 228{deg}, 2001). Porb = 0.07196d. QW Aqr |The first-overtone period is tabulated. P0 = 0.47722d, A1/A0 = 1.3. QZ Aqr |Superhumps: P = 0.064593d? [80233]. V0349 Aqr |Pspin is tabulated. Porb = 0.1344d. V0354 Aqr |Blazhko effect, P = 181.20d. V0357 Aqr |P varies. dP/dt = -0.37 x 10^(-5) d/yr. V0358 Aqr |Epoch of minimum is tabulated. High states: 15.7 - 16.8m; low V0358 Aqr |states: 16.5 - 17.5m. V0360 Aqr |Blazhko effect, P = 54.52d. V0362 Aqr |Light elements for eclipses are tabulated. DSCTC: P = 0.038213d, V0362 Aqr |{Delta} m = 0.03m. V0366 Aqr |Multiperiodic. V0367 Aqr |Double-mode pulsations. First overtone: see the Table. P0 = V0367 Aqr |0.485897d. P1/P0 = 0.7432. V0368 Aqr |P1 is presented in the Table. P0 =0.481835d. P1/P0=0.7443. V0369 Aqr |P1 is presented in the Table. P0 = 0.590458. P1/P0 = 0.7446. V0370 Aqr |P1 is presented in the Table. Fundamental mode: Max = 2454700.685 + V0370 Aqr |0.532434d x E. P1/P0 = 0.7469. V0371 Aqr |Double-mode pulsation. The period in the Table is for the V0371 Aqr |fundamental mode. P1 = 0.0624379d. P1/P0 = 0.7748. V0373 Aqr |Double-mode pulsation. The period in the Table is for the first V0373 Aqr |overtone. P0 = 0.554570d. P1/P0 = 0.7456. V0375 Aqr |Double-mode pulsation. The period in the Table is for the first V0375 Aqr |overtone. P0 = 0.479278d. P1/P0 = 0.7443. V0379 Aqr |Double-mode pulsation. The period in the Table is for the first V0379 Aqr |overtone. P0 = 0.530200d. P1/P0 = 0.7459. V0380 Aqr |Double-mode pulsation. The period in the Table is for the first V0380 Aqr |overtone. P0 = 0.4900d. P1/P0 = 0.7429. V0381 Aqr |Period varies. V0383 Aqr |Period varies strongly. V0384 Aqr |Blazhko effect? V0387 Aqr |Blazhko effect? V0398 Aqr |Blazhko effect? V0399 Aqr |Blazhko effect. V0409 Aqr |Blazhko effect? V0413 Aqr |Blazhko effect. V0425 Aqr |VB A (B sp). Blazhko effect? V0427 Aqr |Field star? Blazhko effect? Another possible period: P = 0.746053d. V0429 Aqr |Blazhko effect. V0432 Aqr |P varies. V0440 Aqr |Strong Blazhko effect [g0006]. P varies? [g0001]. V0457 Aqr |P varies, the light elements in the Table are for JD 2452433 - V0457 Aqr |2452445. V0462 Aqr |P varies, the light elements in the Table are for JD 2452433 - V0462 Aqr |2452445. V0477 Aqr |Period varies. V0485 Aqr |Porb = 1.68d. V0486 Aqr |P1 is presented in the Table. P0 = 0.582264d, P1/P0 = 0.7455. V0488 Aqr |P1 is presented in the Table. P0 = 0.564100d, P1/P0 = 0.7454. V0489 Aqr |VB A (14.2mG; B 15.5mG, 4", 36{deg}, 2000). The range in the Table V0489 Aqr |is for combined brightness. V0491 Aqr |P1 is presented in the Table. P0 = 0.600176d, P1/P0 = 0.7454. V0493 Aqr |Period varies strongly. V0494 Aqr |P1 is presented in the Table. P0 = 0.488297d, P1/P0 = 0.7444. V0497 Aqr |P1 is presented in the Table. P0 = 0.471482d, P1/P0 = 0.7438. V0499 Aqr |Period varies? V0500 Aqr |P1 is presented in the Table. P0 = 0.501303d, P1/P0 = 0.7457. V0501 Aqr |MinII - MinI = 0.53P. V0503 Aqr |P1 is presented in the Table. P0 = 0.546980d, P1/P0 = 0.7466. V0504 Aqr |P1 is presented in the Table. P0 = 0.467934d, P1/P0 = 0.7429. V0505 Aqr |Period varies strongly. V0508 Aqr |P1 is presented in the Table. P0 = 0.549393d, P1/P0 = 0.7463. V0509 Aqr |P1 is presented in the Table. P0 = 0.551978d, P1/P0 = 0.7462. V0512 Aqr |O'Connell effect. V0513 Aqr |VB B (A 16.1mG, B 17.3mG; AB 12", 116{deg}, 2000). Blazhko effect, V0513 Aqr |P = 107d. V0518 Aqr |P1 is presented in the Table. P0 = 0.570136d, P1/P0 = 0.7463. V0519 Aqr |P1 is presented in the Table. P0 = 0.506748d, P1/P0 = 0.7449. V0521 Aqr |P1 is presented in the Table. P0 = 0.482006d, P1/P0 = 0.7447. R Aql |Period decreases, current elements are given. OH, H2O, SiO maser. U Aql |SB, Porb = 1856.4d. VB A (B 11.7m, 2", 224{deg}, 2009). V Aql |Biperiodic, P0 is tabulated, P1 = 215d. W Aql |SiO maser. Y Aql |Speckle binary (0.3"). Z Aql |H2O maser. RR Aql |OH, H2O, SiO maser. RS Aql |OH, H2O, SiO maser. SV Aql |OH, H2O maser. SY Aql |OH, H2O, SiO maser. SZ Aql |P varies, current elements are tabulated. TU Aql |VB A (B 10.9m, 9", 356{deg}, 2000). TW Aql |OH maser. UU Aql |Porb = 0.163532d. UX Aql |VB A (B 4", 123{deg}). VX Aql |Double maxima. XZ Aql |P varies, current elements are tabulated. YY Aql |IR excess. YZ Aql |d = 0.03P. P varies, current elements are tabulated. AA Aql |[Fe/H] = -0.58. AK Aql |VB A (B 12.4m, 17", 86{deg}, 1999). BC Aql |[Fe/H] = 0.1. BF Aql |Multiple. CD Aql |VB, the SW component varies. Combined magnitudes are tabulated. CI Aql |The first outburst was detected in 1917. Eclipsing variations in CI Aql |quiescence: 15.3-16.2-15.7mV, Min = 2448412.167 + 0.618355d x E, D CI Aql |= 0.20:P [N0252]. CL Aql |Multiple. CR Aql |Blazhko effect? CS Aql |VB A (B p). DM Aql |VB A (B 13.2m, 14", 178{deg}; C 14.0m, 8", 12{deg}, 1996). DO Aql |Eclipses: variable amplitude of the orbital variations, up to 0.8m. DO Aql |Min = 2448832.4408 + 0.167762d x E [N0255]. EU Aql |H2O, SiO maser. EV Aql |P varies, current elements are tabulated. [A/H] = -0.3. EW Aql |VB A (A 12.2mV; B 12.4mV, 16", 188{deg}, 2000). EX Aql |Double wave, RV Tauri-like. FF Aql |VB A (B 10.1m, 7", 144{deg}, 2002; Aa, Ab 0.2", 157{deg}, 1990). FF Aql |SB1 (P = 1433d). P varies, quadratic term +84d x 10^(-10) x E^2. FG Aql |In the dark nebula B130. FH Aql |In the dark nebula B130. FK Aql |P varies, current elements are tabulated. FN Aql |P varies, current elements are tabulated. FO Aql |Porb = 0.217d. FY Aql |VB A (B 14.5:mV, 5", 219{deg}, 2000; B is a blend). FZ Aql |VB A (B 11.5m, F2V, 15", 163{deg}, 1999). The combined brightness FZ Aql |in the ASAS photometry varies between 10.02m and 10.12mV. GK Aql |VB A (A 13m:V; B 13.1mV, 24", 3{deg}, 1999). Available deep surveys GK Aql |do not show a large amplitude. GU Aql |d = 0.02P. GY Aql |OH, SiO maser. GZ Aql |VB? HI Aql |VB A (B 14.1m, 26", 332{deg}, 2000). II Aql |VB A (B 15.4m, 10", 39{deg}, 1996; C 15.5m, 13", 235{deg}, 1996). IM Aql |P varies, the tabulated elements are valid between JD 2432772 and IM Aql |2439000. IQ Aql |VB A (B 13.8m, 23", 168{deg}, 2000). KL Aql |[A/H] = 0.6. KM Aql |Blazhko effect, P = 192.20d. KO Aql |P varies, current elements are tabulated. KX Aql |Porb = 0.06035d. LS Aql |A wave with a cycle of 50-60d and an amplitude about 0.2-0.3m is LS Aql |superposed. LT Aql |Several companions at distances between 16" and 34". MQ Aql |VB A (B 8", 109{deg}, 1998). MV Aql |VB B (A 7.1mJ, B 10.0mJ; AB 6", 77{deg}, 2000). OO Aql |P varies, current elements are tabulated. OP Aql |P varies, current elements are tabulated. OS Aql |VB A (7.1mJ; B 11.3mJ, 8.5", 171{deg}, 1999). PP Aql |[A/H] = 0.0. P varies, current elements are tabulated. PQ Aql |Porb = 0.24675d. QS Aql |VB AB (6.69m, 6.75m, 0.2", 311{deg}, 2010). QY Aql |P varies, current elements are tabulated. V0337 Aql |P varies? V0341 Aql |[Fe/H] = -1.22. V0342 Aql |VB B (A 8.3mV, B 8.7mV; AB 20", 14{deg}, 1999). P varies, current V0342 Aql |elements are tabulated. V0343 Aql |P varies, current elements are tabulated. V0346 Aql |VB A (B 11.4m, 3", 244{deg}, 2012); the magnitude in the table are V0346 Aql |for combined brightness. P varies, current elements are tabulated. V0360 Aql |VB A (B 15.3mpg, 3", 215{deg}). V0368 Aql |Eclipses: Min = 2449189.5230 + 0.69050942d x E, amplitude about V0368 Aql |0.25mR [N0263]. V0379 Aql |VB A (A 9.1mJ; B 13.6mJ, 6", 1998). Combined magnitudes are V0379 Aql |tabulated. V0387 Aql |VB A (B 15.0mV, 8", 332{deg}, 1999; also other components). V0409 Aql |Spectral type A2-A3 in a different publication. V0413 Aql |A very unusual light curve, with a large (up to 0.5mV) scatter V0413 Aql |outside of minima. IR excess? V0417 Aql |P varies, current elements are tabulated. V0418 Aql |P varies? Current elements are tabulated. V0419 Aql |Superposed shorter (80d - 100d) waves with an amplitude about 0.3m. V0434 Aql |Several companions within 40". V0435 Aql |Several companions within 25". V0441 Aql |Often exhibits double maxima. V0455 Aql |OH, H2O maser. V0459 Aql |VB A (B 15m, 8", 131{deg}). V0461 Aql |VB A (B 14.2m, 8", 286{deg}, 1990). V0466 Aql |VB A (B 11.0m, 22", 19{deg}, 2000). V0470 Aql |H2O maser. V0483 Aql |In the region of the open cluster NGC 6709. A cycle about 927d is V0483 Aql |possible. V0484 Aql |VB B (A 11.0mV, B 12.2mV; AB 26", 84{deg}, 1999). V0486 Aql |VB A (B 15.0mV, 9", 276{deg}). V0497 Aql |VB A (B 15.2mV, 10", 26{deg}, 1993). V0500 Aql |Eclipses: P = 0.1452d, depth about 0.4m [N0264]. V0502 Aql |VB A (B 5", 335{deg}); combined magnitudes are tabulated. V0522 Aql |VB A (A 8.9mJ, B 12.7mJ; AB 5", 249{deg}, 1998); combined V0522 Aql |magnitudes are tabulated. V0526 Aql |P varies? Current elements are tabulated. V0528 Aql |VB A (B 16.3m, 10", 74{deg}, 1951). V0530 Aql |VB A (B 13.0mR, 24", 18{deg}, 1999; C 13.2mR, 16", 336{deg}). V0535 Aql |VB A (B 15.6m, 9", 279{deg}, 1999). V0536 Aql |Speckle-interferometric binary (0.5", 17{deg}). V0539 Aql |VB A (B 15.2mpg, 7", 235{deg}). V0556 Aql |VB A (B 7", 270{deg}). V0557 Aql |P varies, current elements are tabulated. V0561 Aql |VB A (12.5:mV; B 13.6mV, 22", 205{deg}, 1999; C 14.1mV, 20", V0561 Aql |169{deg}, 1999). V0572 Aql |P varies, current elements are tabulated. [Fe/H] = 0.0. V0602 Aql |P varies, current elements are tabulated. V0603 Aql |Porb = 0.13815d, reflected in the X-ray flux and polarization. V0603 Aql |Variations at minimum brightness: 11.62-12.15mV, Positive V0603 Aql |(0.144-0.145d) and negative (about 0.135d) superhumps, quasi-peri V0605 Aql |VB A (B 15.6m, in 8" sf). A maximum was observed in 1919, with V0605 Aql |secondary brightenings. Faint after 1923. In the center of the V0605 Aql |planetary nebula A58. Probably an event of the final helium V0609 Aql |VB A (B 5", 90{deg}, 1998). Combined magnitudes are presented. P V0609 Aql |varies? Currents elements are tabulated. V0635 Aql |VB A (B 13.8m, 13", 187{deg}, 1999). The tabulated magnitudes are V0635 Aql |influenced with the companion. OH maser. V0641 Aql |VB B (A 13.6m; AB 14", 303{deg}, 2000). V0654 Aql |VB B (A 12.8m; AB 20", 305{deg}, 2000). The tabulated magnitudes V0654 Aql |are probably influenced with the companion. V0666 Aql |VB A (B 5", 356{deg}, 1997). Combined magnitudes are tabulated. V0672 Aql |Blazhko effect? V0676 Aql |VB A (A 13.8mV; B 14.2mV, 12", 51{deg}, 2000). V0694 Aql |VB A? (B 1"). V0703 Aql |VB A (7.54mK; B 8.82mK, 23", 90{deg}). V0724 Aql |P varies? Current elements are tabulated. V0725 Aql |VB A (B 12.7m; AB 13", 10{deg}, 1991). V0734 Aql |VB A (B 16.3m, 7", 114{deg}, 1997). V0755 Aql |The light elements Min = 2429195.290 + 1.01598d x E are not V0755 Aql |excluded. V0761 Aql |P varies? Current elements are tabulated. V0762 Aql |The period 2.1d/N [00387] cannot be confirmed with more recent V0762 Aql |epochs of minima. V0766 Aql |[Fe/H] = -1.98. V0778 Aql |VB A (B 13.2m, 20", 18{deg}, 2000; C 13.4m, 13", 78{deg}, 2000). V0780 Aql |OH maser. V0782 Aql |VB A (B 15.9mV, 6", 322{deg}, 2000). V0793 Aql |[Fe/H] = -1.53. V0801 Aql |VB A (B 14.0m, 14", 240{deg}, 1999). V0803 Aql |P varies, current elements are tabulated. V0812 Aql |VB A (B 14.4mV, 11", 122{deg}, 1999; C 6", 226{deg}). V0814 Aql |VB A (13.8mR; B 15.8mR, 8", 236{deg}, 1999). V0819 Aql |VB B (A 13.3mV; B 14.1mV, 11", 235{deg}, 1999). V0822 Aql |VB A (B 9.6m, 1", 70{deg}, 1991; C 10.5m, 297{deg}, 2003). V0825 Aql |VB A (12.4mV; B 13.3mV, 26", 236{deg}, 1999; C 13.4mV, 18", V0825 Aql |213{deg}, 1999). V0829 Aql |Multiperiodic. V0845 Aql |VB A (B 13.2m, 29", 28{deg}, 2000). V0846 Aql |Modern photometric surveys do not confirm the tabulated variability V0846 Aql |data. V0866 Aql |VB A (B 5"s). V0871 Aql |MinII - MinI = 0.55P. V0877 Aql |VB A (B 16.5mpg, 6", 49{deg}, 1999; C 17.2mR, 7", 155{deg}, 1999). V0878 Aql |VB A (11.6mV; B 12.0mV, 21", 180{deg}, 1999). V0888 Aql |VB C (A 12.4mV, B 13.0mV; AC 18", 307{deg}, 1999; BC 23", 111{deg}, V0888 Aql |1999). In the region of the open cluster NGC 6738. V0889 Aql |MinII - MinI = 0.36P. P varies, current elements are tabulated. V0889 Aql |Light-time effect, apsidal motion? V0895 Aql |[Fe/H] = -0.54. V0909 Aql |VB A (14.4mR; B 15.7mR, 8", 171{deg}, 1998; C 16.0mR, 19", V0909 Aql |100{deg}, 1998). V0912 Aql |VB A (B 13.6m, 12", 309{deg}, 1999). V0913 Aql |The tabulated period corrects a misprint in [08717]. V0917 Aql |d = 0.03P. V0923 Aql |Periodic variations with P = 0.8518d were reported in [03178]. SB, V0923 Aql |P = 214.756d. V0926 Aql |P varies? Current elements are tabulated. V0927 Aql |VB B (A 14.2mV, B 14.9mV; AB 7", 328{deg}, 1999). V0936 Aql |P varies, current elements are tabulated. VB B (A 13.3mV, B 13.6mV; V0936 Aql |AB 11", 35{deg}, 2000). V0958 Aql |VB A (A 15.4mV; B 15.7mV, 8", 57{deg}, 1999; C 16.1mV, 12", V0958 Aql |313{deg}, 1999). V0962 Aql |P varies, current elements are tabulated. V0965 Aql |VB A (B 14.7mV, 11", 118{deg}, 1998). V0968 Aql |Multiple. V0971 Aql |[Fe/H] = -0.3. V0991 Aql |Multiple. V0999 Aql |Observations from [07806] contradict the tabulated elements. V1012 Aql |P2 = 83.7d, P3 = 1146d. V1019 Aql |VB A (A 12.7mV; B 16.7mV, 16", 196{deg}, 1997; also fainter V1019 Aql |companions). V1046 Aql |P varies? V1058 Aql |VB A (A 12.5mJ; B 13.9mJ, 11", 225{deg}, 1998). V1062 Aql |OH, H2O maser. V1069 Aql |VB (4"). V1070 Aql |VB B (A 14.0mV, B 14.1mV; AB 12", 160{deg}, 2000). V1076 Aql |VB B (A 14m; AB 12", 284{deg}, 1998). V1086 Aql |VB A (B 7", 291{deg}, 2000). Combined magnitudes are tabulated. V1096 Aql |P varies, current elements are tabulated. V1101 Aql |Porb = 0.1442d. V1102 Aql |P = 0.594045d is also possible. V1112 Aql |MinII - MinI = 0.30P? V1132 Aql |VB B (A 14.1V; AB 5", 228{deg}, 2000). V1140 Aql |P varies? V1147 Aql |VB B (A 12.6m; AB 24", 259{deg}, 1998). V1154 Aql |MinII - MinI = 0.70P. V1166 Aql |Type UG is also possible. V1173 Aql |VB A (B 17.6m, 13", 241{deg}, 2000). V1199 Aql |Not red. V1204 Aql |VB A (B p). V1208 Aql |Multiperiodic. V1215 Aql |The tabulated period can be a multiple of the true one. V1248 Aql |OH, H2O maser. V1251 Aql |Another solution from different data: EB:, 13.0m - 13.7mV, MinII V1251 Aql |13.5mV, Min = 2451443 + 0.49942d x E. V1269 Aql |VB A (B 7", 43{deg}, 1999). Combined magnitudes are tabulated. V1285 Aql |SB2, Porb = 10.3191d. V1286 Aql |Rapid oscillations: P = 11.6 minutes, multiperiodic, amplitude V1286 Aql |about 0.001mB [N0287]. V1293 Aql |Long-term variations: P = 270:d. V1297 Aql |d = 0.05P. V1298 Aql |A flare was detected spectroscopically [06835]. A V1298 Aql |common-proper-motion companion of BD+04 4048. V1300 Aql |OH, SiO maser. V1302 Aql |OH, SiO maser. Was gradually brightening in 1925 - 1970. Becomes V1302 Aql |gradually hotter. A protoplanetary object? V1309 Aql |P = 6.97d/N. V1319 Aql |H2O maser. V1323 Aql |Several companions. V1325 Aql |VB A (B 4" sf). V1333 Aql |Aql X-1. VB B (A 19.4m; B 0.5" p). Outbursts once in several V1333 Aql |months. V1338 Aql |VB B (A 15.8mR; B 16.0mR, 6", 84{deg}, 1999). V1339 Aql |SB?, P = 1.27219d. Speckle-interferometry binary, {rho} = 0.057". V1340 Aql |d = 0.06P:. Intrinsic brightness variations outside eclipses are V1340 Aql |possible. V1342 Aql |P varies, current elements are tabulated. V1343 Aql |SS 433. B - V = +2.0m. Associated with the SNR W 50. The light V1343 Aql |elements for eclipses are tabulated. Eclipses: the depth of MinI V1343 Aql |varies between 0.2 and 0.9m; that of MinII, between 0 and 0.4m. The V1343 Aql |mean light varies between 14.0m and 14.6m with the period 162.15d, V1343 Aql |which varies; this period is usually interpreted as precession of V1343 Aql |the accretion disk. Also noted is the period 6.2877d, interpreted V1343 Aql |as nutation. Different kinds of activity and irregularity are V1343 Aql |present in the light curves. Three systems of H, HeI, HeII emission V1343 Aql |lines are observed in the spectrum: the "stationary" one, featuring V1343 Aql |radial velocity variations between 150 and 300 km/s with the V1343 Aql |orbital period, and two "relativistic" ones, with radial velocity V1343 Aql |variations, opposite in phase, between -35000 and +50000 km/s. The V1343 Aql |"relativistic" systems correspond to two jets consisting of V1343 Aql |high-density condensations of matter emerging from the system at a V1343 Aql |relativistic velocity (0.27 c). The system is generally considered V1343 Aql |a prototype microquasar, but its properties remain extreme for the V1343 Aql |whole class of such objects. V1352 Aql |VB A (B 14.6m, Sp M3, 6", 172{deg}, 1999). A chain of Herbig - Haro V1352 Aql |objects near the variable. V1355 Aql |P varies? V1360 Aql |OH, SiO maser. V1361 Aql |OH, SiO, H2O maser. V1362 Aql |OH, SiO, H2O maser. V1363 Aql |OH maser. V1364 Aql |OH, SiO, H2O maser. V1365 Aql |OH, SiO, H2O maser. V1366 Aql |OH, SiO, H2O maser. V1367 Aql |OH, SiO maser. V1368 Aql |OH, SiO, H2O maser. V1369 Aql |OH, SiO maser. V1376 Aql |VB (9", 356{deg}, 2000). The light elements need verification. V1379 Aql |The period of RS variations is tabulated. Eclipses: Min = V1379 Aql |2449656.4804 + 20.66118d x E, D = 0.07P, d = 0.06P, depth 0.17mU. V1401 Aql |P2 = 11.8d. [Fe/H] = -1.1. V1402 Aql |Multiple. Probably multiperiodic. V1405 Aql |The tabulated light elements are for eclipse-like fadinds, there V1405 Aql |amplitude being about 0.4m - 0.5m. V1406 Aql |VB B (A 7.03mV, B 11.3mV; AB 10", 180{deg}, 2012). V1408 Aql |The tabulated elements are for the maximum of small-scale periodic V1408 Aql |variations. V1413 Aql |d = 0.05P. The depth of eclipses outside outburst peaks is about V1413 Aql |2m. V1415 Aql |OH, SiO, H2O maser. V1416 Aql |OH, SiO, H2O maser. V1427 Aql |Possibly a protoplanetary object. V1433 Aql |OH, H2O maser. V1436 Aql |VB A (9.4mV; B 12.3mV, 4", 33{deg}, 2001). Possibly spurious V1436 Aql |variability. V1440 Aql |VB A (8.6mV; B 9.9mV, 22", 198{deg}, 2013). V1452 Aql |P = 2.5930d is also possible. V1461 Aql |VB AB (9.3m, 10.5m, 2.5", 306{deg}, 2002). V1462 Aql |VB A (8.3mV; B 11.5mV, 13", 88{deg}, 2000). V1466 Aql |VB A (6.5mV; B 10.3mV, 14", 310{deg}, 2012). V1470 Aql |VB AB (8.2m, 9.2m, 2", 286{deg}, 2011). Probably the fainter V1470 Aql |component varies. V1472 Aql |VB AB (6.6mV, 11.0mV; 3", 120{deg}, 2008). SB, Porb = 198.716d. V1473 Aql |Multiperiodic, P2 = 2.04036d, P3 = 3.41274d. V1477 Aql |VB AB (9.73mV, 12.56mV, 1", 2{deg}, 1991). Another companion: V1477 Aql |9.2mR, 20", 112{deg}, 1998. Possibly spurious variability. V1479 Aql |The spectral type presented in the Hipparcos catalog (K7) V1479 Aql |contradicts the star's color indices. Possibly spurious V1479 Aql |variability. V1488 Aql |Erroneously called GM Aql in several publications by V.P. V1488 Aql |Tsesevich. V1494 Aql |VB A (B 18.1m, 1"). Eclipses: Min = 2452462.4966 + 0.1346141d x E, V1494 Aql |depth 0.25m, D = 0.20P [N0308]. V1532 Aql |Several companions. V1538 Aql |Possible RRC periods: 0.3661945d, 0.2678428d. V1546 Aql |VB B (A 10.3mV; B 11.52mJ, 11.22mK, 16", 299{deg}, 2000). V1575 Aql |In the region of the globular cluster NGC 6749. V1576 Aql |In the region of the globular cluster NGC 6749. V1648 Aql |Brightening over 10 years, probably due to dissipating dust V1648 Aql |envelope, plus quasi-periodic variations. [Fe/H] = -1.1. V1656 Aql |The tabulated ephemeris is for eclipses. P varies, quadratic term V1656 Aql |+1.14 x 10^(-6)d x E^2. Instead, period jumps are not excluded. V1656 Aql |Occasional brightness humps: P = 8.628d. V1665 Aql |MinII - MinI = 0.40P. Slight apsidal motion. V1706 Aql |Epoch of minimum brightness is tabulated. V1707 Aql |VB A (B 13.9m, 18", 166{deg}, 1999). V1710 Aql |Epoch of maximum is tabulated. Continuous periodic brightness V1710 Aql |variations. V1719 Aql |A twice longer period is not excluded. V1737 Aql |VB A (B 12.2mV, 7", 130{deg}, 2000). V1742 Aql |VB A (B 16.5m, 2" sp). V1743 Aql |The elements tabulated are for EB variations. EA: amplitude 0.14m, V1743 Aql |Min = 2450646.6692 + 1.1920d x E, D = 0.14P. V1752 Aql |P2 = 0.3586d. V1760 Aql |P2 = 0.8381d. V1801 Aql |An asymptotic-giant-branch star. SB, Porb = 119.5d, e = 0.37. Porb V1801 Aql |is not detected in photometry. V1811 Aql |A twice shorter period is not excluded. V1815 Aql |A magnetic white dwarf, varies presumably due to starspots and V1815 Aql |axial rotation. V1820 Aql |O'Connell effect. V1834 Aql |A period about 230d is superposed. V1837 Aql |The period for the first overtone is given in the Table. Second V1837 Aql |overtone: Max = 2453729.40+ 1.01121d x E. P1 given in the Table. V1837 Aql |P2/P1 = 0.8040. V1844 Aql |Multiperiodic. V1853 Aql |VB (2"). Other possible periods: 0.66579d or 0.49934d. RRC type V1853 Aql |with P = 0.24967d is also possible. V1861 Aql |VB (3"). V1876 Aql |The one-day alias, P = 0.058916d, is also possible. V1877 Aql |P = 0.30306d is also possible. V1878 Aql |VB A (B 4", 24{deg}, 1999). V1880 Aql |P = 0.42243d is also possible. V1881 Aql |Blazhko effect. V1883 Aql |The one-day alias, P = 0.109205d, is also possible. V1886 Aql |Period varies. V1889 Aql |Multiperiodic. P2 = 0.1004498d. V1898 Aql |P = 0.4102d is also possible. V1922 Aql |The light elements in the Table are for minina of the orbital V1922 Aql |variations. Also present are pulsations with P = 198d and an V1922 Aql |amplitude of 0.6mV. V1927 Aql |Period varies. Multiperiodic. V1928 Aql |VB A (9.8mV; B 10.2mV, 7", 104{deg}, 2013). The range in the Table V1928 Aql |is for combined brightness. V1936 Aql |A red star, despite the spectral type O4I in the literature. V1946 Aql |VB A (11.4mG; B 14.3mV, 6", 200{deg}, 2000). V1968 Aql |VB A (13.5mG; B 14.7mG, 3", 165{deg}, 2000); the range in the Table V1968 Aql |is influenced by the companion. V1971 Aql |MinII - MinI = 0.61P. V1977 Aql |P = 31.5d is superposed. V1992 Aql |VB A (8.3mG; B 11.4mG, 9", 72{deg}, 2000). The range in the Table V1992 Aql |is for combined brightness. V2001 Aql |P = 34.7:d is superposed. V2005 Aql |VB A (B 12.26mV, 18", 346{deg}, 2015). V2006 Aql |P = 39.9d is superposed. alf Aql |Multiperiodic. eta Aql |The presence of an unresolved A0V companion is suspected. P varies, eta Aql |current elements are tabulated. R Ara |VB A (B 8.2m, 4", 123{deg}, 1933). S Ara |[Fe/H] = -0.71. P var. Max = 2420047.2382 + 0.451888176d*E - S Ara |1.36d*10**(-10)*E**2 (2414000 - 2441200) [03126]. For current S Ara |elements after 2441000, see Table. T Ara |VB A (B 11.0m, 34", 60{deg}). RW Ara |d = 0.02P. Changes of the shape of the light curve due to gaseous RW Ara |streams or to a hot spot are possible. SZ Ara |P var [N0005]. TV Ara |In the region of the open cluster NGC 6208. TX Ara |VB A (B 16.5m 5" sf). A twice shorter period is possible. AD Ara |[A/H] = -0.4. AW Ara |Before JD 2417300, Max = 2412600 + 186d*E. BF Ara |The superoutburst cycle is given. CC Ara |VB A (B 14.9m 7" sp). CT Ara |Between JD 2420400 and 2425000, Max = 2413080 + 215d:*E. DU Ara |P var. DZ Ara |VB A (B 12.9m 12" np). EH Ara |VB A (B 14.7m 12" nf). EK Ara |VB A (B 15m pg 5" s). FS Ara |VB A (B 15.1m V 7" nf). FT Ara |VB A (B 15.4m 7" nf). GI Ara |VB A (B 10" sp). It is not quite clear which star varies. GK Ara |The coordinates in [00251] and the chart in [06286] are believed to GK Ara |be wrong. IN Ara |[Fe/H] = -1.75. IW Ara |VB A (B 15.9m 9" sp). KP Ara |VB A (B 14.8m 7" p). KY Ara |Only one sharp Max (JD2428715 - 721) was observed [00629]. Possibly KY Ara |a Nova. KZ Ara |VB A (B 13.5m 13" p). LW Ara |As of May 2006, erroneously called LX Ara in [N0002]. MQ Ara |VB A (B = NSV 9784 25" sp). MR Ara |[Fe/H] = -1.0. MS Ara |[Fe/H] = -1.48. MT Ara |VB A (B 13.5m 26" sf). MV Ara |VB A (B 17.6m 7" nf), a star 13.5m 18" n. MX Ara |VB A (B 15.5m 14" sf). NU Ara |VB B (A 16.4m 8" sp). OY Ara |Eclipsing variations [N0010]: amplitude 1.9m (wide B+V filter), Min OY Ara |= 2449862.8220 + 0.155466d*E. QR Ara |Marked in the chart for BV 1443. ASAS-3 data do not show noticeable QR Ara |variations. QX Ara |Erroneously called V675 Ara in [N0002]. V0340 Ara |[A/H] = 0.6. V0341 Ara |X-ray source 1RXS J165743.7-631237. V-Ic between 0.08m and 0.20m V0341 Ara |[N0012]. The periods 11.95d [00080], 10.919d [HIP], 14.11045d V0341 Ara |[N0012] satisfy observations only during some intervals of time. V0342 Ara |P >= 140d. V0345 Ara |P >= 180d. V0355 Ara |P > 220d. V0356 Ara |P > 170d. VB B (A 12.65m B, 22" nf). V0360 Ara |Min II - Min I = 0.35P. V0383 Ara |VB A (B 16.5m 8" nf). V0419 Ara |Not red [00001]. V0422 Ara |According to [04001] and [01385], UG. The spectral type suggests V0422 Ara |another type [N0013]. V0433 Ara |Eclipses: Min = 2453065.5502 + 0.19573d*E [N0014]. According to V0433 Ara |[N0014], the outside-eclipse brightness varies between 16.8m and V0433 Ara |18.4m V, suggesting a type like NL+EA or UGZ+EA. The faintest V0433 Ara |magnitude observed in an eclipse was about 19.6m V. V0447 Ara |Another possible solution of the data from [N0002]: Min = V0447 Ara |2451936.878 + 18.146d*E [N0015]. V0461 Ara |Identified with a bright IR object in the 2MASS catalogue. V0520 Ara |No objects with Mira-like colors in the field [00001]. V0528 Ara |Not an RR Lyrae star according to [N0006], where no period could be V0528 Ara |found between 0.25d and 2.0d. V0539 Ara |VB A (B 9.22m, 12", 269{deg}). DII = 0.13P. Apsidal motion. V0539 Ara |Tabulated are: the epoch of MinI based on observations in [HIP] and V0539 Ara |the siderial period from [N0017]. In 1982 - 1994, MinI = V0539 Ara |2445056.777 + 3.169112d*E, MinII = 2445067.825 + 3.169076d*E, U = V0539 Ara |150 years. The fainter component of the eclipsing pair pulsates, V0539 Ara |the detected periods are 1.36d, 1.78d, 1.08d [N0017]. V0544 Ara |VB A (B 14.5m pg, 17" sp). V0577 Ara |The chart in [03776] leads to a much brighter star than the V0577 Ara |magnitudes in [03776]; for this brighter star, the data in [N0002] V0577 Ara |permit to suspect type EA, Max 13.1m V, MinI 13.6m V, MinII 13.3:m V0577 Ara |V, MinI = 2453090.826 + 0.6880d*E, with a large light-curve scatter V0577 Ara |[00001]. V0583 Ara |The chart in [03776] leads to a much brighter star than the V0583 Ara |magnitudes in [03776]. V0613 Ara |VB B (A 12" np). V0617 Ara |VB B (A 13.1m Bj, 12" nf). Combined magnitudes of the pair are V0617 Ara |given. V0624 Ara |MaxII 11.9 at the phase 0.4. V0639 Ara |V1 (NGC 6397). Cluster non-member. V0650 Ara |Individual cycles have amplitudes about 0.7m, the mean brightness V0650 Ara |level varies. V0656 Ara |EW type is not excluded. V0658 Ara |The suggested type is in contradiction with the star's red color V0658 Ara |[00001]. V0687 Ara |Type RRC is possible. V0710 Ara |Individual cycles have amplitudes from 0.5m to 1m, secondary cycle V0710 Ara |about 750d. V0729 Ara |Type RV with a twice longer period is possible. V0744 Ara |Not red. V0755 Ara |The chart in [07772] (BV 1310) shows a different variable star. V0793 Ara |Not red. V0801 Ara |MXB 1636-53. Description of the spectrum [01356]. Modulation with V0801 Ara |Porb = 0.15804738d [N0020], amplitudes up to 0.6m V. V0808 Ara |Type EW is possible. V0816 Ara |Type RR: was suggested in [01385], but the star is red. V0820 Ara |Epoch of Min is given. Strong magnetic field. Either an eclipsing V0820 Ara |binary or a white-dwarf oblique rotator. V0821 Ara |4U 1658-48. Complex behavior. Three X-ray states: off, hard-low, V0821 Ara |high-soft, poorly correlated with optical variations. The latter V0821 Ara |consist of flickering, possible low-amplitude quasi-periodic V0821 Ara |variations, and large-amplitude changes. Porb near 0.7d is V0821 Ara |suspected. V0825 Ara |V2 (NGC 6397), cluster non-member. V0826 Ara |V3 (NGC 6397), cluster non-member. V0827 Ara |V4 (NGC 6397) according to the numbering system from [67025] V0827 Ara |(differs from the numbering system in [N0025]). Probably cluster V0827 Ara |non-member. V0829 Ara |Type SRB is possible [71065]. According to [HIP], ELL, 6.06m - V0829 Ara |6.14m Hp, Min = 2448504.951 + 7.5010d*E; these type and period seem V0829 Ara |improbable for the spectral type. V0832 Ara |Porb = 5200d. V0834 Ara |Oscillations: P = 12 minutes. V0835 Ara |Oscillations: P = 10.75 minutes. V0837 Ara |Associated with a nebula. V0839 Ara |Associated with a nebula. V0883 Ara |MinII - MinI = 0.44P. V0898 Ara |Multiperiodic. V0909 Ara |Called "BH Ara?" in [80474]; the suggested identification is wrong. V0919 Ara |SB2. V0927 Ara |VB A (B 13.3m, 14", 121{deg}, 1999). The magnitude in minimum is V0927 Ara |influenced with the companion. V0943 Ara |Similarity to FG Sge is not excluded. V0952 Ara |Multiperiodic, 5 frequencies detected. V0969 Ara |VB A (B 13.8m, 16", 148{deg}, 1999). V0978 Ara |P=46.5d is superposed. V0981 Ara |Blazhko effect, P = 58.66d. V0982 Ara |VB B (A 13.9mpg, B 14.3mpg; AB 13", 351{deg}, 2000). The magnitudes V0982 Ara |in the Table are influenced by the companion. V1000 Ara |VB A (B 9" p). V1011 Ara |Period varies. V1027 Ara |VB A (B 14.0m, 12", 51{deg}, 2000). The magnitudes in the Table V1027 Ara |were influenced by the companion. V1042 Ara |VB A (B 12.5m, 8.5", 329{deg}, 2000). V1054 Ara |Cluster non-member. V1055 Ara |Cluster non-member. V1058 Ara |Cluster non-member. V1059 Ara |Additional mode, P = 0.6285d [g0025]. V1060 Ara |Blazhko effect, P(Blazhko) = 57.710d [g0025]. Blazhko effect, V1060 Ara |P(Blazhko) = 35.2368d [g0025]. V1061 Ara |Cluster non-member. MinII - MinI = 0.26P. V1063 Ara |Cluster non-member. V1064 Ara |Cluster non-member. V1065 Ara |Additional mode, P = 0.1707740d [g0025]. V1067 Ara |A second high-amplitude mode: P = 0.2509836d. V1071 Ara |Blazhko effect, P(Blazhko) = 34.809d; additional period 216.34d V1071 Ara |[g0025]. V1072 Ara |A0 = 0.3771mV. P1 = 0.3266817d, A1 = 0.0275mV, P1/P0 = 0.7304 V1072 Ara |(abnormal ratio). V1073 Ara |Blazhko effect, P(Blazhko) = 13.764d. Additional mode, P = V1073 Ara |0.1897573d. V1075 Ara |Cluster non-member. V1077 Ara |Cluster non-member. V1078 Ara |MinII - MinI = 0.75P. V1080 Ara |Blazhko effect, P(Blazhko) = 82.267d [g0025]. V1083 Ara |Blazhko effect, P(Blazhko) = 66.917d [g0025]. V1084 Ara |A0 = 0.3089mV. P1 = 0.3596333d, A1 = 0.0177mV, P1/P0 = 0.7275 V1084 Ara |(abnormal ratio). V1085 Ara |Blazhko effect, P(Blazhko) = 17.4043d [g0025]. V1088 Ara |Blazhko effect, P(Blazhko) = 41.191d [g0025]. V1090 Ara |Period varies. V1092 Ara |Additional mode, P = 0.1688913d [g0025]. V1093 Ara |Blazhko effect, P(Blazhko) = 17.3010d [g0025]. V1094 Ara |Blazhko effect, P(Blazhko) = 73.332d [g0025]. V1095 Ara |Additional mode, P = 0.1715296d [g0025]. V1096 Ara |Cluster non-member. V1097 Ara |Double-periodic Blazhko effect, P1(Blazhko) = 15.4504d, P2(Blazhko) V1097 Ara |= 13.771d. V1100 Ara |Additional mode, P = 0.2002600d [g0025]. V1101 Ara |Additional mode, P = 0.1783040d [g0025]. V1103 Ara |Blazhko effect, P(Blazhko) = 56.190d [g0025]. V1105 Ara |Blazhko effect, P(Blazhko) = 78.036d [g0025]. V1108 Ara |Additional mode, P = 0.1730099d [g0025]. V1109 Ara |Cluster non-member. V1113 Ara |Blazhko effect, P(Blazhko) = 8.52242d. V1116 Ara |Additional modes, P = 0.1924287d, P = 0.1955796d, P = 0.1984818d V1116 Ara |[g0025]. V1117 Ara |Cluster non-member. V1118 Ara |Additional modes, P = 0.187836d and 0.19332d. V1119 Ara |According to [g0026], cluster non-member, in contradiction to Gaia V1119 Ara |DR2 proper motion. V1121 Ara |Cluster non-member. V1124 Ara |Cluster non-member. V1126 Ara |Cluster non-member. V1133 Ara |The Table presents the probable first-overtone period. P0 = 0.52d. V1133 Ara |Probable cluster non-member [g0023]. The suggested P0 gives P1/P0 = V1133 Ara |0.66, not typical of first-overtone and fundamental-mode pulsators V1133 Ara |[g0001]. V1143 Ara |Chandra X-ray source. V1144 Ara |Chandra X-ray source. V1146 Ara |Optical counterepart of the millisecond pulsar PSR J1740-5340. R Ari |H2O, OH maser. T Ari |H2O, SiO maser. P varies strongly, current elements are given. U Ari |SiO maser. W Ari |A "missing BD star", no certain identification. X Ari |P varies, current elements are given. [Fe/H] = -2.50. RU Ari |OH, H2O maser. RV Ari |Double-mode. P0 is given in the Table, P1 = 0.0719469d. Both RV Ari |periods vary. RW Ari |[Fe/H] = -1.16. RX Ari |d = 0.02P. P varies, current elements are given. RY Ari |H2O maser. SS Ari |P varies, current elements are given. SU Ari |A "missing BD star", identification uncertain. SZ Ari |P varies, current elements are given. TT Ari |Porb = 0.13755d. Usually near maximum brightness, occasional deep TT Ari |fadings. Numerous photometric periods were reported. According to TT Ari |[N0138], the star experiences alternating "negative superhump" (P = TT Ari |0.13270 - 0.1398d) and "positive superhump" (P = 0.14840 - TT Ari |0.14926d) intervals, with amplitudes of several tenths of a TT Ari |magnitude. Quasiperiodic oscilations, flickering. TU Ari |P varies, current elements are given. TX Ari |P varies, current elements are given. UU Ari |Multiperiodic. UV Ari |Probably multiperiodic. UX Ari |VB (0.4", 61{deg}, 1990.8). SB2, Porb = 6.43791d. Photometric UX Ari |variations with a period close to Porb. Mean brightness varies. VW Ari |Multiperiodic. VY Ari |SB1, Porb = 13.20d. WW Ari |VB (3"). Probably both components vary. WX Ari |The elements are for eclipses. Flickering. YY Ari |H2O, OH maser. YZ Ari |OH maser. AD Ari |According to [N0146], DSCTC pulsations with a period about 0.06d AD Ari |can be also present. BF Ari |Periodically variable brown dwarf. BG Ari |Superhumps detected: P1 = 0.084897, P2 = 0.084683. BI Ari |Multiperiodic. BL Ari |Blazhko effect? BQ Ari |VB A (A 10.9m; B 11.5m, 14", 19{deg}, 2000). The tabulated BQ Ari |magnitudes are possibly affected by the companion. BS Ari |VB (0.5", 104{deg}, 2001). BU Ari |VB (0.4", 52{deg}, 2001); VB A (B 4", 61{deg}, 2001; C = BV Ari, BU Ari |15", 23{deg}, 2001). BV Ari |VB (0.4", 234{deg}, 2001); VB C (A = BU Ari; AC 15", 23{deg}, BV Ari |2001). BX Ari |VB AB (1", 165{deg}, 2001). CP Ari |VB A (B 7", 149{deg}, 1997). CR Ari |Type ELL with the light elements Min = 2455181.6141 + 0.361849d x E CR Ari |is also possible. DN Ari |P1 is presented in the Table. P0 = 0.547871d; P1/P0 = 0.7466. DO Ari |P1 is presented in the Table. P0 = 0.564048d; P1/P0 = 0.7455. DP Ari |P1 is presented in the Table. P0 = 0.492409d; P1/P0 = 0.7449. DQ Ari |P1 is presented in the Table. P0 = 0.480781; P1/P0 = 0.7441. DS Ari |VB B (A 15.3mV, const, at the coordinates of 1SWASP DS Ari |J022727.03+115641.7; B varies, AB 12", 309{deg}, 2000; C 17.3mV, AC DS Ari |14", 348{deg}, 2000). The data in in [82030] are for combined DS Ari |brightness. The magnitudes in the Table also seem to be somewhat DS Ari |influenced with the companions. DT Ari |P1 is presented in the Table. P0 = 0.561570d; P1/P0 = 0.7455. DV Ari |P1 is presented in the Table. P0 = 0.481500d; P1/P0 = 0.7448. gam Ari |VB A (B 4.65m, B9V, 8", 0{deg}). tau 1 Ari |VB AB (B 8.4m V, 0.7", 246{deg}, 1968). R Aur |H2O, SiO maser. P varies, current elements are given. T Aur |Eclipses: Min = 2452283.261 + 0.20437826d * E. The minima from T Aur |0.10m to 0.28m deep in integrated light [03195]. U Aur |OH, H2O, SiO maser. Z Aur |P varies, current elements are given. RS Aur |Biperiodic, the second period is 168d [N0039]. RT Aur |P varies, current elements are given. RU Aur |OH, SiO maser. RV Aur |Mean magnitude probably varies with Pi = 10400d [01059]. RW Aur |VB ABC (1.4", 255{deg}, 1994; B 13.6m, K5, suspected in flare RW Aur |activity; BC 0.12"). RX Aur |P varies [N0147]. Elements for 1990s are given in the Table. [Fe/H] RX Aur |= -0.13. RY Aur |P varies, current elements are given. RZ Aur |P varies, current elements are given. SS Aur |Porb = 0.1828d. Intervals of abnormal photometric behavior SS Aur |(frequent low-amplitude outburts) occur sometimes. ST Aur |VB A (B 14m, 7" sp). SU Aur |OH maser. SX Aur |P varies, current elements are given. SY Aur |P varies, current elements are given. SZ Aur |SiO maser. TW Aur |The mean brightness varies with P = 1380d. TZ Aur |[Fe/H] = -0.79. UU Aur |Double-mode, also P = 235d. UV Aur |A symbiotic Mira. Very variable heights of maxima. [NeIII] and UV Aur |[OIII] emissions in the spectrum. VB A (B 10.96m, B9V, 3.4", UV Aur |4{deg}). The B9V companion is apparently not hot enough to excite UV Aur |the nebula. UW Aur |Epoch of Min is given. UY Aur |OH maser. VB AB (B 12m?, M2, 0.9", 228{deg}, 1999). VW Aur |VB AB (9.0m, 11.8m V, 1.4", 332{deg}, 1976). XX Aur |P varies? Current elements are given. YZ Aur |SB. AB Aur |Rare deep fadings. AE Aur |The well-known "runaway star" from Ori OB1. AH Aur |The depth of MinII is 0.50m. AM Aur |P varies, current elements are given. AO Aur |P varies? Current elements are given. AP Aur |P varies, quadratic term 6.3398d*10^(-10)E^2. The depth of MinII is AP Aur |0.51m. AQ Aur |SiO maser. AR Aur |P varies, current elements are given. Period variations are AR Aur |possibly periodic, with a period of 25-27 years [N0158]. AW Aur |SiO maser. AZ Aur |VB A (B 16.3m B, 4", 165{deg}, 1953). BF Aur |P varies, current elements are given. CG Aur |Apsidal motion? P(MinII)=1.8048647d. CI Aur |P varies, current elements are given. CL Aur |The depth of MinII is 0.32m Rc. P var. Quadratic term CL Aur |+2.52d*10^(-10)E^2. Third body, P = 21.7 years. CO Aur |The tabulated period is that of the first overtone; the second CO Aur |overtone period is 1.427781d. DN Aur |[Fe/H] = -0.46. VB A (B 7", 46{deg}, 2000). EM Aur |P varies? EP Aur |P varies, current elements are given. The depth of MinII is 0.22m. EQ Aur |P varies, current elements are given. ER Aur |P varies, current elements are given. EW Aur |[Fe/H] = -0.6. FF Aur |[Fe/H] = -0.3. FP Aur |d = 0.08 P. FS Aur |Porb = 0.059479d. FZ Aur |A two times shorter period is also possible. GX Aur |P varies, current elements are given. HN Aur |The secondary period is about 1400d. II Aur |MinII 15.0:. IS Aur |VB A (B 15.4m, 18", 47{deg}, 1999). The tabulated range is for the IS Aur |combined magnitude of the pair. IU Aur |A well-documented light-time effect (P = 294.3d, the semi-amplitude IU Aur |of the O-C residuals is 0.0059d) because of a third body on an IU Aur |eccentric orbit. Precession causes changes of the brightness IU Aur |amplitude: the amplitude of the MinI was observed to vary between IU Aur |0.46m and 0.70m and that of MinII, between 0.37m and 0.55m. The IU Aur |depths of minima reached their maximum values about JD 2445800 and IU Aur |began to decrease [N0176]. KR Aur |Porb = 0.1628d. KU Aur |P varies? KW Aur |VB A (B 9.0m, 10", 9{deg}, 2004; C 7.3m, F4V+DA1, Porb = 2.99d, KW Aur |14", 225{deg}, 1991). SB, Porb = 3.7886d. The pulsation period is KW Aur |tabulated. Other pulsation harmonics: 0.096533d, 0.088243d. The KW Aur |brightness varies with the orbital period. KX Aur |In the nebula IC 405. KY Aur |In the nebula IC 405. LW Aur |VB A (B 17.5m, 9", 46{deg}, 1999). LY Aur |d = 0.017P. VB A (B 9.154m Hp, 0.6", 253{deg}, 1991). MN Aur |P varies, current elements are given. MT Aur |d = 0.02 P. NQ Aur |VB A (B 12.8m, 17", 143{deg}, 1999). NU Aur |Blazhko effect. NV Aur |OH, SiO, H2O maser. NW Aur |In the open cluster NGC 1893. NX Aur |In the open cluster NGC 1893. OP Aur |In the region of the open cluster Stock 8. OX Aur |VB A (B 10.2m, G5V(n), 22", 224{deg}, 1998). Multiperiodic. P0 is OX Aur |tabulated. P1 = 0.115442d. QT Aur |VB A (B 15.8mV, 10", 266{deg}, 2000). QU Aur |VB A (B 6", 199{deg}, 1999). QY Aur |SB2, Porb = 10.4265d. QZ Aur |Eclipses outside the outburst: 16.98m - 18.95mV, Min = 2448555.1595 QZ Aur |+ 0.3574961d x E [N0193]. V0348 Aur |VB A (B 12.8m V, 25", 222{deg}, 2007). V0353 Aur |The protoplanetary nebula "Red Rectangle". The star was brightening V0353 Aur |for several decades, between 1940s and 1970s. V0356 Aur |Multiperiodic, P2 = 0.15642d. V0358 Aur |In the region of the open cluster NGC 2099. V0361 Aur |Multiperiodic, P = 273s is dominating. V0373 Aur |SiO maser. V0382 Aur |[Fe/H] = -1.6. V0386 Aur |[Fe/H] = -1.75. V0387 Aur |[Fe/H] = -1.40. V0390 Aur |VB (A 7.25m Hp; B 9.10m Hp, 0.4", 80{deg}, 1991). Accoring to V0390 Aur |[N0197], also exhibits flares with amplitudes up to 0.29m U. V0394 Aur |VB A (B F7V, 10.72m, 9", 209{deg}, 2007). V0397 Aur |SB1, Porb > 1000d. V0398 Aur |VB A (B 12.2m, 5", 82{deg}, 1958). Multiperiodic, P2 = 2.89404d. V0403 Aur |Porb = 83.1d. V0404 Aur |Porb = 0.1726d. Amplituda (Min II) = 0.28:. V0410 Aur |P varies, current elements are given. V0411 Aur |The HD catalogue identifies HD 32447 (K) with BD+30 775, which is V0411 Aur |V0411 Aur. In the HDE Atlas, V0411 Aur = HD 282867 (M0), and HD V0411 Aur |32447 (F2) is a different star. V0424 Aur |VB (0.25", 229{deg}, 1998). V0431 Aur |In the region of the open cluster NGC 1960. V0432 Aur |d = 0.03 P. One of the components probably pulsates. V0433 Aur |SB? V0437 Aur |The HIPPARCOS observations can be represented with several V0437 Aur |different periods, the tabulated one contradicts later V0437 Aur |observations. V0440 Aur |ADS 4443A (B 12.0mV, 14", 15{deg}, 2000). V0462 Aur |ADS 5582A (B 9.76m, 8", 210{deg}, 1991). V0469 Aur |VB B (A = V499 Aur; AB 25", 87{deg}, 1999). V0490 Aur |VB. V0499 Aur |VB A (B = V469 Aur, 25", 87{deg}, 1999). V0501 Aur |SB. V0528 Aur |SiO maser. V0530 Aur |SiO maser. V0539 Aur |In the open cluster M37 (NGC 2099). Probably non-member. V0540 Aur |In the open cluster M37 (NGC 2099). V0541 Aur |In the open cluster M37 (NGC 2099). V0542 Aur |In the open cluster M37 (NGC 2099). The depth of MinII is 0.3m. V0543 Aur |In the open cluster M37 (NGC 2099). The depth of MinII is 0.66m. V0544 Aur |In the open cluster M37 (NGC 2099). The depth of MinII is 0.31m. V0545 Aur |In the open cluster M37 (NGC 2099). Non-member? V0546 Aur |In the open cluster NGC 2166. Type RS with P = 1.64470d is V0546 Aur |possible. V0547 Aur |In the open cluster NGC 2166. Probably non-member. V0548 Aur |In the open cluster NGC 2166. Probably non-member. V0549 Aur |In the open cluster NGC 2166. V0550 Aur |In the open cluster NGC 2166. V0551 Aur |In the open cluster NGC 2166. {Delta} Scuti variations: amplitude V0551 Aur |0.05m, P = 0.12936d. V0552 Aur |The period is for small-amplitude variations, flickering is also V0552 Aur |observed; the combined amplitude of these variations is 0.03m. V0560 Aur |VB (A 9.2m; B 9.6m, 0.9", 37{deg}, 1991). V0574 Aur |VB A (B 15.0mV, 11", 72{deg}, 2000). V0579 Aur |VB A (B 15.4mV, 8", 133{deg}, 1999). V0581 Aur |Originally erroneously named FS Boo, at a wrong position. V0584 Aur |VB AB (10.1m, 11.4m, 0.5", 272{deg}, 2002). V0603 Aur |VB AB (5", 59{deg}, 1999). V0608 Aur |VB A (B 15.8m, 9", 118{deg}, 2000). V0617 Aur |VB AB (8.27mHp, 11.42mHp, 1.2", 184{deg}, 1991). V0624 Aur |A twice longer period is not excluded. V0637 Aur |VB A (B 11.6mV, 14", 286{deg}, 2007). V0645 Aur |MinII - MinI = 0.789: x P. V0647 Aur |Porb = 201min, Pspin = 1008.3408s or 930.5829s. V0674 Aur |P = 0.29779d is not excluded. Type EW, with periods 0.59563d or V0674 Aur |0.63533d, is also possible. V0681 Aur |Blazhko effect. V0695 Aur |Running numbers and USNO-B1.0 numbers in [81080] are mixed up; V0695 Aur |corrected by GCVS compilers. V0696 Aur |Running numbers and USNO-B1.0 numbers in [81080] are mixed up; V0696 Aur |corrected by GCVS compilers. V0697 Aur |VB A (B 6", 70{deg}, 1997). V0698 Aur |Eccentric binary. Running numbers and USNO-B1.0 numbers in [81080] V0698 Aur |are mixed up; corrected by GCVS compilers. V0707 Aur |O'Connell effect. V0708 Aur |O'Connell effect. V0716 Aur |MinII - MinI = 0.47P. V0742 Aur |DSCTC type with P=0.132695d is also possible. V0744 Aur |VB A (B 5", 9{deg}, 2000). P = 0.362922d is also possible. V0746 Aur |P = 0.086921d is also possible. V0750 Aur |Multiperiodic, P2 = 0.069397. V0754 Aur |P = 0.33285d is also possible. V0765 Aur |VB A (B 4", 91{deg}, 1997). V0786 Aur |VB A (B 3", 183{deg}, 1989). V0790 Aur |Type EW with a twice longer period is not excluded. V0798 Aur |VB A (12.4mV; B 14.7:mV, 7", 286{deg}, 1998). V0803 Aur |Multiperiodic. P2 = 0.05503008d, P3 = 0.04250400d. V0808 Aur |Eclipses: Min = 2455126.8960 + 0.081376d x E, range 17.8 - 21.4 V, V0808 Aur |D = 0.06P. V0815 Aur |VB A (B 16.5mpg, 5", 75{deg}, 2000). V0817 Aur |MinII - MinI = 0.32P. V0823 Aur |Secondary period P2 = 0.2980d. V0829 Aur |Possible BY variations outside flares: P = 1.04098d, 16.4m - 16.6m. V0830 Aur |VB A (B 6", 176{deg}, 2000). The range in the Table is for combined V0830 Aur |brightness. V0837 Aur |VB A (B 13.4m, 19", 94{deg}, 2000; C 5", 281{deg}, 2000). V0838 Aur |MinII - MinI = 0.330P. V0839 Aur |MinII - MinI = 0.438P. V0841 Aur |VB B (A 10.8mV; AB 16", 351{deg}, 2007). V0849 Aur |Two systems of eclipses. The Table presents the light elements for V0849 Aur |system A. MinII - MinI = 0.52P. System B: MinI = 2455968.3398 + V0849 Aur |0.806931 x E; D = 0.14P. V0856 Aur |VB A (B 13.3m, 17", 345{deg}, 1998). V0860 Aur |The data for 1SWASP J070953.45+364417.3 in [82030] are combined V0860 Aur |measurementss for a non-variable star (V = 12.8) near the SuperWASP V0860 Aur |position and the real variable. V0861 Aur |P1 is presented in the Table. P0 = 0.555912d; P1/P0 = 0.7464. bet Aur |VB A (C 14.1m, 13", 174{deg}, 1934). eps Aur |d = 0.04 P. VB A (B 14.0m, 30", 225{deg}, 2008; C 11.3m, 43", eps Aur |276{deg}, 2008; D 12.0m, 45", 316{deg}, 2008). Probably eclipses eps Aur |are caused by a gas and dust disk. Besides eclipses, quasi-periodic eps Aur |brightness variations with an amplitude of several tenths of a eps Aur |magnitude and a cycle of 105 - 120 days (e.g., [N0204]). More rapid eps Aur |variations were also reported. zet Aur |D = 0.041P, d = 0.038P (varies?). tet Aur |VB A (B 7.2m, 4", 306 {deg}, 2008). psi 1 Aur |P1 = 150 - 200d, P2 = 2000d. R Boo |H2O maser. V Boo |Biperiodic, P1 = 137d. A long-term amplitude decrease. SiO maser. Z Boo |H2O, SiO, OH maser. RS Boo |P varies, current elements are given. Possible Blazhko effect RS Boo |periods: 533d, 58d, 62d [04832]. [Fe/H] = -0.36. RU Boo |[Fe/H] = -1.50. RX Boo |P2 = 304.7d, possibly P3 = 2692d. H2O, SiO, OH maser. SS Boo |The depth of MinII is 0.1m, the distortion wave ampitude is up to SS Boo |0.2m. ST Boo |[Fe/H] = -1.76. Blazhko effect, Pi = 284d [07238]. SU Boo |P varies, current elements are given. SV Boo |[Fe/H] = -1.55. SW Boo |[Fe/H] = -1.12. P varies, current elements are given. SZ Boo |[Fe/H] = -1.68. TU Boo |P varies, current elements are given. TV Boo |[Fe/H] = -2.44. TW Boo |[Fe/H] = -1.46. P varies, current elements are given. TX Boo |P varies, current elements are given. TY Boo |P varies, current elements are given. TZ Boo |P varies, current elements are given. Magnitudes in the minima TZ Boo |vary, sometimes MinII becomes deeper than MinI. UU Boo |P varies, current elements are given. UW Boo |P varies, current elements are given. The depth of MinII is 0.1m UW Boo |pg. UY Boo |P varies. VW Boo |P varies, current elements are given. XY Boo |P varies, current elements are given. AC Boo |P varies, current elements are given. The light curve shape varies. AE Boo |[Fe/H] = -1.39. AO Boo |P varies, the mean P is given. AR Boo |P varies, current elements are given. BE Boo |P varies? BI Boo |In the region of the globular cluster NGC 5466. BK Boo |In the region of the globular cluster NGC 5466. BL Boo |V19 (NGC 5466), cluster member. [Fe/H] = -1.92. P varies. BN Boo |In the region of the globular cluster NGC 5466. BO Boo |Blazhko effect. BR Boo |[Fe/H] = -1.03. BU Boo |Blazhko effect? BW Boo |MinII - MinI = 0.45P (1991). BX Boo |VB A (B 9.6m, 35", 156{deg}, 2007). CC Boo |z = 0.172. CD Boo |z = 1.045. CE Boo |Multiple. CK Boo |P varies, current elements are given. The light curve shape varies. CM Boo |[Fe/H] = -1.48. DE Boo |Porb = 125.4d. DM Boo |X-ray source. DQ Boo |VB AB (A 9.64m; B 10.92m, 9", 151{deg}, 1991). DU Boo |O'Connell effect. EF Boo |P varies, current elements are given. EQ Boo |MinII - MinI = 0.399P. VB AB (A 9.4m; B 10.1m, 1.3", 271{deg}, EQ Boo |2005). FL Boo |VB AB (A 10.04m; B 10.37m, 7", 26{deg}, 1991). FP Boo |P varies? Current elements are given. FS Boo |Erroneously named at a wrong position because of a misprint. See FS Boo |V0581 Aur. GM Boo |P varies, current elements are given. GN Boo |P varies, current elements are given. GQ Boo |P varies, current elements are given. GS Boo |P varies, current elements are given. GV Boo |P varies, current elements are given. GX Boo |Type DSCT with a twice shorter period is possible. HK Boo |SB2. HQ Boo |VB A (B 15.0mV, 24", 21{deg}, 1998). The tabulated amplitude can be HQ Boo |influenced by the companion. V0381 Boo |P1 is presented in the Table. P0 = 0.534137d; P1/P0 = 0.7457. V0383 Boo |P1 is presented in the Table. P0 = 0.472061d; P1/P0 = 0.7439. V0384 Boo |P1 is presented in the Table. P0 = 0.532235d; P1/P0 = 0.7460. V0386 Boo |P1 is presented in the Table. P0 = 0.555941d; P1/P0 = 0.7457. V0388 Boo |P1 is presented in the Table. P0 = 0.527220d; P1/P0 = 0.7460. V0392 Boo |Additional non-radial mode, P = 0.2909421d; P(Blazhko) = 27.6d. V0394 Boo |P1 is presented in the Table. P0 = 0.478545d; P1/P0 = 0.7449. V0395 Boo |P0 is presented in the Table. P1 = 0.345662d; P1/P0 = 0.7433. V0396 Boo |P1 is presented in the Table. P0 = 0.536540d; P1/P0 = 0.7464. V0397 Boo |P1 is presented in the Table. P0 = 0.506502d; P1/P0 = 0.7440. V0398 Boo |Additional non-radial mode, P = 0.2645555d; P(Blazhko) = 14.1d. V0399 Boo |P1 is presented in the Table. P0 = 0.492554d; P1/P0 = 0.7453. V0401 Boo |P1 is presented in the Table. P0 = 0.493517d; P1/P0 = 0.7444. V0403 Boo |P1 is presented in the Table. P0 = 0.564890d; P1/P0 = 0.7457. V0405 Boo |P1 is presented in the Table. P0 = 0.546206d; P1/P0 = 0.7453. V0407 Boo |VB A (14.1mV; B 14.5mV, 22", 113{deg}, 1998). V0411 Boo |P1 is presented in the Table. P0 = 0.476987d; P1/P0 = 0.7442. V0412 Boo |P1 is presented in the Table. P0 = 0.483115d; P1/P0 = 0.7444. V0413 Boo |P1 is presented in the Table. P0 = 0.480226d; P1/P0 = 0.7440. V0414 Boo |Additional non-radial mode, P = 0.324200d; P(Blazhko) = 36.6d. V0415 Boo |P1 is presented in the Table. P0 = 0.552367d; P1/P0 = 0.7457. V0421 Boo |Multiperiodic. V0423 Boo |Blazhko effect. P varies? V0424 Boo |Blazhko effect. V0426 Boo |The period in the Table is for suspected eclipsing variations. V0426 Boo |Pulsations: P = 0.040264d. V0429 Boo |O'Connell effect. V0432 Boo |Multiperiodic. V0433 Boo |Multiperiodic. V0434 Boo |Multiperiodic. V0435 Boo |Multiperiodic. V0444 Boo |Multiperiodic. V0445 Boo |Blazhko effect. V0447 Boo |Multiperiodic. V0450 Boo |P varies. gam Boo |VB A (A speckle binary, 0.07", 78{deg}, 1975, unresolved on several gam Boo |other dates; B 12.7m, 48", 121{deg}, 1998). kap 2 Boo |Multiperiodic. VB A (B 6.69m, F2V, SB1, 14", 237{deg}, 2009). ksi Boo |VB AB (4.73m, 7.04m, a = 4.9", Porb = 150 y). i Boo |VB B (A = NSV 20241, 5.31m Hp, G0; B 6.09m Hp, a = 3.8", e = 0.43, i Boo |Porb = 225 y); combined (A + B) magnitudes are tabulated. P varies i Boo |strongly, current elements are given. R Cae |SiO maser. U Cae |[Fe/H] = -1.11. Blazhko effect? V Cae |[Fe/H] = -2.00. X Cae |Multiperiodic. RR Cae |d = 0.02P. RX Cae |Variability type and spectral type do not agree. RZ Cae |VB (7.9m, 9.4m, 3", 222{deg}, 1993). SX Cae |A twice shorter period is also possible. U Cam |Triply periodic; other periods are 400d and 220d. V Cam |H2O, SiO maser. Y Cam |P varies, current elements are given. According to [N0223], MinI = Y Cam |2424443.4806 + 3.30552340d x E + 0.1564d x sin(0.011052{deg} x E + Y Cam |225.8{deg}) + 0.0452d x sim(0.022105 x E + 65.49{deg}). Superposed Y Cam |are pulsations with an amplitude up to 0.07m and P = 0.066457537d. Z Cam |Porb = 0.2898406d. RR Cam |Biperiodic; the other period is P0 = 223d. RS Cam |Triply periodic; other periods are 160d and 966d. RT Cam |H2O maser. RU Cam |[A/H] = 0.9. P varies. An unusual CWA variable with a carbon RU Cam |spectrum. In 1965, the star has abruptly changed the character of RU Cam |its variations, from nearly-regular, large-amplitude ones to mostly RU Cam |chaotic, with much smaller amplitude, sometimes decreasing to RU Cam |nearly zero. RV Cam |Multiperiodic. VB (0.07", 222{deg}, 1995) from speckle RV Cam |interferometry. RX Cam |SB, Porb = 1114d. RY Cam |VB (0.1", 350{deg}, 1997) from speckle interferometry. RZ Cam |[Fe/H] = -1.01. SS Cam |d = 0.06P. P varies, current elements are given. ST Cam |Triply periodic; other periods are 202d and 1580d. SU Cam |P varies, mean elements are given. Period variations have a SU Cam |possible period somewhat longer than 40 years. SZ Cam |ADS 2984B (A 6.93m; AB 18", 305{deg}, 2008). A very complex SZ Cam |multiple star; for component identifications see [N0228]. In the SZ Cam |open cluster NGC 1502. P varies, current elements are given. TW Cam |[Fe/H] = -0.8. TX Cam |VB A (B 16.6mpg, 8" nf). SiO maser. UU Cam |P varies, current elements are given. UY Cam |[Fe/H] = -1.33. WW Cam |MinII - MinI = 0.495P. XX Cam |Only one deep minimum near JD 2429632. No strong IR excess. P = XX Cam |36:d in maximum [N0230]. AF Cam |Porb = 0.2306d. AG Cam |SiO maser. AH Cam |VB A (B 14.32m, 7", 35{deg}, 1999). P varies, current elements are AH Cam |given. Blazhko effect with P = 11.0d [00232]. AK Cam |P varies, current elements are given. AL Cam |P varies, current elements are given. AO Cam |P varies, current elements are given. AS Cam |d = 0.02P. DII = 0.06P. MinII - MinI = 0.437P. Long-period apsidal AS Cam |motion. Third body, P = 805d. According to [N0236], pulsations with AS Cam |P = 0.913d and amplitude 0.02m are observed outside minima. AX Cam |VB (Porb = 6.644y, a = 0".554, e = 0.660). AY Cam |d = 0.02P. BD Cam |SB1, Porb = 596d. BL Cam |Multiperiodic; P varies [N0237]. BM Cam |SB1, Porb = 80.1745d, e = 0.35. BT Cam |Multiperiodic. P2 = 0.0079d, other periods. BW Cam |H2O, OH maser. BX Cam |H2O, SiO, OH maser. BY Cam |Other detected periods: 7.3d; 145d. BZ Cam |In a nebula. CE Cam |SB? CH Cam |The central star of the planetary nebula NGC 1501. Multiperiodic. CI Cam |A single strong outburst in 1998. According to [N0245], CI Cam |multiperiodic pulsations are observed outside the outburst, the CI Cam |dominating periods being 0.41521d and 0.26647d. Porb = 19.407d. CL Cam |SB1, Porb = 20.8d. CM Cam |SB1, Porb = 3770d. CS Cam |VB A (B 8.22m, 2", 164{deg}, 1991). doubt which of the components CS Cam |varies. CV Cam |VB AB (9.80m, 10.84m, 4", 44{deg}, 1991). CZ Cam |The detected semiregular variations are not typical of the spectral CZ Cam |type. DL Cam |VB A (B 6.96m, 10", 308{deg}, 1991). DM Cam |VB AaAb (7.82m, 8.10m, 0".1, 170{deg}, 1991). FH Cam |Alternatively, can be a pulsating star with a twice shorter period. FT Cam |Porb = 0.074990d. GS Cam |VB A (8.39mJ, Sp C; B 12.09mJ, 23", 219{deg}, 2000). There remains HT Cam |Porb = 0.060d. IQ Cam |Biperiodic. Second periodicity: P = 0.3248d. LL Cam |SiO maser. LQ Cam |SiO maser. LS Cam |Porb = 0.143d. LU Cam |Porb = 0.15d. LW Cam |Porb = 0.06754658d. MM Cam |Chromospherically active giant, slow photometric variations. MU Cam |The orbital period is tabulated. The spin period from photometry is MU Cam |0.01374127d. MW Cam |Biperiodic, P2 = 0.1282d. NR Cam |O'Connell effect. V0524 Cam |Distortion wave: P = 0.499464d. V0525 Cam |Distortion wave: P = 0.461208d. V0534 Cam |MinII - MinI = 0.545P. V0542 Cam |Multiperiodic. P1 is presented in the Table; P0 = 0.174773d. VB A V0542 Cam |(11.70mV; B 13.55mV, 17", 191{deg}, 1999). V0549 Cam |MinII - MinI = 0.543P. O'Connell effect. V0565 Cam |VB A (B 14.9mF, 7", 139{deg}, 2000); the amplitude in the Table is V0565 Cam |too low because of the companion. V0588 Cam |Period varies. V0602 Cam |Type SR with P = 92d is not excluded. V0609 Cam |VB B (A 11.7m; AB 26", 239{deg}, 2000; C 14.2m, AC 38", 302{deg}, V0609 Cam |2000). V0610 Cam |P1 is presented in the Table. P0 = 0.47921d6; P1/P0 = 0.7443. R Cnc |OH, H2O, SiO maser. S Cnc |In the region of the open cluster NGC 2632 (Praesepe). P varies? T Cnc |SiO maser. U Cnc |In the region of the open cluster NGC 2632 (Praesepe). V Cnc |VB A (B 13.7m, 9", 276{deg}, 2002). W Cnc |H2O, SiO maser. X Cnc |Other periods suspected. SB?, Porb = 491.4:d. Y Cnc |Blazhko effect. RS Cnc |Multiperiodic, P2 = 128.760d. H2O, SiO maser. RW Cnc |Blazhko effect periods: 29.9d, 91.1d [02088]. [Fe/H] = -1.67. RY Cnc |In the region of the open cluster NGC 2632 (Praesepe). P varies, RY Cnc |current elements are tabulated. SS Cnc |[Fe/H] = -0.07. SW Cnc |P varies? SY Cnc |Porb = 0.38d. SZ Cnc |SiO maser. TT Cnc |P varies, current elements are tabulated. Blazhko effect, P = TT Cnc |89.3d. [Fe/H] = -1.57. TU Cnc |P varies, current elements are tabulated. TX Cnc |In the open cluster NGC 2632 (Praesepe). P varies, current elements TX Cnc |are tabulated. TY Cnc |P varies, current elements are tabulated. UV Cnc |In the region of the open cluster NGC 2632 (Praesepe). VZ Cnc |P2 = 0.142804d. Beat period: 0.716292d. WW Cnc |P varies, current elements are tabulated. WY Cnc |VB A (B+C 12.5m; B 25", 356{deg}, 1998; C 28", 1{deg}, 1998). P WY Cnc |varies, current elements are tabulated. XX Cnc |In the region of the open cluster NGC 2632 (Praesepe). YZ Cnc |Porb = 0.0868d. AC Cnc |Physical variations, additional minima were reported. AE Cnc |VB A (B 15.5m, 11", 18{deg}, 2000). AF Cnc |Blazhko effect, P = 27.23d. AG Cnc |In the region of the open cluster NGC 2682 (M 67). SB2, Porb = AG Cnc |2.823094d. AH Cnc |P varies, quadratic term +1.56d x 10^(-10) x E^2. In the open AH Cnc |cluster NGC 2682 (M 67), probable member. AK Cnc |Porb = 0.0651d. AN Cnc |[Fe/H] = -1.45. AO Cnc |P varies? AP Cnc |Blazhko effect? AR Cnc |The period tabulated is for eclipses that occur, in quiescence, AR Cnc |from the V = 18.7 level. AS Cnc |[Fe/H] = -1.89. AT Cnc |Surrounded with a filamentary nebula, which is presumably a Nova AT Cnc |remnant. AU Cnc |In the open cluster NGC 2632 (Praesepe). AV Cnc |In the open cluster NGC 2632 (Praesepe). AW Cnc |In the open cluster NGC 2632 (Praesepe). AX Cnc |In the open cluster NGC 2632 (Praesepe). AY Cnc |In the open cluster NGC 2632 (Praesepe). AZ Cnc |In the open cluster NGC 2632 (Praesepe). BB Cnc |In the open cluster NGC 2632 (Praesepe). BC Cnc |In the open cluster NGC 2632 (Praesepe). BD Cnc |In the open cluster NGC 2632 (Praesepe). BE Cnc |In the open cluster NGC 2632 (Praesepe). BF Cnc |VB A (B 16.7mV, 9", 37{deg}, 2000). Blazhko effect? BG Cnc |In the open cluster NGC 2632 (Praesepe). BM Cnc |SB, Porb = 585.4154d. BN Cnc |In the open cluster NGC 2632 (Praesepe). Multiperiodic. BO Cnc |P2 = 270d. BQ Cnc |Multiperiodic. SB2. In the open cluster NGC 2632 (Praesepe). BR Cnc |Multiperiodic. In the open cluster NGC 2632 (Praesepe). BS Cnc |Multiperiodic. In the open cluster NGC 2632 (Praesepe). BT Cnc |Multiperiodic. In the open cluster NGC 2632 (Praesepe). BU Cnc |Multiperiodic. In the open cluster NGC 2632 (Praesepe). BV Cnc |Multiperiodic. In the open cluster NGC 2632 (Praesepe). BW Cnc |Multiperiodic. In the open cluster NGC 2632 (Praesepe). BX Cnc |Multiperiodic. In the open cluster NGC 2632 (Praesepe). BY Cnc |In the open cluster NGC 2632 (Praesepe). BZ Cnc |In the open cluster NGC 2632 (Praesepe). CC Cnc |Porb = 0.07352d. In the region of the open cluster NGC 2632 CC Cnc |(Praesepe). CD Cnc |In the open cluster NGC 2632 (Praesepe). CE Cnc |In the open cluster NGC 2632 (Praesepe). CF Cnc |In the open cluster NGC 2632 (Praesepe). CG Cnc |In the open cluster NGC 2632 (Praesepe). CH Cnc |In the open cluster NGC 2632 (Praesepe). CI Cnc |In the open cluster NGC 2632 (Praesepe). CK Cnc |In the open cluster NGC 2632 (Praesepe). CL Cnc |In the open cluster NGC 2632 (Praesepe). CM Cnc |In the open cluster NGC 2632 (Praesepe). CN Cnc |In the open cluster NGC 2632 (Praesepe). CO Cnc |In the open cluster NGC 2632 (Praesepe). CP Cnc |In the open cluster NGC 2632 (Praesepe). CR Cnc |In the open cluster NGC 2632 (Praesepe). CS Cnc |In the open cluster NGC 2632 (Praesepe). CU Cnc |VB A (B = CV Cnc, 10", 348{deg}, 2001, common proper motion). In CU Cnc |the region of the open cluster NGC 2632 (Praesepe), non-member. CU Cnc |Eclipses: 11.67 - 11.82V, MinII 11.75V, D = 0.03P, Min = CU Cnc |2450208.5068 CV Cnc |VB Bab (0.8", 200{deg}, 2006; A = CU Cnc, AB 10", 348{deg}, 2001, CV Cnc |common proper motion). In the region of the open cluster NGC 2632 CV Cnc |(Praesepe), non-member. CW Cnc |H2O maser. CY Cnc |In the open cluster NGC 2632 (Praesepe). DD Cnc |In the open cluster NGC 2632 (Praesepe). DF Cnc |In the region of the open cluster NGC 2632 (Praesepe), non-member? DG Cnc |In the region of the open cluster NGC 2632 (Praesepe), non-member? DH Cnc |In the open cluster NGC 2632 (Praesepe). DI Cnc |In the open cluster NGC 2632 (Praesepe). DK Cnc |In the region of the open cluster NGC 2632 (Praesepe). DL Cnc |In the open cluster NGC 2632 (Praesepe). DM Cnc |In the open cluster NGC 2632 (Praesepe). DN Cnc |In the open cluster NGC 2632 (Praesepe). DO Cnc |In the open cluster NGC 2632 (Praesepe). DP Cnc |In the open cluster NGC 2632 (Praesepe). DQ Cnc |In the region of the open cluster NGC 2632 (Praesepe), non-member? DR Cnc |In the open cluster NGC 2632 (Praesepe). DS Cnc |In the region of the open cluster NGC 2632 (Praesepe), non-member? DT Cnc |In the open cluster NGC 2632 (Praesepe). DU Cnc |In the open cluster NGC 2632 (Praesepe). DY Cnc |In the open cluster NGC 2632 (Praesepe). DZ Cnc |In the open cluster NGC 2632 (Praesepe). EE Cnc |In the open cluster NGC 2632 (Praesepe). EG Cnc |Porb = 0.05997d. EH Cnc |P varies, current elements are tabulated. EI Cnc |VB AB (1.4", 77{deg}, 2005). EL Cnc |In the open cluster NGC 2632 (Praesepe). EM Cnc |In the open cluster NGC 2632 (Praesepe). EN Cnc |In the open cluster NGC 2632 (Praesepe). EO Cnc |In the open cluster NGC 2632 (Praesepe). EP Cnc |Multiperiodic. In the region of the open cluster NGC 2632 EP Cnc |(Praesepe). EQ Cnc |In the open cluster NGC 2632 (Praesepe). ER Cnc |In the open cluster NGC 2632 (Praesepe). ES Cnc |In the region of the open cluster NGC 2682 (M 67). ET Cnc |In the open cluster NGC 2682 (M 67). EU Cnc |In the open cluster NGC 2682 (M 67). EV Cnc |O'Connell effect. A blue straggler in the open cluster NGC 2682 (M EV Cnc |67). EW Cnc |Multiperiodic. A blue straggler in the open cluster NGC 2682 (M EW Cnc |67). EX Cnc |Multiperiodic. A blue straggler in the open cluster NGC 2682 (M EX Cnc |67). EY Cnc |In the open cluster NGC 2682 (M 67). FL Cnc |Multiperiodic. FM Cnc |Blazhko effect? FN Cnc |Blazhko effect, P = 50.3d? FP Cnc |VB A (B 12.3mV, M3, 14", 240{deg}, 2004). FV Cnc |In the open cluster NGC 2632 (Praesepe). SB2, Porb = 2.981781d. GS Cnc |VB A (12.5mV; B 12.7mV, 10", 267{deg}). GY Cnc |Eclipses of different depth, from all all outburst brightness GY Cnc |levels. The light elements for eclipses are tabulated. GZ Cnc |Porb = 0.08825d. HI Cnc |In the open cluster NGC 2632 (Praesepe). HK Cnc |Multiperiodic. HM Cnc |Two white dwarfs on a very-short-period orbit. HN Cnc |P varies, current elements are tabulated. HO Cnc |VB AB (9.62m, 9.76m, 3", 1{deg}, 2011). HP Cnc |VB AB (9.91m, 10.09m, 1.4", 168{deg}, 2010). HQ Cnc |In the open cluster NGC 2682 (M 67), non-member. HR Cnc |In the open cluster NGC 2682 (M 67). HS Cnc |The light curve shape varies. In the open cluster NGC 2682 (M 67). HT Cnc |Porb = 1.358766d. In the open cluster NGC 2682 (M 67). HU Cnc |SB1, Porb = 18.396d. In the open cluster NGC 2682 (M 67). HV Cnc |In the open cluster NGC 2682 (M 67). HW Cnc |SB2, Porb = 10.05525d. In the open cluster NGC 2682 (M 67). HX Cnc |SB, Porb = 2.66059. In the open cluster NGC 2682 (M 67). HY Cnc |In the open cluster NGC 2682 (M 67). HZ Cnc |Multi-mode pulsations at a time scale of hours. IO Cnc |P varies? KK Cnc |VB (the NW component varies). Superhumps: P = 0.060818d. KQ Cnc |Blazhko effect? KV Cnc |Blazhko effect, P = 42d:. KZ Cnc |In the region of the open cluster NGC 2682 (M 67). LN Cnc |In the region of the open cluster NGC 2682 (M 67). Type RRC with a LN Cnc |twice shorter period is also possible. LO Cnc |In the region of the open cluster NGC 2682 (M 67), probably LO Cnc |non-member. LP Cnc |In the region of the open cluster NGC 2682 (M 67). LT Cnc |Pulsations at a timescale of about an hour. SB, Porb = 6.1163d. LV Cnc |Multiperiodic, P2 = 0.0025d. SB, Porb = 0.0567d. Cataclysmic LV Cnc |spectrum. MR Cnc |Pulsates in the first overtone (see Table) and fundamental (Max = MR Cnc |2454701.537 + 0.536525d x E) modes. P1/P0 = 0.7462. MY Cnc |Double-mode, with a radial and a none-radial modes excited. The MY Cnc |second light elements: Max = 2454700.652 + 0.281995d x E. P2/P1 = MY Cnc |0.9824. NN Cnc |P1 is presented in the Table. P0 = 0.478318d; P1/P0 = 0.7448. NP Cnc |P1 is presented in the Table. P0 = 0.498566d; P1/P0 = 0.7449. NU Cnc |P1 is presented in the Table. P0 = 0.472146d; P1/P0 = 0.7432. NW Cnc |P1 is presented in the Table. P0 = 0.481136d; P1/P0 = 0.7446. OO Cnc |P1 is presented in the Table. P0 = 0.505835d; P1/P0 = 0.7443. PR Cnc |P1 is presented in the Table. P0 = 0.482865d; P1/P0 = 0.7450. PS Cnc |P1 is presented in the Table. P0 = 0.478487d; P1/P0 = 0.7442. PU Cnc |P1 is presented in the Table. P0 = 0.489181d; P1/P0 = 0.7443. PW Cnc |VB A (B = NEXT STAR IN THE LIST, 12", 171{deg}, 1997). PX Cnc |A twice longer period is not excluded. VB B (A = PREVIOUS STAR IN PX Cnc |THE LIST; AB 12", 171{deg}, 1997). QQ Cnc |P1 is presented in the Table. P0 = 0.483002d; P1/P0 = 0.7441. QU Cnc |P1 is presented in the Table. P0 = 0.542956d; P1/P0 = 0.7456. kap Cnc |SB, P = 6.39616d. R CVn |OH, SiO maser. U CVn |OH, H2O maser. V CVn |Multiperiodic, P2 = 186d. OH, H2O, SiO maser. W CVn |[Fe/H] = -1.22. P varies, current elements for 1999 are tabulated. W CVn |Quadratic elements: Max = 2421402.421 + 0.55175963d x E -0.4156d x W CVn |10^{-10}E^2 [N0347]. Y CVn |Multiperiodic, other periods: 273d, 160d. Z CVn |[Fe/H] = -1.98. P varies, elements valid after 1999 are tabulated. Z CVn |Blazhko effect, P = 22.75d. RR CVn |[Fe/H] = -1.08. RS CVn |d = 0.033P. P varies, current elements are tabulated. Distorsion RS CVn |wave: {Delta}(m) from 0.09m to 0.20m, P = 4.7917d [07209]. RU CVn |[Fe/H] = -1.38. P varies, current elements are tabulated. RV CVn |V141 (M3 = NGC 5272), cluster non-member. P varies, current RV CVn |elements are tabulated. RX CVn |[Fe/H] = -1.31. RZ CVn |[Fe/H] = -1.84. P varies, current elements are tabulated. SS CVn |[Fe/H] = -1.37. P varies? Blazhko effect? ST CVn |[Fe/H] = -1.07. SV CVn |[Fe/H] = -2.20. P varies, current elements are tabulated. SW CVn |P varies, quadratic term +2.0334d x 10^{-10}E^2. [Fe/H] = -1.53. TX CVn |Porb = 199.0:d. UU CVn |In the region of the globular cluster NGC 5466. P varies, current UU CVn |elements are tabulated. Blazhko effect? UV CVn |In the region of the globular cluster NGC 5466; cluster non-member. UV CVn |P varies, current elements are tabulated. UW CVn |In the region of the globular cluster NGC 5466. UZ CVn |[Fe/H] = -1.89. P varies, current elements for Hipparcos UZ CVn |observations are tabulated. VW CVn |P varies, current elements for 1999 are tabulated. The light curve VW CVn |shape varies? WW CVn |Blazhko effect. WY CVn |V205 (M3 = NGC 5272). WZ CVn |V206 (M3 = NGC 5272). Blazhko effect, P = 25.4d? XX CVn |V113 (M3 = NGC 5272). XY CVn |[Fe/H] = -2.03. XZ CVn |[Fe/H] = -1.46. P varies strongly, elements for JD 2455939 - XZ CVn |2456462 are tabulated. YY CVn |P varies strongly, elements for JD 2455939 - 2456462 are tabulated. AA CVn |[Fe/H] = -1.78. AC CVn |Blazhko effect. AD CVn |[Fe/H] = -1.39. VB A (B 16.0mV, 10", 147{deg}, 1998). AF CVn |[Fe/H] = -1.19. AG CVn |[Fe/H] = -2.01. AH CVn |[Fe/H] = -1.93. AI CVn |Multiperiodic. AK CVn |[Fe/H] = -1.62. AM CVn |Multiperiodic; also Min = 2448742.5610 + 0.011906623d x E AM CVn |(presumably orbital variations) and other periods. The tabulated AM CVn |period (double wave) can be interpreted as positive superhumps. AM CVn |Often con AN CVn |[Fe/H] = -1.54. AP CVn |VB A (13.6mV; B 13.9mV, 23", 183{deg}, 2000). AQ CVn |A probable field horizontal-branch star. A single strong AQ CVn |brightening, about 20 minutes duration, was observed. BD CVn |Blazhko effect? BF CVn |VB A (B = NSV 6039, 13.16m, dM3.5e, 16", 226{deg}, 1991). Flares in BF CVn |the combined light of the pair ({Delta} U up to 0.95m) were BF CVn |observed [02195]. BG CVn |Multiperiodic. Also P = 780s (0.00903d), etc.; different periods BG CVn |dominate at different times. BI CVn |P varies, current elements are tabulated. BM CVn |SB, Porb = 20.625d. Somewhat different periods were observed during BM CVn |different seasons of observations. BN CVn |P varies, quadratic term +1.7372d x 10^{-10}E^2. BO CVn |P varies, current elements are tabulated. CH CVn |SB. CP CVn |SB. CS CVn |HIPPARCOS data are in contradiction with the M0V spectral type. CU CVn |Multiperiodic. CX CVn |VB (A 9.5mHp, B 13.2mHp, 1.3", 308{deg}, 1991). DD CVn |Multiperiodic. DE CVn |EA-like in U and B light, EB at longer wavelengths. Amplitude DE CVn |decreases with wavelength. DG CVn |VB ({Delta}(mK) = 0.16m, 0.17", 253{deg}, 2000). DK CVn |The light curve shape varies strongly. DN CVn |P varies strongly [00001]. DY CVn |P varies, current elements are tabulated. VB A (B 15m, 5", DY CVn |250{deg}, 1998). DZ CVn |Blazhko effect. EF CVn |P varies? EG CVn |P varies, current elements are tabulated. EI CVn |P varies? FL CVn |Blazhko effect? FT CVn |Blazhko effect. FV CVn |P varies, current elements are tabulated. GP CVn |Light elements for eclipses: Min = 2453796.248245 + 0.062959041d x GP CVn |E [81139]. GR CVn |The Table presents the period of first-overtone pulsations; P0 = GR CVn |0.486651d. P1/P0 = 0.7443. HK CVn |P1 is presented in the Table. P0 = 0.478824d; P1/P0 = 0.7442. HL CVn |P1 is presented in the Table. P0 = 0.555276d; P1/P0 = 0.7462. HM CVn |P1 is presented in the Table. P0 = 0.526289d; P1/P0 = 0.7459. HP CVn |P1 is presented in the Table. P0 = 0.479250d; P1/P0 = 0.7446. HQ CVn |Strong O'Connell effect. HS CVn |P1 is presented in the Table. P0 = 0.531760d; P1/P0 = 0.7451. HU CVn |The mean brightness slowly varies by about 0.1mV. The depths of HU CVn |MinI and MinII are about 0.1mV. HV CVn |P1 is presented in the Table. P0 = 0.514168d; P1/P0 = 0.7450. HX CVn |P1 is presented in the Table. P0 = 0.513224d; P1/P0 = 0.7452. IK CVn |A second-overtone RR Lyrae star. IY CVn |Blazhko effect. IZ CVn |Blazhko effect. KN CVn |Blazhko effect. KS CVn |Blazhko effect. KU CVn |Blazhko effect. KZ CVn |Blazhko effect. LL CVn |Blazhko effect. LN CVn |Blazhko effect. LO CVn |Blazhko effect. LP CVn |Blazhko effect. LR CVn |Blazhko effect. LS CVn |P1 = 0.35672d, P1/P0 = 0.7354. LV CVn |Blazhko effect. MP CVn |Blazhko effect. MU CVn |VB with NGC 5272 V 155 (V029 - V155: 2", 135{deg}, 2000). There can MU CVn |be confusion between the light elements of the two stars. MV CVn |VB with NGC 5272 V029 (V029 - V155: 2", 135{deg}, 2000). There can MV CVn |be confusion between the light elements of the two stars. MZ CVn |Blazhko effect. NO CVn |Blazhko effect. NP CVn |Blazhko effect. NR CVn |Blazhko effect. NS CVn |VB A (B 0.5", 139{deg}, 1993). Resolved by the Hubble Space NS CVn |Telescope. NU CVn |VB B (AB 0.5", 139{deg}, 1993). Resolved by the Hubble Space NU CVn |Telescope. NX CVn |Blazhko effect? NY CVn |Blazhko effect. OO CVn |VB (15.6mG; companion 15.3mG, 1.2", 282{deg}, 2000). OT CVn |Blazhko effect. PS CVn |P1 = 0.35072d, P1/P0 = 0.7314; P2 = 0.28160d, P2/P1 = 0.8029. PV CVn |Blazhko effect. QR CVn |Blazhko effect? V0345 CVn |Blazhko effect. V0351 CVn |Blended. V0354 CVn |A close pair within 1"? V0355 CVn |P0 = 0.4530, P1/P0 = 0.7419. V0356 CVn |P0 = 0.4762, P1/P0 = 0.7438. V0357 CVn |Blazhko effect. V0359 CVn |P0 = 0.48530d, P1/P0 = 0.7439. V0362 CVn |A close pair. V0367 CVn |Blazhko effect. V0369 CVn |In a close pair of two RR Lyrae variables. V0370 CVn |In a close pair of two RR Lyrae variables. V0377 CVn |Blazhko effect. V0380 CVn |Blended. V0394 CVn |P0 = 0.4778805d, P1/P0 = 0.7449. V0400 CVn |Blazhko effect. V0411 CVn |Blazhko effect. V0416 CVn |P0 = 0.479, P1/P0 = 0.74. The star switched from RRAB variations to V0416 CVn |double-mode pulsations in 1992. According to [g1066], it was an V0416 CVn |RRAB star again in 2007. V0418 CVn |Blazhko effect. V0419 CVn |Blazhko effect. V0420 CVn |Blazhko effect. V0436 CVn |VB B (A 14.6mG, B 15.6mG; AB 5", 219{deg}, 2000). V0440 CVn |Blazhko effect. V0446 CVn |P0 = 0.48017d, P1/P0 = 0.7445. V0453 CVn |Blazhko effect? V0454 CVn |Blazhko effect. V0455 CVn |Blazhko effect. V0459 CVn |Blazhko effect. V0460 CVn |P1 = 0.36812, P1/P0 = 0.7307. V0463 CVn |Blazhko effect. V0465 CVn |P0 = 0.48209d, P1/P0 = 0.7491. V0466 CVn |Period varies. V0467 CVn |Blazhko effect. V0469 CVn |Blazhko effect. V0474 CVn |Blazhko effect. V0475 CVn |Period varies? alf 2 CVn |Epoch of Max is tabulated. VB A (2.81mHp; B 5.86mHp, 19", 229{deg}, alf 2 CVn |1991). R CMa |P varies, current elements are tabulated. Y CMa |SiO maser. Z CMa |Speckle interferometry: VB (0.1", 305{deg}, 1993). RR CMa |P varies, current elements are tabulated. RT CMa |P varies, current elements are tabulated. RX CMa |P varies. RZ CMa |P varies? Current elements are tabulated. SS CMa |P varies? Current elements are tabulated. SW CMa |MinII - MinI = 0.31P. e = 0.32. SY CMa |VB A (companions: 7", 156{deg}; 14", 270{deg}, 1994). TT CMa |SiO maser. UU CMa |P varies, current elements are tabulated. UZ CMa |Multiperiodic, P2 = 38.4d. VY CMa |In the region of the young open cluster NGC 2362. Embedded in a VY CMa |reflecting nebula. ADS 6033 A; numerous companions are probably VY CMa |details of the nebula. H2O, OH, SiO maser. AO CMa |In the region of the open cluster Ruprecht 18. AS CMa |d = 0.04P. BG CMa |VB (5", 20{deg}, 1999). The variable is probably the southern BG CMa |component. BQ CMa |In the region of the open cluster NGC 2354. CE CMa |MinII - MinI = 0.663P. CG CMa |VB A (B 16m, 4", 261{deg}, 1999). CN CMa |[Fe/H] = 0.0. CV CMa |Currently, MinII - MinI = 0.46P. Apsidal motion. DL CMa |OH maser. DM CMa |No red star near the published position. Cataclysmic? [00001]. DS CMa |VB A (B 15.8m, 9", 320{deg}, 1998). DZ CMa |The elements for fundamental mode are tabulated. P1 = 1.64495d. EW CMa |VB (4.920mHp, 5.394mHp, 0.131", 324{deg}, 1991). SB, P = 0.261975d. EW CMa |Shell events. BCEP-like variations, P = 0.0918d [N0367]. Other EW CMa |reported periods: about 20d [N0366], 1.2572d [N0367]. EY CMa |Multiperiodic. EZ CMa |SB. In the ring nebula S308. In the region of the open cluster EZ CMa |Collinder 121. P2 = 1.18d was possible in 1988. FF CMa |In the region of the open cluster Collinder 132a. FN CMa |VB (A 5.685mHp; B 7.042mHp, 0.571", 116{deg}, 1991; C 9.0mV, B6V, FN CMa |18", 350{deg}, 2011). The range in the table is for the A+B pair. FN CMa |Associated with the nebula vB 95. The period needs confirmation. FR CMa |VB (A 5.55mV; B 9.7mV, 4", 23{deg}, 2003). FU CMa |VB Aab (6.52m, 0.1", 337{deg}, 2010; B 11,07m, 14", 232{deg}, FU CMa |1999). FV CMa |VB AB (5.7mV, 7.7mV, 0.1", 11{deg}, 2012). FZ CMa |In the HII region S 295. GG CMa |In the open cluster Cr 132a. GU CMa |VB AB (7.03m, 7.70m, 0.6", 198{deg}, 1991). In the HII region S GU CMa |293. HK CMa |In the region of the open cluster NGC 2287. HL CMa |Probably related to XM variables. The X-ray source 1E 0643.0-1648. HL CMa |Lx/Lopt is from 0.002 to 1. Porb = 0.2145d. HN CMa |Multiperiodic. HP CMa |Several possible periods or cycles were reported. VB A (B 8.21m, HP CMa |5", 220{deg}, 1999). HQ CMa |VB A (B 13.0m, 9", 220{deg}, 1999). HW CMa |Orbital eccentricity e = 0.500. II CMa |In the region of the open cluster Be 33. IK CMa |In the open cluster Be 33. IL CMa |Pulsation periods (unstable) of 1.19d and 1.28d were reported. IU CMa |VB (6.85m, 8.15m, 0.8", 156{deg}, 1991). IY CMa |VB (5.86mV, 7.60mV, 1.2", 43{deg}, 1999). KL CMa |Apsidal motion. MinII = 2448.171.228 + 1.762168d x E. VB A (B KL CMa |10.47m, 21", 43{deg}, 2011). KQ CMa |VB A (B 11.29mV, 7", 42{deg}, 1999). KY CMa |Mean brightness varies with P2 = 493d. LT CMa |Apsidal motion. MinII = 2448389.445 + 1.759503d x E. LX CMa |P = 4.362d according to [HIP]. MX CMa |In the region of the open cluster NGC 2362. NN CMa |Semiperiodic bursts (P = 210d). NO CMa |In the region of the open cluster Cr 140. NQ CMa |VB (9.9mV, 13.2mV, 5", 64{deg}, 1999). NS CMa |In the region of the open cluster NGC 2243. NT CMa |In the region of the open cluster NGC 2243. NU CMa |In the region of the open cluster NGC 2243. NV CMa |In the region of the open cluster NGC 2243. NW CMa |In the region of the open cluster NGC 2243. NX CMa |In the region of the open cluster NGC 2243. PX CMa |In the region of the open cluster Tombaugh 2. PY CMa |In the region of the open cluster Tombaugh 2. PZ CMa |In the region of the open cluster Tombaugh 2. QQ CMa |In the region of the open cluster Tombaugh 2. QR CMa |In the region of the open cluster Tombaugh 2. QS CMa |In the region of the open cluster Tombaugh 2. QT CMa |VB A (B 9", 252{deg}, 2000). QU CMa |In the region of the open cluster NGC 2354. QX CMa |Type EW is also possible. In the open cluster NGC 2362. V0347 CMa |VB A (B 13.5m, 8", 92{deg}, 1998). The tabulated magnitude at V0347 CMa |maximum is influenced by the companion. V0350 CMa |Multiperiodic, P2 = 0.7750d. VB A (6.332mHp; B 8.895mHp, 18", V0350 CMa |144{deg}, 1991). V0356 CMa |VB AB (2", 22{deg}, 2001; C 10.8m, 14", 116{deg}, 1999). V0367 CMa |Superposed variations with an amplitude up to 0.5m and a period of V0367 CMa |89d. V0377 CMa |A twice shorter period is not excluded. V0388 CMa |VB (9.1m, 9.1m, 3", 330{deg}, 1991). MinII - MinI = 0.61P. V0400 CMa |In the open cluster NGC 2204. V0401 CMa |In the open cluster NGC 2204. V0402 CMa |In the open cluster NGC 2204. V0403 CMa |In the open cluster NGC 2204. V0404 CMa |P varies, dP/dt = -0.47 x 10^(-5) d/yr. V0406 CMa |In the open cluster NGC 2243. V0407 CMa |In the open cluster NGC 2243. V0408 CMa |In the open cluster NGC 2243. V0409 CMa |Type EW with a twice longer period is also possible. In the open V0409 CMa |cluster NGC 2243. V0410 CMa |In the open cluster NGC 2243. V0411 CMa |In the open cluster NGC 2243. V0412 CMa |In the open cluster NGC 2243. V0413 CMa |In the open cluster NGC 2243. V0415 CMa |VB A (B 9.3m, 9", 335{deg}, 1999). V0416 CMa |P varies, dP/dt = 0.27 x 10^(-5) d/yr. V0422 CMa |In the open cluster NGC 2362. V0432 CMa |MinII - MinI = 0.53P. V0436 CMa |The data for 1SWASP J061236.44-281553.0 in [82030] are combined V0436 CMa |measurements for a non-variable star (V = 14.8m) near the SuperWASP V0436 CMa |position and the real variable. V0441 CMa |Multiperiodic. V0442 CMa |Multiperiodic. V0445 CMa |MinII - MinI = 0.56P. V0450 CMa |MinII - MinI = 0.73P. V0451 CMa |For SRD light elements, see the Table. Eclipses: Min = 2453707.98 + V0451 CMa |8.2958d x E, amplitude 0.2m. bet CMa |Multiperiodic. iot CMa |Non-radial pulsations? tau CMa |VB Aa, Ab (4.89mV, 5.33mV, 0.1", Porb = 154.9d; B 10.2mV, 9", tau CMa |93{deg}, 2002; C 11.2mV, 14". 87{deg}, 2002; E 9.7mV, Ab-E 0.9", tau CMa |88{deg}, 2012). ome CMa |P = 1.3719d in radial velocities was reported. S CMi |SiO maser. U CMi |Often shows double-peaked maxima, the second peak being usually U CMi |brighter. X CMi |{Delta} S = 3. Y CMi |Blazhko effect. RX CMi |MinII - MinI = 0.52:P. The light elements need improvement. SY CMi |P varies. XZ CMi |P varies, current elements are given in the Table. YZ CMi |Quasi-periodic BY variations: 11.12 - 11.38mV, P = 2.7774d [00001]. AA CMi |[Fe/H] = -0.14. AG CMi |P varies, current elements are given in the Table. AH CMi |VB A (B 14.7m, 10", 120{deg}, 2000). AI CMi |OH, H2O maser. AL CMi |[Fe/H] = -0.85. AM CMi |P varies, current elements are given in the Table. AW CMi |P = 1.04d/N is possible. BB CMi |O'Connell effect. BG CMi |Intermediate polar. The orbital period is presented in the Table. BG CMi |Spin period: 0.010572993d (varies). BH CMi |O'Connell effect. BI CMi |Multiperiodic. BM CMi |VB A (B 14,5m, 7', 68grad, 2000). BO CMi |Several episodes of outburst-like activity. BU CMi |MinII - MinI = 0.37P. DE CMi |Multiperiodic. DL CMi |A twice shorter period is not excluded. DO CMi |Multiperiodic. P0 is tabulated. P1 = 0.14862d, P2 = 0.11908d, P3 = DO CMi |0.11617d. DR CMi |MinII - MinI = 0.669P. DY CMi |Superhumps: P = 0.060750d. Y Cap |H2O maser. RU Cap |OH, H2O, SiO maser. RV Cap |[Fe/H] = -1.61. Blazhko effect, P = 231.66d. RW Cap |P varies, current elements are given. RX Cap |[Fe/H] = -0.30. RY Cap |VB B (A 7.9mV; AB 7", 89{deg}, 1991). Mira classification [01731] RY Cap |seems improbable, no red stars around. SY Cap |Superhumps: P = 0.063759d. TW Cap |P varies, the Table presents current elements. [Fe/H] = -1.20. TY Cap |P varies, the Table presents current elements. UW Cap |P varies? VV Cap |Blazhko effect? VX Cap |[Fe/H] = -1.0. WY Cap |Blazhko effect? YZ Cap |[Fe/H] = -1.06. AN Cap |[Fe/H] = -1.1:. AS Cap |Porb = 49.137d. AV Cap |Porb = 9.3464d. AW Cap |Posc = 10.8 minutes. AZ Cap |VB (2.2", 140{deg}). BB Cap |VB (a = 0.14", Porb = 1.933 years). BC Cap |P2 = 57d. BM Cap |VB AB (9.68m, 9.84m, 6", 141{deg}, 2000). BN Cap |VB AB (8.90m, 9.00m, 2", 89{deg}, 2013). Probably the fainter BN Cap |component varies. BY Cap |Porb = 13.17d. BZ Cap |VB A (B 9", 346{deg}, 1998; C 8", 154{deg}, 1998). CR Cap |The first-overtone period is tabulated. P0 = 0.47302d. CR Cap |{Delta}(m)1/{Delta}(m)0 = 1.5. DF Cap |Multiperiodic. DM Cap |Porb = 0.2215d. DO Cap |Period varies strongly. DQ Cap |Blazhko effect [81005]. EG Cap |VB A (11.1mG; B 14.0mG, 7", 313{deg}, 2000). EH Cap |Double-mode pulsations. The Table contains light elements for the EH Cap |fundamental mode. P1/P0 = 0.7746. EM Cap |VB AB (A 14.3 mG; B 15.0mG, 4", 334{deg}, 2000). The variability EM Cap |range in the Table is for combined light. ER Cap |Other possible types: CWA:, EB: (with a twice longer period). EV Cap |Type EB with a twice longer period is not excluded. EY Cap |P1 is presented in the Table. P0 = 0.550510d, P1/P0 = 0.7463. FI Cap |Cluster non-member. Porb = 0.0923d. FP Cap |The range in the Table is for combined brightness of a blend of at FP Cap |least three stars. FU Cap |On the subgiant branch of the cluster's color-magnitude diagram; FU Cap |probably a blend. FX Cap |Blazhko effect? R Car |H2O, SiO maser. VB A (B 11.3m, 1.8", 140{deg}, 1978). Y Car |The elements for the fundamental mode are given in the Table (A = Y Car |0.58m). The first overtone: P1 = 2.5596d (A = 0.28m). P1/P0 = Y Car |0.7032. [Fe/H] = -0.33. SB (P = 1006.9d). VB A (B 12.22m, 12", Y Car |47{deg}, 2000; C 12.96m, 34", 33{deg}, 2000). RR Car |S6.5/1-. RT Car |In the region of the open cluster Tr 15. RY Car |VB A (B 14.1m, 14", 149{deg}, 1997). SU Car |SiO maser. SZ Car |In the region of the open cluster NGC 3114. UX Car |In the region of the open cluster IC 2581. VV Car |In the region of the open cluster C 1036-589, embedded in a nebula. VY Car |VB A (B 11.1m, 10.5", 153{deg}, 2000). WZ Car |P varies, the Table gives elements for 2451887 - 2455188. YZ Car |P varies, the Table gives elements for 2450541 - 2453024. SB, Porb YZ Car |= 657.3d. AE Car |In the region of the open cluster NGC 3532. AG Car |The central star of the planetary nebula PK 289-00 1. AW Car |d = 0.015P. AY Car |VB A (B 13.2m, 12", 182{deg}, 2000). The magnitudes in the Table AY Car |were influenced by the companion. BC Car |SiO maser. BL Car |In the region of the open cluster Tr 16. BO Car |VB A (B 11.6m, B8III, 14", 42{deg}, 1998). In the region of the BO Car |association Tr 15; non-member. BP Car |In the region of nebulae around Eta Carinae. The elements were BP Car |derived from ASAS-3 data, where the magnitudes are for a blend of BP Car |three stars. BS Car |In the region of the open cluster IC 2602. BX Car |Double maxima. CD Car |In the central region of the open cluster Cr 236. CF Car |VB A (B 12.3m, 20", 88{deg}, 2000; C 7.5", 110{deg}, 2000). In the CF Car |region of the open cluster NGC 3496. CG Car |Several close companions. CH Car |VB A (B 8", 194{deg}, 2000). CI Car |In the region of the open cluster NGC 3572. Several close CI Car |companions; the magnitudes in the Table were influenced by them. DF Car |A twice longer period is not excluded. DH Car |VB (4.5", 99{deg}, 2000). It is unclear which component varies. A DH Car |star with V = 13.2m in 14", 159{deg} and several other close DH Car |neighbors. DM Car |d = 0.040P. DN Car |A close blend of several components. DP Car |d = 0.034P. DU Car |In the region of the open cluster IC 2602. DW Car |In the region of the open cluster Cr 228. EE Car |VB A (B 5", 316{deg}, 2000). The magnitudes of the Table were EE Car |probably influenced with the companion. EG Car |VB (12.0mV, 13.4mV, 6", 280{deg}, 2000; also other companions). It EG Car |is unclear which component varies. In the region of the open EG Car |cluster NGC 3532. EH Car |VB (13.1mV, 13.7mV, 8", 317{deg}, 2000; also other companions). It EH Car |is unclear which component varies. EK Car |In the region of the open cluster NGC 3632. EM Car |MinII - MinI = 0.57P; apsidal motion? In the region of the open EM Car |cluster Tr 18. EQ Car |d = 0.030P. ER Car |In the region of the open cluster NGC 3532. ES Car |In the region of the open cluster NGC 3572. EV Car |P2 = 820d. EY Car |The Table presents the fundamental-mode period. P1 = 2.036d. FK Car |VB A (B 7", 237{deg}, 2000). FO Car |VB A (B 14m, 6", 90{deg}, 2000). FQ Car |In the region of the open cluster Tr 18. FS Car |In the region of the open cluster C1036-589. FU Car |VB A (11.2mV; B 11.6mV, 23", 305{deg}, 2000). FV Car |VB A (B 8", 59{deg}, 1998). FY Car |The mean brightness varies, P = 1036: days. GG Car |VB (8.88mHp, 11.58mHp, 0.3", 289{deg}, 1991). SB, Porb = 31.030d. GG Car |Photometry shows a single wave during the orbital period. Gas and GG Car |dust envelope. GH Car |In the region of the open cluster Tr 18. GI Car |In the region of the open cluster Tr 19. GK Car |In the region of the open cluster Tr 19. GL Car |In the region of the open cluster NGC 3572. Apsidal motion, P = GL Car |25.22 years. The elements in the Table are for the primary minimum GL Car |(JD 2454410 - 2455168). For the same time interval, MinII = 24548 GM Car |In the region of the open cluster C1036-589. GN Car |VB A (A 14.4mV, B 14.4mV; AB 14", 42{deg}, 2000). GR Car |MinII - MinI = 0.316P. DII = 0.05P. GV Car |In the region of the open cluster NGC 3512. GZ Car |The Table presents the light elements for the fundamental mode. GZ Car |First overtone: Max = 2443259.6 + 2.933762d x E. P1/P0 = 0.7054. HH Car |VB A (B 11.1m, 13", 337{deg}, 2000; C 12.2m, 6", 254{deg}, 2000; D HH Car |12.6m, 16", 11{deg}, 2000). HK Car |VB A (B 13.4mHp, 2", 91{deg}, 1991). HM Car |Multiple. HP Car |VB A (B 9.5m, 0.4", 177{deg}, 2010). The Table gives combined HP Car |magnitudes of the pair. HQ Car |P varies? HR Car |Associated with a nebula. HT Car |In the region of the open cluster IC 2581. HU Car |VB B (A 13.2mV, B 13.6mV; AB 13", 116{deg}, 2000). HV Car |d = 0.025P. HX Car |In the region of the open cluster NGC 3532. IK Car |In the region of the open cluster IC 2602. IN Car |A twice longer period is not excluded. IQ Car |In the region of the open cluster NGC 3532. IR Car |In the region of the open cluster NGC 3532. IU Car |[Fe/H] = -1.85. P varies, the elements in the Table are for JD IU Car |2454090 - 2455166. IW Car |Shorter-period oscillation: {Delta} V = 0.4m. Longer-period IW Car |oscillation: P = 1400d. IX Car |In a nebula. KK Car |SiO maser. MP Car |VB A (14.0mV; B 15.7mV, 12", 190{deg}, 2000). MZ Car |VB B (A 12.9mV, B 13.8mV; AB 15", 147{deg}, 2000). NO Car |VB A (B 3" sf). OY Car |The cycle in the Table is for superhumps. Eclipses: Min = OY Car |2443993.553839 + 0.0631209239 x E [N0394], D = 0.05P. The depth of OY Car |Min varies. PU Car |Blended. QU Car |Porb = 0.450d - 0.456d. Brightness variations sometimes reveal the QU Car |same period. QX Car |MinII = 2453630.997 + 4.47793d x E. DII = 0.11P. QY Car |SB1, P = 8.6d. In the region of the open cluster C 1010-577. QZ Car |Unresolved system of two SB1 stars, A (Porb = 20.73596d) and B QZ Car |(eclipsing), combined magnitudes are given in the Table. In the QZ Car |open cluster Collinder 228 and Eta Carinae nebula. V0338 Car |Ellipsoidal variations 9.19m - 9.48m; the narrow eclipse starts V0338 Car |from the level of 9.40m. V0341 Car |In the variable reflecting nebula IC 2220. In the region of the V0341 Car |open cluster NGC 2516. V0343 Car |SB, Porb = 133.92d. V0345 Car |SB, Porb = 1.13028d. V0348 Car |In the open cluster IC 2581. V0356 Car |In the open cluster NGC 2516. V0357 Car |SB, P = 6.74483d. V0361 Car |In the open cluster NGC 3293. V0365 Car |In the region of the open cluster NGC 3532. V0370 Car |In a nebula. In the region of the open cluster NGC 3324. SB2. V0372 Car |Second period 0.124151d. V0373 Car |In the open star cluster NGC 2516. V0374 Car |In the open star cluster NGC 2516. V0375 Car |P = 0.359d is also possible. V0378 Car |Multiperiodic. In the open cluster NGC 3293. V0379 Car |In the open cluster NGC 3293. Crowded. V0380 Car |In the open cluster NGC 3293. V0381 Car |In the region of the open cluster NGC 3293. The light elements in V0381 Car |the Table are for eclipses. Pulsations: {Delta} V = 0.06m, P = V0381 Car |0.1773d [N0397]. V0382 Car |In the region of the open cluster NGC 3532. V0384 Car |The mean brightness varies, P = 790d. V0385 Car |In the ring nebula RCW 58. SB1. V0391 Car |In the open cluster NGC 2516. V0392 Car |In the open cluster NGC 2516. V0395 Car |VB A (B 6", 144{deg}, 2000). V0399 Car |In the open cluster IC 2581. V0400 Car |Multiperiodic. In the region of the open cluster NGC 3293. V0401 Car |Multiperiodic. In the region of the open cluster NGC 3293. V0402 Car |In the region of the open cluster NGC 3293. V0403 Car |In the region of the open cluster NGC 3293. V0404 Car |In the region of the open cluster NGC 3293. V0405 Car |Multiperiodic. In the region of the open cluster NGC 3293. V0406 Car |Multiperiodic. In the region of the open cluster NGC 3293. V0407 Car |In the region of the open cluster IC 2602. V0408 Car |VB (4") or multiple. The magnitudes in the Table are for combined V0408 Car |brightness. In the HD catalog, the spectral type is K0. V0409 Car |Photometric Prot is given in the Table. Oscillations: P = 12.6 min V0409 Car |[68057]. V0410 Car |In the open cluster NGC 2516. V0412 Car |In the region of the open cluster NGC 3293. V0416 Car |In the region of the open cluster NGC 2516. V0417 Car |In the region of the open cluster NGC 2516. V0418 Car |In the region of the open cluster NGC 2516. V0419 Car |In the region of the open cluster NGC 2516. V0420 Car |In the region of the open cluster NGC 2516. V0421 Car |In the region of the open cluster NGC 2516. V0422 Car |In the region of the open cluster NGC 2516. V0424 Car |In the region of the open cluster NGC 3114. V0425 Car |OH, SiO maser. V0426 Car |VB (A 10.5m; B 13m, 9", 198{deg}, 2000; C 13m, 8", 264{deg}, 2000; V0426 Car |D 14m, 5", 238{deg}, 2000); combined brightness in the Table. SB1, V0426 Car |P = 43.5d. V0428 Car |VB A (B 13", 276{deg}, 2000, Comp. A VB, 0.6", 135{deg}, 1991). V0429 Car |In a nebula. V0432 Car |In a ring nebula. V0433 Car |Multiperiodic. V0434 Car |OH, SiO maser. V0436 Car |Porb = 0.1497d. V0438 Car |In the region of the open cluster NGC 3293. V0439 Car |In the region of the open cluster NGC 3293. V0440 Car |In the region of the open cluster NGC 3293. V0441 Car |In the region of the open cluster NGC 3293. V0442 Car |In the region of the open cluster NGC 3496. Crowded. V0450 Car |VB A (B 6.8m, 1.4", 86{deg}, 1997); one of the components is SB, V0450 Car |Porb = 340d. V0460 Car |In the region of the open cluster NGC 2516. V0466 Car |Apsidal motion. MinII = 2448036.284 + 3.455887d x E. V0467 Car |MinII - MinI = 0.62P. V0470 Car |VB Aab (7.61mHp, 9.79mHp, 0.1", 42{deg}, 2015). V0486 Car |O'Connell effect. V0487 Car |The mean brightness varies with a cycle about 780d. V0491 Car |The mean Hipparcos magnitude is 9.69mHp. Const at 8.93mV? [00001]. V0493 Car |Apsidal motion. MinII = 2447947.768 + 3.22937 x E. V0498 Car |Type BE: is also possible. V0499 Car |Possible periods: 0.081566d, 4.98753d. V0513 Car |In the region of the open cluster NGC 3293. V0514 Car |Porb is given in the Table. Pulsations: P = 4.655d. V0519 Car |In the region of the open cluster Cr 228. In a nebula. V0523 Car |P = 0.9155d is also possible. V0526 Car |VB A (B 10.6m, 23", 153{deg}, 2000). V0527 Car |VB AB (9.15m, 11.83m, 1", 230{deg}, 1991). V0529 Car |Apsidal motion. MinII = 2448159.970 + 4.74449d x E. V0530 Car |VB A (B 14.0m, 1.4", 355{deg}, 1944; C 14.2m, 4", 169{deg}, 1944; D V0530 Car |12.3m, 19", 176{deg}, 2000). V0531 Car |VB A (B 13.0m, 16", 189{deg}, 1998). V0533 Car |In the region of the open cluster NGC 3572a. V0534 Car |Flare-like activity. V0542 Car |In the region of the open cluster IC 2602. V0543 Car |In the region of the open cluster IC 2602. V0544 Car |In the region of the open cluster IC 2602. V0545 Car |In the region of the open cluster IC 2602. V0546 Car |In the region of the open cluster IC 2602. V0547 Car |In the region of the open cluster IC 2602. V0548 Car |In the region of the open cluster IC 2602. V0549 Car |In the region of the open cluster IC 2602. V0550 Car |In the region of the open cluster IC 2602. V0551 Car |In the region of the open cluster IC 2602. V0552 Car |In the region of the open cluster IC 2602. V0553 Car |In the region of the open cluster IC 2602. V0554 Car |In the region of the open cluster IC 2602. V0555 Car |In the region of the open cluster IC 2602. V0556 Car |In the region of the open cluster IC 2602. V0557 Car |In the region of the open cluster IC 2602. V0558 Car |In the region of the open cluster IC 2602. V0559 Car |In the region of the open cluster IC 2602. V0560 Car |Apsidal motion. V0561 Car |In the region of the open cluster IC 2602. V0562 Car |In the region of the open cluster IC 2602. V0563 Car |In the region of the open cluster IC 2602. V0564 Car |In the region of the open cluster IC 2602. V0565 Car |In the region of the open cluster IC 2602. V0566 Car |In the region of the open cluster IC 2602. V0567 Car |In the region of the open cluster IC 2602. V0568 Car |In the region of the open cluster IC 2602. V0569 Car |In the region of the open cluster IC 2602. V0570 Car |In the region of the open cluster IC 2602. V0571 Car |In the region of the open cluster IC 2602. V0572 Car |In the region of the open cluster Tr 16 and Eta Car nebula. V0572 Car |Eclipses are in the O7V+O9.5V pair; for the B0.2IV star, Porb = V0572 Car |285.1d or 1340.5d is possible [77090]. V0573 Car |In the region of the open cluster Trumpler 16. V0574 Car |VB A (B 4"p). Almost monotonic brightening for 12 years. V0583 Car |VB A (B 15m, 14", 286{deg}, 2000). V0601 Car |A cycle of about 70d is sometimes superposed. V0606 Car |MinII - MinI = 0.583P. V0607 Car |In the region of the open cluster NGC 2516. V0610 Car |MinII - MinI = 0.26P. V0613 Car |VB A (companion B of comparable brightness, 16", 0{deg}, 2000). The V0613 Car |magnitudes in the Table were inflienced by the companion. V0621 Car |VB A (B 14.6m, 12", 347{deg}; C 15.2m, 5", 27{deg}, 2000). V0627 Car |VB A (B 13.5mpg, 22", 18{deg}, 1998). V0638 Car |VB A (B 15.1mpg, 6", 27{deg}, 2000). V0645 Car |VB A (B 11.6m, 15", 54{deg}, 2000). V0652 Car |VB A (B 13.2m, 10", 55{deg}, 1997; other companions). V0653 Car |VB A (B 14.4m, 10", 285{deg}, 2000). V0654 Car |In the region of the open cluster Cr 223. V0655 Car |MinII - MinI = 0.38P. V0656 Car |Blended. V0660 Car |In the Eta Carinae nebula. VB A (B 10.8m, 21", 206{deg}, 1998), the V0660 Car |tabulated magnitude at maximum can be influenced. V0661 Car |MinII - MinI = 0.65P. In the Eta Carinae nebula. VB A (B 12.5m, V0661 Car |12", 158{deg}, 2000). V0662 Car |In the Eta Carinae nebula. In the region of the open cluster NGC V0662 Car |3372. V0674 Car |MinII - MinI = 0.29P. Multiple (faint companions). V0675 Car |VB A (B 12.2mR, 6", 20{deg}, 1996). The magnitudes in the Table are V0675 Car |for combined brightness. V0680 Car |VB B (A 7.74m, A0V; AB 17", 238{deg}, 1998). V0681 Car |The Table presents light elements for eclipses. Pulsations: P = V0681 Car |0.214292d, amplitude about 0.03m. V0684 Car |VB AB (A 9.03m; B 10.70m, 4", 188{deg}, 1941). V0701 Car |P0 is tabulated, P1 = 2.869. VB AB (11.44m, 11.66m, 0.9", 1991). V0706 Car |The mean brightness varies with a cycle about 1900d. V0712 Car |In the region of the open cluster Westerlund 2. V0714 Car |In the region of the open cluster IC 2581. V0717 Car |Besides variations with the tabulated period, a second EB V0717 Car |periodicity is revealed, P2 = 1.110270d, with amplitudes 0.20m V0717 Car |(primary) and 0.15m (secondary). V0718 Car |Besides variations with the tabulated period, a second EW V0718 Car |periodicity is revealed, P2 = 0.388607d, with amplitudes of both V0718 Car |minima about 0.1m. V0720 Car |VB B (A 10.15m; B 16", 53{deg}, 1991). V0721 Car |In the Eta Carinae nebula. V0722 Car |In the Eta Carinae nebula. V0723 Car |In the region of the open cluster Tr 14. In the Eta Carinae nebula. V0724 Car |VB A (B 13.2m, 4", 80{deg}, 1934). V0725 Car |MinII - MinI = 0.15P. In the Eta Carinae nebula. V0726 Car |In the Eta Carinae nebula. V0727 Car |VB B (A 10.4m; AB 12", 51{deg}, 2000). V0728 Car |In the Eta Carinae nebula. V0729 Car |In the Eta Carinae nebula. V0730 Car |In the Eta Carinae nebula. V0731 Car |In the Eta Carinae nebula. In the region of the open cluster Tr 16. V0731 Car |VB A (B 9.61m, 27", 2{deg}, 1991; C 9.64m, 15", 195{deg}, 1991). V0734 Car |MinII - MinI = 0.44P. V0742 Car |VB A (B 1"p). V0750 Car |SB3. V0754 Car |SB3. V0777 Car |VB A (B 5"sp). V0786 Car |Outside eclipses, sinusoidal variations, full amplitude 0.0035m, P V0786 Car |about 0.23d [80369]. V0788 Car |SB2, a triple system. V0790 Car |SB2, a triple system. V0802 Car |Mean brightness varies. VB A (B 11.7m, 5", 222{deg}, 2000). V0821 Car |SB3. V0829 Car |In the open cluster Cr 240. V0831 Car |Possibly also an intrinsic variable. V0835 Car |SB2. SB2. V0845 Car |SB2. SB2. V0846 Car |Multiperiodic, 3 harmonics. Multiperiodic, 3 harmonics. V0865 Car |MinII - MinI = 0.605P. MinII - MinI = 0.605P. V0867 Car |VB B (A 12.6mV; AB 4.5", 194{deg}, 2000). VB B (A 12.6mV; AB 4.5", V0867 Car |194{deg}, 2000). V0869 Car |MinII - MinI = 0.45P. MinII - MinI = 0.45P. V0887 Car |MinII - MinI = 0.445P. MinII - MinI = 0.445P. V0889 Car |MinII - MinI = 0.370P. MinII - MinI = 0.370P. V0890 Car |A twice shorter period is also possible. A twice shorter period is V0890 Car |also possible. V0899 Car |Double-mode pulsations. The Table gives the fundamental-mode V0899 Car |elements. For the first overtone, P1 = 0.0858512d. P1/P0 = 0.7748. V0899 Car |Double-mode pulsations. The Table gives the fundamental-mode V0899 Car |elements. For the first overtone, P1 = 0.0858512d. P1/P0 = 0.7748. V0901 Car |Large scatter outside eclipses; intrinsic variability? Large V0901 Car |scatter outside eclipses; intrinsic variability? V0911 Car |Epoch of minimum brightness is given in the Table. Secondary V0911 Car |minimum at about 11.4m. P = 44.9d is superposed. V0914 Car |MinII - MinI = 0.90P. V0924 Car |Blended. Blazhko effect. V0944 Car |Cluster non-member. eta Car |In the HII region NGC 3372, in the region of the open cluster Tr eta Car |16. Multiple from speckle interferometry. Maximum brightness was eta Car |observed in 1843. The bipolar Homunculus nebula was formed in the eta Car |1843 event. Several periodicities were reported by different eta Car |authors. R Cas |VB A (B 14.5m, 14", 273{deg}). SiO, OH maser; OH, H2O, SiO maser. R Cas |VB A (B 13.2m, 22", 265{deg}, 2011; C 11.0m, 31", 318{deg}, 2011). S Cas |SiO maser. T Cas |SiO maser. Double maxima are often observed. U Cas |S4.5/4e. V Cas |SiO maser. X Cas |P varies. Y Cas |OH, H2O, SiO maser. Z Cas |SiO maser. RV Cas |SiO maser. RW Cas |P varies. RX Cas |P varies, quadratic term +1.151d x 10^{-5} x E^2. The magnitude at RX Cas |MinII varies between 9.12m and 9.49m. RZ Cas |Irregular period variations, the Table presents current elements. RZ Cas |The light curve shape varies. SU Cas |Probable member of the open cluster Alessi 95. SB? SV Cas |Biperiodic, P2 = 460d. SX Cas |d = 0.04P. P varies, the Table presents current light elements. SX Cas |Light curve shape varies. VB A (B 12.1m, 20", 249{deg}, 2015). SY Cas |P varies, the Table presents current light elements. SZ Cas |P varies, quadratic term +1.01d x 10^(-5) x E^2. TU Cas |The Table presents the period of the fundamental mode. First TU Cas |overtone: P1 = 1.51833. TV Cas |P varies, the Table presents current light elements. Light curve TV Cas |shape varies. TW Cas |P varies, the Table presents current light elements. TY Cas |H2O maser. P varies. P = 545.0d was reported for JD 2419200 - TY Cas |2425000. UV Cas |According to [N0230], pulsations with P = 40.2d at maximum with an UV Cas |amplitude of 0.04m. VV Cas |P varies. The light elements in the Table are valid after JD VV Cas |2432500. WY Cas |In the region of the open cluster NGC 7789. WZ Cas |Biperiodic, second period 187d. ZZ Cas |P varies, the Table presents mean light elements. AB Cas |The light elements in the Table are for eclipses. Pulsations: P = AB Cas |0.05828649d [N0415], amplitude 0.04mV, associated with the primary. AE Cas |P varies, the Table presents current light elements. AH Cas |P varies, the Table presents current light elements. AL Cas |P varies? The Table presents current light elements. AM Cas |Porb = 0.1649: days. AO Cas |The shape of the light curve varies? AR Cas |VB A (B 9.3m, 0.8", 356{deg}, 2002; other distant components). AR Cas |MinII = 2435796.6429 + 6.0662969d x E. The period of the AR Cas |apsidalmotion is about 1100 years. AS Cas |VB A (B 15.2m, 9", 57{deg}, 2000). The light elements in the Table AS Cas |are for the fundamental mode (amplitude 0.59m). First overtone: Max AS Cas |= 2448510.5 + 2.155557d x E, amplitude 0.13m. AX Cas |P varies, the Table presents current light elements. AZ Cas |D = 110d, d = 88d = 0.026P. BD Cas |P varies, the Table presents current light elements. Type DCEPS is BD Cas |not excluded. BE Cas |VB A (B Sp G, 14.8m, 19", 264{deg}, 2000). BH Cas |VB A (B 13.5m, 10", 209{deg}, 2000). P varies, the Table presents BH Cas |current light elements. BM Cas |Variations outside eclipses with an amplitude from 0.1m to 0.2m at BM Cas |time scales of 20d, 80-90d [N0421]. BS Cas |P varies, the Table presents current light elements. BT Cas |SiO maser. BY Cas |In the region of the open cluster NGC 663. P varies, the Table BY Cas |presents current light elements. Quadratic light elements: Max = BY Cas |2431933.033 + 3.221494d x E + 2.251d x 10(^-7) x E^2 [N0256]. SB. BZ Cas |P varies, the Table presents current light elements. CE CasA |In the open cluster NGC 7790. VB A (B = CE Cas B, 2.4", 265{deg}, CE CasA |2002). CE CasB |In the open cluster NGC 7790. VB B (A = CE Cas A; AB 2.4", CE CasB |265{deg}, 2002). CF Cas |In the open cluster NGC 7790. CG Cas |In the region of the open clusters Be 58 and NGC 7790. CQ Cas |The slow variations are superposed with smaller-amplitude waves, CQ Cas |110d to 250d long. CR Cas |P varies, the Table presents provisional current light elements. CR Cas |Contradictory spectral type information. CW Cas |P varies (decreases systematically), the Table presents current CW Cas |light elements. Depths of minima vary. DD Cas |P varies? The Table presents current light elements. DF Cas |In the region of the open cluster NGC 1027. DI Cas |VB A (B 16.0mpg, 7", 190{deg}, 1995). DK Cas |Close companions. DL Cas |Member of the open cluster NGC 129. SB, Porb = 684.4d. DQ Cas |In the region of the emission nebula NGC 7635. DR Cas |In the region of the emission nebula NGC 7635. DS Cas |In the region of the emission nebula NGC 7635. DZ Cas |P varies, the Table presents current light elements. EG Cas |P varies, the Table presents current light elements. EI Cas |P varies? The Table presents current light elements. EM Cas |P varies. Amplitude varies strongly. EP Cas |P varies? The Table presents current light elements. EU Cas |SiO maser. EY Cas |P varies, the Table presents current light elements. FN Cas |VB A (B 16.1m, 7", 51{deg}, 1990). FO Cas |VB A (B 14.7m, 16", 304{deg}, 1992; other companions). FV Cas |P varies, the Table presents current light elements. GG Cas |P varies, the Table presents current light elements. GH Cas |P varies, the Table presents current light elements. GT Cas |d = 0.02P. P varies, the Table presents current light elements. GX Cas |Superoutbursts: the cycle is about 386d. Porb = 0.08902d. HN Cas |d = 0.038P. HS Cas |Several close companions. HT Cas |The light elements in the Table are for EA eclipses. 16.0 - 16.5mV HT Cas |in quiescence outside eclipses. Rare superoutbursts and normal HT Cas |outbursts during recent years. HU Cas |P varies. VB A (B 16.1mpg, 7", 273{deg}, 1999). HY Cas |P = 12.07d/n. IR Cas |P varies, the Table presents current light elements. IS Cas |P varies, the Table presents current light elements. IT Cas |MinII - MinI = 0.553P. Possible apsidal motion cycle: 404 years. IT Cas |DSCTC pulsations of the secondary were suspected [N0426]. IV Cas |P varies, the Table presents current light elements. Probable third IV Cas |body, P = 60 years [N0427]. Pulsations of the primary: P = IV Cas |0.026545d, {Delta} m = 0.01mB [N0428]. IX Cas |P varies. SB, Porb = 110.29d. KO Cas |VB A (B 13.6m, 24", 314{deg}, 1998). KX Cas |VB C (A 13.0m, B 13.1m; AC 14", 76{deg}, 1998; BC 12", 264{deg}, KX Cas |1998). KY Cas |VB A (A 15.8mV; B 15.9mV, 8", 245{deg}, 1998). KZ Cas |VB A (B 18.1m, 7", 26{deg}, 1998). LQ Cas |P varies? The Table presents current light elements. LW Cas |In the nebulosity associated with the open cluster IC 1848. Single LW Cas |strong brightening in 1951 - 1952. LX Cas |In the region of the open cluster Collinder 33. MinII - MinI = LX Cas |0.47P. dI = 0.10P. LY Cas |In the region of the open cluster Collinder 33. d = 0.03P. MM Cas |P varies, the Table presents current light elements. Variations of MM Cas |the primary reported in [N0432], with a combined-brightness MM Cas |amplitude of 0.08m and P = 0.15d. MO Cas |In the region of the nebula NGC 7635. 10.2 - 13.1mI. MP Cas |In the region of the nebula NGC 7635. 10.4 - 13.5mI. MR Cas |P varies? MT Cas |d = 0.04P. P varies? The Table presents current light elements. MU Cas |MinII - MinI = 0.37P. MW Cas |VB A (B 8", 75{deg}, 2000). The magnitude range in the Table is for MW Cas |combined brightness. MY Cas |P varies? The Table presents current light elements. NN Cas |VB A (B 9", 29{deg}, 2000; C 6", 238{deg}, 2000). NT Cas |P varies? NV Cas |d = 0.03P. NX Cas |In an HII region. OX Cas |In the region of the open cluster NGC 381. The Table presents mean OX Cas |light elements. Apsidal motion, P = 39.8 years [N0434]. PV Cas |P varies, the Table presents current light elements. Apsidal PV Cas |motion, P = 92.9 years. PZ Cas |VB A (B 12.8m, 12", 99{deg}, 2011). Biperiodic, P2 = 3195d. QQ Cas |P varies, the Table presents current light elements. QX Cas |In the region of the open cluster NGC 7790. VB A (B 13.1m, 3"). QX Cas |MinII - MinI = 0.38P. QY Cas |[Fe/H] = -1.30. V0341 Cas |P varies, the elements in the Table are valid prior to JD 2440443. V0346 Cas |VB A (12.7mV; B 13.9mV, 15", 22{deg}, 1990). V0348 Cas |VB A (B 16.8m, 7", 65{deg}, 2000). V0350 Cas |P varies, the Table presents current light elements. V0355 Cas |P varies, the Table presents current light elements. V0359 Cas |P varies, the Table presents current light elements. V0363 Cas |P1 = 0.438243d. V0365 Cas |P varies, the period in the Table is for JD 2430000 - 2440000. V0366 Cas |P varies, the Table presents current light elements. V0368 Cas |P varies? The Table presents current light elements. V0373 Cas |MinII - MinI = 0.58P. Peculiar light curve. Suspected apsidal V0373 Cas |motion. V0375 Cas |P varies, the Table presents current light elements. V0377 Cas |VB AB (8.11mV, 8.48mV, 2", 182{deg}, 1991). V0381 Cas |Apsidal motion? The Table presents current light elements for MinI. V0384 Cas |P varies? The Table presents current light elements. V0385 Cas |P varies, the Table presents current light elements. V0387 Cas |P varies, the Table presents current light elements. V0388 Cas |Wolf 47. {mu} = 0.727" per year, p = 82.5{deg}. A V0388 Cas |common-proper-motion pair with BD +61{deg} 195 = Wolf 46 at an V0388 Cas |angular distance of 294". V0389 Cas |P varies, the Table presents current light elements. V0392 Cas |P varies? V0398 Cas |In the region of the emission nebula NGC 7635. V0404 Cas |[Fe/H] = -1.6:. V0411 Cas |P varies? V0412 Cas |VB A (B 15", 259{deg}, 2000). V0424 Cas |P = 3.09d/N. V0425 Cas |SB1, Porb = 0.14964d. V0430 Cas |VB A (B 17.7m, 6", 188{deg}, 1995). V0442 Cas |P varies, the Table presents current light elements. V0444 Cas |P varies, the Table presents mean light elements. V0445 Cas |P varies? The Table presents current light elements. V0450 Cas |VB A (B 17.5:m, 3", 189{deg}, 1999). The range in the Table is for V0450 Cas |combined light. V0452 Cas |VB A (B 15.8m, 7", 160{deg}, 1998). V0466 Cas |In the region of the open cluster NGC 457. V0470 Cas |P varies, the Table presents light elements for JD 2436200 - V0470 Cas |2450013. V0471 Cas |P varies? The Table presents current light elements. V0473 Cas |P varies, the Table presents current light elements. V0480 Cas |Red. LB: [00001]. V0482 Cas |P = 0.28292d is also possible [05522]. No reliable periodic V0482 Cas |variations were detected in [00075]. VB Aab (7.8mV, 10.5mV, 0.4", V0482 Cas |90{deg}, 2008; B 9.9mV, 7", 190{deg}, 2015; C 10.5mV, 53", 9{deg}, V0482 Cas |2008; D 1 V0487 Cas |P2 = 99.6d. V0494 Cas |The chart in [05849] is believed to be distorted. V0495 Cas |VB (3"). V0497 Cas |In the region of the open cluster IC 1848. V0498 Cas |In the region of the open cluster IC 1848. V0499 Cas |In the region of the open cluster IC 1848. V0509 Cas |P2 = 299.2d; possibly P3 = 385.4d. Other authors report different V0509 Cas |periods. V0518 Cas |In the region of the open cluster Stock 2. V0520 Cas |P varies, the Table presents current mean light elements. V0521 Cas |In the open cluster NGC 7789. V0523 Cas |P varies, the Table presents current light elements. V0524 Cas |OH, H2O, SiO maser. V0526 Cas |Multiperiodic; also P = 0.0526d. V0528 Cas |VB A (B 10.9mV, 15", 104{deg}, 2011). V0530 Cas |In the region of the emission nebula NGC 7635. V0532 Cas |VB B (A 9.8m; AB 24", 237{deg}, 2006). In the open cluster NGC V0532 Cas |7789. V0533 Cas |In the region of the open cluster NGC 7789. V0536 Cas |P varies, the Table presents light elements for JD 2441533 - V0536 Cas |2442016. V0542 Cas |In the region of the open cluster NGC 7789. V0544 Cas |P varies, the Table presents current light elements. V0546 Cas |In the region of the open cluster NGC 103. V0547 Cas |VB A (Aa, Ab 0.4", 222{deg}, 2014; B 12.2mV, 4", 182{deg}, 2013). V0547 Cas |The range in the Table is for combined magnitudes. V0559 Cas |VB AB (7.5m, 8.2m, 0.4", 71 {deg}, 2007). The range in the Table is V0559 Cas |for combined brightness. V0563 Cas |In the region of the nebula NGC 7635. V0566 Cas |VB (5.70m, 8.07m, 1.5", 194{deg}, 2015). The range in the Table is V0566 Cas |for combined brightness. V0568 Cas |Possible Blazhko effect. V0569 Cas |In the region of the nebula NGC 7635. V0570 Cas |In the region of the nebula NGC 7635. V0571 Cas |In the region of the nebula NGC 7635. V0572 Cas |In the region of the nebula NGC 7635. V0573 Cas |In the region of the nebula NGC 7635. V0574 Cas |In the region of the nebula NGC 7635. V0575 Cas |In the region of the nebula NGC 7635. V0576 Cas |In the region of the nebula NGC 7635. V0577 Cas |In the region of the nebula NGC 7635. V0578 Cas |In the region of the nebula NGC 7635. V0579 Cas |In the region of the nebula NGC 7635. V0580 Cas |In the region of the nebula NGC 7635. V0581 Cas |In the region of the nebula NGC 7635. V0582 Cas |In the region of the nebula NGC 7635. V0583 Cas |In the region of the nebula NGC 7635. V0584 Cas |In the region of the nebula NGC 7635. V0585 Cas |In the region of the nebula NGC 7635. V0586 Cas |In the region of the nebula NGC 7635. V0587 Cas |In the region of the nebula NGC 7635. V0589 Cas |In the region of the open cluster NGC 663. V0592 Cas |Porb = 0.112d. Variations with P = 0.0150d were reported in V0592 Cas |[N0451]. V0594 Cas |In the region of the open cluster NGC 225. V0597 Cas |Not red. V0600 Cas |Not red. V0601 Cas |Not red. V0603 Cas |Not red. V0604 Cas |Not red. V0606 Cas |Not red. V0608 Cas |P varies, the Table presents current light elements. V0612 Cas |Not red enough for its variability type and spectral type. V0614 Cas |Not red enough for its variability type and spectral type. V0615 Cas |VB A (B 13.4m, 12", 166{deg}, 2003). Optical variations with the V0615 Cas |orbital period, radio outbursts with the same period. P2 about V0615 Cas |1670d was reported. V0627 Cas |H2O, SiO, OH maser. V0628 Cas |Several close companions reported. In a nebula with a complex V0628 Cas |structure. V0629 Cas |In the open cluster Stock 12. V0630 Cas |Very rare outbursts (1950, 1992, 2009). Porb = 2.56387d. V0633 Cas |H2O maser. V0635 Cas |Porb = 24.3d, Prot = 3.6s. V0638 Cas |VB Aa (Ab 10.52m, 0.6", 137{deg}, 2009; B 10.15m, 19", 48{deg}, V0638 Cas |2007). V0639 Cas |VB A (6.52m; B 8.32m, 0.2", 34{deg}, 1998). The range in the Table V0639 Cas |is for combined brightness. V0640 Cas |VB (A 6.34mV; B 7.99mV, 1.4". 357{deg}, 2015; Porb = 106.8 years). V0640 Cas |B SB, P = 47.685d. V0643 Cas |Seems too white for a Cepheid [00001]. V0644 Cas |Seems too white for a Cepheid [00001]. V0645 Cas |In the region of the open cluster NGC 457. V0650 Cas |VB AB (6.76mV, 7.76mV, 0.7", 319{deg}, 2011). V0656 Cas |OH, SiO maser. V0657 Cas |H2O, SiO maser. V0662 Cas |Porb = 11.59d, e = 0.16. X-ray flaring activity. V0663 Cas |Multiperiodic. V0664 Cas |The central star of the planetary nebula HFG1. V0665 Cas |Optical pulsations at 285.6 MHz were reported. A 7-second X-ray V0665 Cas |pulsar. The star remains a doubtful variable with no reliable V0665 Cas |optical identification. V0669 Cas |H2O, SiO, OH maser. V0702 Cas |P varies, the Table presents current light elements. V0709 Cas |Pspin = 312.77s, Pbeat = 317.94s. V0710 Cas |A double IR source (6") in a nebula within a dark cloud. H2O maser. V0711 Cas |In the region of the galaxy NGC 185; a foreground object? V0712 Cas |In the region of the galaxy NGC 185; a foreground object? V0713 Cas |In the region of the galaxy NGC 185; a foreground object? V0714 Cas |In the region of the galaxy NGC 185; a foreground object? V0715 Cas |In the region of the galaxy NGC 185; a foreground object? V0716 Cas |In the region of the galaxy NGC 185; a foreground object? V0717 Cas |In the region of the galaxy NGC 185; a foreground object? V0718 Cas |In the region of the galaxy NGC 185; a foreground object? V0719 Cas |In the region of the galaxy NGC 185; a foreground object? V0723 Cas |Long-term variations: Max = 2450136 + 182d x E. Short-term V0723 Cas |variations (eclipses?): Min = 2450421.4405 + 0.63501d x E. V0730 Cas |In the region of the open cluster NGC 7789. V0731 Cas |In the region of the open cluster NGC 7789. V0732 Cas |In the region of the open cluster NGC 7789. V0733 Cas |In the region of the open cluster NGC 7789. V0734 Cas |In the region of the open cluster NGC 7789. V0735 Cas |In the region of the open cluster NGC 7789. V0736 Cas |In the region of the open cluster NGC 7789. V0737 Cas |In the region of the open cluster NGC 7789. O'Connell effect. V0738 Cas |In the region of the open cluster NGC 7789. VB A (B 2" sf). V0742 Cas |SB, Porb = 55.9233d. V0745 Cas |VB A (B 11.13m, 9.5", 85{deg}, 2012). V0746 Cas |VB AB (5.95m, 6.84m, 0.1", 94{deg}, 2007). Multiperiodic; P2 V0746 Cas |=1.06502d, P3 = 0.83094d. SB, P = 25.44d. V0747 Cas |VB AB (7.67m, 7.87m, 0.15", 35{deg}, 1991). The variability may be V0747 Cas |due to the fainter component. V0756 Cas |VB AB (9.21m, 10.02m, 0.3", 159{deg}, 2008). V0761 Cas |VB AB (6.50m, 8.97m, 1.5", 262{deg}, 2007). V0765 Cas |In the region of the open cluster NGC 457. V0766 Cas |VB AB (7.30m, 9.18m, 0.4", 90{deg}, 1998). V0773 Cas |VB AB (6.36m, 6.60m, 0.6", 332{deg}, 2010). V0775 Cas |MinII - MinI = 0.65P. V0776 Cas |VB AB (9.08m, 10.64m, 5", 136{deg}, 2011). V0779 Cas |VB AB (6.78m, 8.74m, 1.1", 9{deg}, 2007). V0784 Cas |Multiperiodic. V0791 Cas |VB AB (7.85m, 11.09m, 3", 140{deg}, 1991). V0798 Cas |SB. V0799 Cas |MinII - MinI = 0.68P. V0816 Cas |VB AB (6.6mV, 10.8mV, 3", 277{deg}, 2009). V0821 Cas |Apsidal motion. MinII = 2447965.031 + 1.769720d x E. V0823 Cas |A triple-mode pulsating variable star. Resembles AC And. First V0823 Cas |overtone: see Table. Fundamental mode: P0 = 0.669001d. Second V0823 Cas |overtone: P = 0.410916d. Periods vary. V0825 Cas |The Table presents light elements for the fundamental mode. First V0825 Cas |overtone: Max = 2444825.50 + 2.65262d x E. V0827 Cas |P varies. V0831 Cas |Pulses with P about 8.7s in X-rays and in the optical range V0831 Cas |[N0471]. V0839 Cas |In the open cluster NGC 7654. P = 0.816d is also possible. V0840 Cas |In the open cluster NGC 7654. V0841 Cas |In the open cluster NGC 7654. V0842 Cas |In the open cluster NGC 7654. V0843 Cas |In the open cluster NGC 7654. V0849 Cas |Between JD 2429100 and JD 2447087, brightness oscillated around V0849 Cas |ever increasing mean level. V0861 Cas |SiO maser. V0865 Cas |SiO maser. V0868 Cas |In the open cluster NGC 663. V0869 Cas |In the open cluster NGC 663. V0874 Cas |In the open cluster NGC 7789. V0875 Cas |In the open cluster NGC 7789. V0876 Cas |In the open cluster NGC 7789. V0877 Cas |In the open cluster NGC 7789. V0898 Cas |Several companions. V0923 Cas |VB A (B 6", 353{deg}, 1999). V0934 Cas |VB A (B 14.7m, 14", 334{deg}, 1992). V0947 Cas |SiO maser. V0969 Cas |In the open cluster NGC 654. MinII - MinI = 0.547P. V0971 Cas |In the open cluster NGC 654. V0972 Cas |In the open cluster NGC 663. V0973 Cas |In the open cluster NGC 663. V0974 Cas |In the open cluster NGC 663. V0975 Cas |In the open cluster NGC 663. V0976 Cas |In the open cluster NGC 663. V0977 Cas |VB A (B 10.98m, 7", 38{deg}, 2015). In the open cluster NGC 663. V0978 Cas |VB B (A 9.04m; AB 9", 106{deg}, 2015). In the open cluster NGC 663. V0979 Cas |In the open cluster NGC 663. V0980 Cas |In the open cluster NGC 663. V0981 Cas |In the open cluster NGC 663. V0982 Cas |In the open cluster NGC 663. V0983 Cas |In the open cluster NGC 663. V0984 Cas |In the open cluster NGC 663. V0985 Cas |VB B (A 9.36m; AB 8", 69{deg}, 2015). In the open cluster NGC 663. V0986 Cas |In the open cluster NGC 663. V0987 Cas |VB A (B 10.7m, 10", 329{deg}, 2000). V0988 Cas |VB AB (8.13mV, 10.7mV, 5", 181{deg}, 2003). V0990 Cas |Chromospherically active giant, photometric variations with the V0990 Cas |rotational period. V1006 Cas |Multiperiodic. V1012 Cas |Multiperiodic. VB AB (7.42mV, 9.72mV, 0.1", 76{deg}, 2010). V1018 Cas |VB AB (10.4mV, 11.6mV, 2", 198{deg}, 2001). MinII - MinI = 0.41P. V1022 Cas |MinII - MinI = 0.67:P. V1023 Cas |In the region of the open cluster NGC 7789. V1024 Cas |In the region of the open cluster NGC 7789. V1026 Cas |Multiperiodic. V1027 Cas |Intermediate polar. Porb = 0.16804d. V1036 Cas |VB AB (10.2mV, 10.1mV, 0.4", 91{deg}, 2009). V1037 Cas |Millisecond pulsar (Pspin = 1.7ms). Porb = 0.1024d. Several V1037 Cas |large-amplitude brightenings were observed. V1038 Cas |VB AB (10.7mV, 11.2mV, 0.7", 314{deg}, 1991). V1054 Cas |The tabulated variability range is distorted with GSC 03667-01557. V1066 Cas |MinII - MinI = 0.56P. V1073 Cas |In the region of the open cluster NGC 457, outside its tidal V1073 Cas |radius. V1074 Cas |In the region of the open cluster NGC 457, outside its tidal V1074 Cas |radius. V1075 Cas |In the region of the open cluster NGC 457, outside its tidal V1075 Cas |radius. V1076 Cas |In the region of the open cluster NGC 457, outside its tidal V1076 Cas |radius. V1077 Cas |In the region of the open cluster NGC 457, outside its tidal V1077 Cas |radius. V1078 Cas |In the region of the open cluster NGC 457. V1079 Cas |In the region of the open cluster NGC 457, outside its tidal V1079 Cas |radius. V1080 Cas |In the region of the open cluster NGC 457, outside its tidal V1080 Cas |radius. V1081 Cas |In the region of the open cluster NGC 457, outside its tidal V1081 Cas |radius. V1082 Cas |In the region of the open cluster NGC 457, cluster non-member. V1083 Cas |In the region of the open cluster NGC 457, outside its tidal V1083 Cas |radius. V1084 Cas |In the region of the open cluster NGC 457. V1085 Cas |In the region of the open cluster NGC 457, cluster non-member. V1086 Cas |In the region of the open cluster NGC 457. V1087 Cas |In the region of the open cluster NGC 457, cluster non-member. V1088 Cas |In the region of the open cluster NGC 457, outside its tidal V1088 Cas |radius. V1090 Cas |In the region of the open cluster NGC 457, cluster non-member. V1092 Cas |In the region of the open cluster NGC 457, outside its tidal V1092 Cas |radius. V1093 Cas |In the region of the open cluster NGC 457, cluster non-member. V1095 Cas |In the region of the open cluster NGC 457, outside its tidal V1095 Cas |radius. V1096 Cas |In the region of the open cluster NGC 457, outside its tidal V1096 Cas |radius. V1097 Cas |In the region of the open cluster NGC 457, outside its tidal V1097 Cas |radius. V1098 Cas |In the region of the open cluster NGC 457. V1099 Cas |In the region of the open cluster NGC 457, outside its tidal V1099 Cas |radius. V1101 Cas |In the region of the open cluster NGC 457, outside its tidal V1101 Cas |radius. V1102 Cas |In the region of the open cluster NGC 457, outside its tidal V1102 Cas |radius. V1103 Cas |MinII - MinI = 0.531P. V1104 Cas |In the region of the open cluster NGC 457, outside its tidal V1104 Cas |radius. V1105 Cas |In the region of the open cluster NGC 457, outside its tidal V1105 Cas |radius. V1107 Cas |P varies, the Table presents current light elements. V1110 Cas |MinII - MinI = 0.710P. V1111 Cas |In the open cluster M 103 = NGC 581. V1112 Cas |A twice longer period with minima of the same depth is possible. V1113 Cas |In the open cluster M 103 = NGC 581. V1114 Cas |In the open cluster M 103 = NGC 581. V1115 Cas |P varies, the Table presents current light elements. V1117 Cas |In the open cluster M 103 = NGC 581. V1118 Cas |In the open cluster M 103 = NGC 581. V1119 Cas |In the open cluster M 103 = NGC 581. V1120 Cas |In the open cluster M 103 = NGC 581. V1121 Cas |In the open cluster M 103 = NGC 581. V1122 Cas |VB B (A = NSV 00542, 7.3m; B 14", 143{deg}, 2007; 3 more V1122 Cas |components). In the open cluster M 103 = NGC 581. V1123 Cas |In the open cluster M 103 = NGC 581. MinII - MinI = 0.73P. P = V1123 Cas |6.006d is also possible. V1124 Cas |In the open cluster M 103 = NGC 581. V1125 Cas |In the open cluster M 103 = NGC 581. V1126 Cas |In the open cluster M 103 = NGC 581. V1127 Cas |In the open cluster M 103 = NGC 581. V1129 Cas |In the open cluster M 103 = NGC 581. V1130 Cas |In the open cluster M 103 = NGC 581. V1132 Cas |In the open cluster M 103 = NGC 581. Multiperiodic. V1133 Cas |In the open cluster M 103 = NGC 581. V1134 Cas |In the open cluster M 103 = NGC 581. V1135 Cas |In the open cluster M 103 = NGC 581. V1136 Cas |In the open cluster M 103 = NGC 581. V1137 Cas |Probable apsidal motion. V1139 Cas |P varies, the Table presents current light elements. Third body? V1141 Cas |MinII - MinI = 0.441P. V1142 Cas |In the open cluster NGC 637. V1143 Cas |In the open cluster NGC 637. Multiperiodic. V1144 Cas |In the open cluster NGC 659. V1145 Cas |In the open cluster NGC 659. V1146 Cas |In the open cluster NGC 659. V1147 Cas |In the field of the open cluster NGC 659. V1148 Cas |In the open cluster NGC 659. V1149 Cas |In the field of the open cluster NGC 659. V1150 Cas |In the open cluster NGC 659. V1151 Cas |In the field of the open cluster NGC 663. V1152 Cas |In the field of the open cluster NGC 663. V1153 Cas |In the field of the open cluster NGC 663. V1155 Cas |VB A (A 11.1mV; B 13.2mV, 7", 120{deg}, 2012). In the field of the V1155 Cas |open cluster NGC 663. V1156 Cas |VB A (B 13.5mV, 12", 223{deg}, 2012). In the field of the open V1156 Cas |cluster NGC 663. V1157 Cas |In the field of the open cluster NGC 663. V1160 Cas |A twice shorter period is not excluded. V1162 Cas |MinII - MinI = 0.230P. V1170 Cas |In the open cluster IC 1848. V1176 Cas |MinII - MinI = 0.494P. V1177 Cas |MinII - MinI = 0.53P. V1179 Cas |VB A (B 13.8mV, 29", 323{deg}, 1999). The tabulated magnitudes can V1179 Cas |be distorted by the companion. V1180 Cas |In the dark cloud Lynds 1340. V1183 Cas |Multiperiodic. V1194 Cas |Multiperiodic. V1196 Cas |In the open cluster NGC 7789. V1197 Cas |In the open cluster NGC 7789. V1198 Cas |In the open cluster NGC 7789. V1199 Cas |In the open cluster NGC 7789. V1200 Cas |In the open cluster NGC 7789. V1201 Cas |In the open cluster NGC 7789. V1202 Cas |In the open cluster NGC 7789. V1203 Cas |In the open cluster NGC 7789. V1204 Cas |In the open cluster NGC 7789. V1205 Cas |In the open cluster NGC 7789. V1207 Cas |In the open cluster NGC 7789. V1208 Cas |In the open cluster NGC 7789. V1209 Cas |In the open cluster NGC 7789. V1210 Cas |In the open cluster NGC 7789. V1211 Cas |In the open cluster NGC 7789. V1212 Cas |In the open cluster NGC 7789. V1213 Cas |In the open cluster NGC 7789. V1214 Cas |In the open cluster NGC 7789. V1215 Cas |In the open cluster NGC 7789. V1216 Cas |In the open cluster NGC 7789. V1217 Cas |In the open cluster NGC 7789. V1218 Cas |In the open cluster NGC 7789. V1219 Cas |In the open cluster NGC 7789. V1220 Cas |In the open cluster NGC 7789. V1221 Cas |In the open cluster NGC 7789. V1222 Cas |In the open cluster NGC 7789. V1223 Cas |In the open cluster NGC 7789. V1224 Cas |In the open cluster NGC 7789. V1225 Cas |In the open cluster NGC 7789. V1226 Cas |In the open cluster NGC 7789. V1227 Cas |In the open cluster NGC 7789. V1228 Cas |In the open cluster NGC 7789. V1229 Cas |In the open cluster NGC 7789. V1230 Cas |In the open cluster NGC 7789. V1231 Cas |In the open cluster NGC 7789. V1232 Cas |In the open cluster NGC 7789. V1233 Cas |In the open cluster NGC 7789. V1234 Cas |In the open cluster NGC 7789. V1235 Cas |In the open cluster NGC 7789. V1236 Cas |In the open cluster NGC 7789. O'Connell effect. V1237 Cas |In the open cluster NGC 7789. V1238 Cas |In the open cluster NGC 7789. V1239 Cas |In the open cluster NGC 7789. V1240 Cas |In the open cluster NGC 7789. V1241 Cas |In the open cluster NGC 7789. V1242 Cas |In the open cluster NGC 7789. V1243 Cas |In the open cluster NGC 7789. V1244 Cas |In the open cluster NGC 7789. V1255 Cas |Type RRC with a twice shorter period is also possible. V1271 Cas |MinII - MinI = 0.525P. V1276 Cas |The light curve shape varies. V1277 Cas |Multiperiodic. V1280 Cas |Multiperiodic. V1292 Cas |P = 0.311336d is also possible. V1293 Cas |Oscillations outside MinI, amplitude 0.04mV, periods 0.12d and V1293 Cas |0.045d. V1315 Cas |Type DCEPS is also possible. V1316 Cas |VB B (A 14.3mV; AB 23", 165{deg}, 1998). The object 1SWASP V1316 Cas |J011732.10+525204.9, announced variable in [82030], is a blend of V1316 Cas |the non-variable component A near the SuperWASP position and the V1316 Cas |really variable component B. V1345 Cas |Type EW with a twice longer period is also possible. V1355 Cas |VB (companion: 6", 259{deg}, 1999). V1378 Cas |Type RRC with a twice shorter period is also possible. V1386 Cas |MinII - MinI = 0.465P. V1391 Cas |Porb = 0.15442d. V1402 Cas |VB A (14.0mG; B 16.2mG, 4.5", 194{deg}, 2000). V1404 Cas |VB A (16.3mG; B 16.8mG, 7", 158{deg}, 2000). V1405 Cas |Porb = 0.1883907d. bet Cas |SB, Porb = 27d. gam Cas |VB A (B 10.9m, 2", 259{deg}, 2002). SB? In the HII region S 185. V gam Cas |sin i = 310 km/s. eta Cas |SB. VB A (B 7.4mV, 13", 324{deg}, 2015). iot Cas |VB (Aa 4.63m, Ab 8.48m, 0.6", 42{deg}, 2010; B 6.92m, 3", 232{deg}, iot Cas |2015; C 9.05m, 7", 120{deg}, 2015). The range in the Table is for iot Cas |combined brightness. kap Cas |SB, Porb = 0.14035d. omi Cas |SB1, P = 1033d. V sin i = 220 km/s. rho Cas |Multiperiodic. B Cas |Tycho Brahe's supernova. Maximum probably around November 15, 1572. R Cen |H2O, SiO maser. VB A (B 11.2m, 27", 215{deg}, 2000). Double maxima, R Cen |the elements in the Table are for the brighter maximum. P R Cen |decreases, the Table presents current light elements. V Cen |In the open cluster NGC 5662. X Cen |SiO maser. Y Cen |H2O maser. Z Cen |SN 1895B (NGC 5253). RR Cen |P varies, the Table presents current light elements. RT Cen |OH maser. RX Cen |OH maser. SV Cen |P varies, quadratic term in the light elements: -7.502d x 10^(-8) x SV Cen |E^2. SX Cen |P2 = 610d. TW Cen |H2O maser. UW Cen |VB A (B 13.6m, 23", 336{deg}, 2000). Variations between minima: P = UW Cen |42.82d [N0488]. Associated with a faint nebula. UZ Cen |VB A (B 13.5m, 3", 192{deg}, 1938). The Table presents the UZ Cen |fundamental-mode period. First overtone: P1 = 1.355317d. WX Cen |Epoch of Min is given. Variations with the orbital period plus WX Cen |flickering. XX Cen |P varies, the Table presents current light elements. SB, Porb = XX Cen |909.4d. ZZ Cen |VB D (A 9.75m; B 11.1m, 8", 310{deg}, 1999; C = AA Cen, 12.2m, ZZ Cen |9.5", 110{deg}, 1999; D 12.4m, 9.3", 257{deg}, 1999). In [00027], ZZ Cen |ZZ Cen is called component C. AA Cen |VB C (A 9.75m; B 11.1m, 8", 310{deg}, 1999; C 12.2m, 9.5", AA Cen |110{deg}, 1999; D = ZZ Cen, 12.4m, 9.3", 257{deg}, 1999). In AA Cen |[00027], AA Cen is called component D. AB Cen |d = 0.06P. AQ Cen |OH, SiO, H2O maser. AR Cen |VB A (B 13.2m, 18", 185{deg}, 2000; other companions). AS Cen |VB AB (3", 199{deg}, 2000; there are other companions). AZ Cen |SB. BF Cen |In the region of the open cluster NGC 3766. BH Cen |In the region of the open cluster IC 2944. P varies, the Table BH Cen |presents current light elements. BI Cen |Blazhko effect, P = 79.4d. [Fe/H] = -0.83. BK Cen |Fundamental mode: see Table, A0 = 0.54m. First overtone: P1 = BK Cen |2.222967d, A1 = 0.22m. P1/P0 = 0.700. BP Cen |P varies? BV Cen |During half a century, time intervals between outbursts increase, BV Cen |becoming about 1000d by 2008. Possibly a Nova resembling GK Per, BV Cen |with the major outburst missed. Small-amplitude brightness variat BW Cen |VB A (B 14m, 19", 231{deg}, 2001). DP Cen |VB (5", 52{deg}, 1999; other components). The range in the Table is DP Cen |for combined brightness. DU Cen |P = 1d/N. DX Cen |Multiple. Closest companion: 14.0m, 10", 106{deg}, 2000. The DX Cen |variability range in the Table was influenced by the companions. DY Cen |Deep minima in 1897, 1901, 1924, 1929 [00030]. No recent deep DY Cen |minima, gradual brightness decrease. SB1, Porb = 39.67d. EL Cen |MinII - MinI = 0.31P? EU Cen |VB A (B 14m, 18", 91{deg}, 1997; other faint companions). FN Cen |Smaller-amplitude variations with P2 = 136d are superposed. GI Cen |V1 (NGC 5286). GZ Cen |VB A (B 5", 303{deg}). HN Cen |VB A (B 14m, 11", 175{deg}, 1999). IL Cen |Superposed shorter-period, smaller-amplitude variations. IX Cen |In the region of the open cluster NGC 3766. IY Cen |In the region of the open cluster IC 2944. KO Cen |Multiperiodic, P2 = 164d. KS Cen |[Fe/H] = -0.80. KT Cen |MinII - MinI = 0.47P. Apsidal motion. KW Cen |Blazhko effect? LN Cen |[Fe/H] = -1.89. LU Cen |A twice longer period is also possible. LW Cen |In the region of the open cluster IC 2944. In a nebula. ASAS-3 data LW Cen |show change of brightness level: 9.2m - 9.3m before JD 2453250, LW Cen |then 8.85m - 9.0m before 2454750, with subsequent gradual fading LX Cen |VB AB (6", 63{deg}, 2000). MN Cen |VB A (8.82m; B 10.3m, 7", 145{deg}, 2010; other companions). The MN Cen |magnitudes in the Table are for combined brightness. MQ Cen |Multiple star. The magnitudes in the Table are for combined MQ Cen |brightness. MU Cen |Porb = 0.341883d. NN Cen |VB A (B 16.4V, 3", 195{deg}, 1999, 2000; C 16.5V, 5",129{deg}, NN Cen |2000). QR Cen |In the region of the open cluster NGC 5381. QU Cen |VB B (A 12.0m; AB 9", 240{deg}, 2000). QZ Cen |Blazhko effect? V0339 Cen |VB A (B 12.0m, 17", 238{deg}, 2000). V0346 Cen |Apsidal motion, P = 321yr. The Table presents light elements for V0346 Cen |MinI. MinII = 2444654.0485 + 6.3221513d x E. In the region of the V0346 Cen |open cluster Stock 14. V0359 Cen |Superoutbursts occur with intervals of 307 - 397d. Superhumps: P = V0359 Cen |0.08092d. V0370 Cen |SiO maser. V0371 Cen |Unusual light curve with a secondary minimum at phase 0.22P from V0371 Cen |Catalina data. V0373 Cen |VB A (B 5", 329{deg}, 1999). V0378 Cen |P varies, the Table presents current light elements. Max = V0378 Cen |2434025.452 + 6.459493d x E + 0.0000001723d x E^2 [N0497]. V0383 Cen |MinII - MinI = 0.609P. V0384 Cen |DII = 0.08P. MinII - MinI = 0.65P. V0419 Cen |P varies, quadratic term -0.0000000475d x E^2. V0420 Cen |P varies, quadratic term -0.000090d x E^2. V0436 Cen |Porb = 0.0625d. The cycle of superoutbursts is about 300d. V0441 Cen |VB A (B 14.8mV, 9", 302{deg}, 2000; other companions). V0443 Cen |d = 0.02P. V0458 Cen |Strong Blazhko effect. V0459 Cen |Blazhko effect? V0465 Cen |Blazhko effect? V0481 Cen |Blazhko effect. V0483 Cen |Blazhko effect? P varies? V0491 Cen |Several close companions. V0495 Cen |d = 0.03P:. V0496 Cen |In the region of the open cluster NGC 4755. V0499 Cen |[Fe/H] = -1.43. V0503 Cen |Strong Blazhko effect. V0504 Cen |Occasional deep fadings, spectrum of a cataclysmic variable. V0505 Cen |VB A (B 15m, 20", 106{deg}, 1999). V0507 Cen |VB A (B 13m, 7", 210{deg}, 1996). V0509 Cen |VB (5", 276{deg}, 1999). V0514 Cen |Blazhko effect? V0532 Cen |Identification with the transient X-ray source 3A 1431-409 was V0532 Cen |suggested. V0539 Cen |VB A (B 13.6mF, 12", 172{deg}, 1999). V0540 Cen |VB (companion 14.8mF, 13", 109{deg}, 1999). V0547 Cen |VB A (B 5", 182{deg}, 1999). V0549 Cen |VB A (B 16m, 7", 126{deg}, 1999). V0565 Cen |Type RR with P = 0.238072 is also possible. V0570 Cen |Blazhko effect. V0571 Cen |VB A (B 13m, 22", 285{deg}, 2000; other components). V0574 Cen |VB A (B 4", 131{deg}, 2000); the Table presents combined V0574 Cen |magnitudes. Blazhko effect? V0587 Cen |Blazhko effect? V0592 Cen |The long-period, large-amplitude variations are superposed with V0592 Cen |faster variations, P = 41.7d, {Delta} m = 0.8m. V0593 Cen |In the region of the open cluster Stock 16. V0594 Cen |V133 (NGC 5139 = {omega} Cen); cluster non-member. V0618 Cen |OH maser. V0619 Cen |In the open cluster NGC 5319. Strongly blended; the range in the V0619 Cen |Table is for combined magnitudes. V0622 Cen |VB A (B 5", 77{deg}, 2000). V0633 Cen |Strong Blazhko effect? V0639 Cen |VB A (B 5", 234{deg}, 2000); the Table presents combined V0639 Cen |magnitudes. V0643 Cen |VB A (B 14m, 13", 158{deg}, 1999). V0645 Cen |Proxima Cen = {alpha} Cen C. Soft X-ray source. BY variations with V0645 Cen |a small amplitude; different authors report Prot from 31.5d to 42d. V0646 Cen |d = 0.02P. V0654 Cen |O'Connell effect. V0659 Cen |VB (0.63"). V0671 Cen |[Fe/H] = -1.40. V0672 Cen |O'Connell effect. V0674 Cen |Blazhko effect, P = 46.5d:. [Fe/H] = -1.53. V0687 Cen |DII = 0.12P. MinII - MinI = 0.580P. V0701 Cen |VB A (A 9.32mHp; B 10.06mHp, A0-2V-IV, 1.3", 30{deg}, 1991). The V0701 Cen |magnitudes in the Table are for combined brightness. V0723 Cen |A twice longer period is possible. V0727 Cen |A twice shorter period is not excluded. V0729 Cen |Blazhko effect. V0734 Cen |Blazhko effect? V0747 Cen |O'Connell effect. V0748 Cen |d = 0.08P. Long-term variations of the out-of-eclipse brightness V0748 Cen |between 10.36m and 11.2m. V0752 Cen |P varies, the Table presents current light elements. V0755 Cen |VB A (B 7", 31{deg}, 2000); combined magnitudes are given. Possible V0755 Cen |BY variations: 11.9 - 12.2mV, P = 80: d. V0761 Cen |SB. V0764 Cen |SB1. V0766 Cen |VB AaAb (7.31m, 7.70m, 0.1", 114{deg}, 1991; B 9.9m, 9", 318{deg}, V0766 Cen |1998). V0772 Cen |In the region of the open cluster IC 2944. V0778 Cen |VB A (A 10.2mV; B 11.6mV, 21", 205{deg}, 2000). V0779 Cen |Cen X-3 = 4U 1119-603. The light elements are for MinI of the V0779 Cen |eclipsing variations. X-ray pulses: P = 4.834477s (epoch JD V0779 Cen |2442785.3) [07612]. The orbital period and the pulse period vary. V0784 Cen |Variations with P = 87.3d are sometimes superposed. V0786 Cen |Physical variations outside eclipses can be present. V0790 Cen |P varies? VB C (J 9.56m, 10", 62{deg}, 2000). V0791 Cen |V269 in the globular cluster NGC 5139 ({omega} Cen). Cluster V0791 Cen |non-member. V0796 Cen |VB AB (10.1m, 13m, 11", 171{deg}, 2000). The Table presents the V0796 Cen |combined magnitude. V0801 Cen |Optical brightness variations related to the disk of the Be star. V0801 Cen |Pulsar, P = 292s. X-ray outbursts, about 10d in duration, at V0801 Cen |periastron passages of the neutron star (Porb = 186.5d). V0802 Cen |Helium spectrum, virtually without hydrogen lines. Three brightness V0802 Cen |states, "high" (12.7m - 13.3m), "low" (about 17m), and "cycling" V0802 Cen |(13.4m - 14.5m, at least 50% of the time). Variations with P about V0802 Cen |22 hours in the "cycling" state, probably similar to outbursts of V0802 Cen |dwarf novae. In the "low" state, outbursts probably have a cycle V0802 Cen |about 5d. At all phases, variations with P about 1612 V0802 Cen |seconds,possibly superhumps. V0805 Cen |MinII - MinI = 0.547P. V0807 Cen |VB AB (10.1m, 10.3m, 0.4", 258{deg}, 1931). V0810 Cen |In the open cluster Stock 14. V0811 Cen |Strongly blended. V0813 Cen |V65 in the globular cluster NGC 5139 ({omega} Cen). Cluster V0813 Cen |non-member. V0814 Cen |V78 in the globular cluster NGC 5139 ({omega} Cen). Cluster V0814 Cen |non-member. V0815 Cen |VB A (A 5.25mHp; B 7.96mHp, 1.3", 252{deg}, 1995). The range in the V0815 Cen |Table is for combined brightness. V0816 Cen |Multiperiodic. V0820 Cen |[Fe/H] = -1.72. V0822 Cen |Ellipsoidal variations in quiescence: Min = HJD 2446919.7744 + V0822 Cen |0.628935 x E, 19.24 - 19.62mB, MinII 19.44mB [N0508]. V0825 Cen |V2 in the globular cluster NGC 5139 ({omega} Cen). Cluster V0825 Cen |non-member. V0826 Cen |V129 in the globular cluster NGC 5139 ({omega} Cen). Cluster V0826 Cen |non-member. V0830 Cen |X-ray pulsar: Ppuls = 292s. V0831 Cen |VB ABC (A 5.3m, B 6.0m, 0.2", 125{deg}, 2015; AB 4.55m, C 8.4m, 2", V0831 Cen |15{deg}, 2015); other, more distant, components. The Table presents V0831 Cen |combined magnitudes for ABC. Presumably, A varies. V0832 Cen |V168 in the globular cluster NGC 5139 ({omega} Cen). Cluster V0832 Cen |non-member. V0833 Cen |V56 in the globular cluster NGC 5139 ({omega} Cen). Cluster V0833 Cen |non-member. Blazhko effect. V0836 Cen |Multiperiodic. V0837 Cen |Multiperiodic. V0838 Cen |VB AB (9.35m, 10.64m, 0.2", 231{deg}, 2015; C 13.5m, 14", 29{deg}, V0838 Cen |2000; D 14.0m, 8.5", 143{deg}, 2000). V0840 Cen |VB A (B 4", 313{deg}, 2000). V0841 Cen |SB1. V0843 Cen |In the open cluster NGC 3766. V0844 Cen |In the open cluster NGC 3766. V0845 Cen |In the open cluster NGC 3766. V0846 Cen |In the open cluster NGC 3766. V0847 Cen |In the open cluster NGC 3766. V0848 Cen |In the open cluster NGC 3766. V0849 Cen |In the open cluster NGC 3766. V0850 Cen |X-rays: pulsar, P = 272s; outbursts, P = 132.5d. V0851 Cen |SB1, Porb = 11.9886d. V0852 Cen |In the "Southern Crab" nebula. V0854 Cen |Possible quasi-period outside deep minima: 43.23d. V0855 Cen |In the open cluster NGC 3766. V0869 Cen |SB2, Porb = 26.036d. V0871 Cen |VB (A 7.10m; B 7.42m, 0.4", 117{deg}, 2015; AB is the eclipsing V0871 Cen |star and SB with P = 2.8d; C 9.9m, 1.7", 7{deg}, 2015; D 11.6m, V0871 Cen |9.5". 324{deg}, 2000). Combined magnitudes are given in the Table. V0883 Cen |The light elements in the Table are for eclipses. ACV variations: V0883 Cen |Prot = 61.46d, small amplitude. V0884 Cen |OH, SiO maser. V0885 Cen |The period in the Table is interpreted as due to interaction in an V0885 Cen |eccentric binary. Longer-term variations, P about 1700d. V0886 Cen |Multiperiodic. V0887 Cen |V2 in the globular cluster Ru 106. Cluster non-member, background V0887 Cen |object. V0898 Cen |SB. V0900 Cen |VB AB (7.08mV, 9.09mV, 0.4", 100{deg}, 1996). V0902 Cen |VB A (12.5mV; B 12.8mV, 12", 4{deg}, 1999). Spurious variability? V0903 Cen |P2 = 0.200233d. VB AB (9.73mHp, 12.48mHp, 5", 56{deg}, 1991). V0916 Cen |In the open cluster Stock 14. Superposed pulsations: P1 = 0.22447d, V0916 Cen |P2 = 0.54362d. V0933 Cen |HIPPARCOS data contradict the luminosity class V. V0960 Cen |MinII - MinI = 0.545P. V0963 Cen |MinII - MinI = 0.29P. V0969 Cen |In the open cluster Hogg 16. V0975 Cen |MinII - MinI = 0.073P. V0983 Cen |VB A (B 6.05m, 8", 104{deg}, 2013). V1000 Cen |MinII - MinI = 0.60P. V1002 Cen |VB A (B 11.5mV, 4", 131{deg}, 1963). V1006 Cen |In the open cluster NGC 5617. V1014 Cen |VB A (B 22", 217{deg}, 1998). Spurious variations in the HIP V1014 Cen |catalog? V1025 Cen |Porb = 0.05876d. V1030 Cen |In the region of the globular cluster NGC 5139. V1039 Cen |In May, 2004, varied between 15.60 and 15.75mV with P = 0.00832d V1039 Cen |[79019]. V1043 Cen |Porb = 0.1746d. V1044 Cen |Porb = 985d. V1045 Cen |In the region of the globular cluster NGC 5139. Background star. V1048 Cen |The Table gives the period of the first overtone (P1). Second V1048 Cen |overtone: P2 = 0.743241d. P2/P1 = 0.8058. V1051 Cen |In the open cluster IC 2944. V1056 Cen |VB A (B 11.5m, 20", 246{deg}, 1999); the magnitude in maximum is V1056 Cen |influenced by the companion. V1057 Cen |VB A (B 13.2m, 22", 290{deg}, 2000). V1059 Cen |VB A (B 13m, 26", 285{deg}, 1999); the magnitude in maximum is V1059 Cen |influenced by the companion. V1060 Cen |VB A (B 11.7m, 15", 151{deg}, 2000); the magnitudes in the Table V1060 Cen |are influenced by the companion. Possibly a Mira. V1070 Cen |VB A (B 14.4m, 23", 22{deg}; C 14.4m, 25", 218{deg}, 2000). V1070 Cen |Possibly a Mira. V1087 Cen |VB AB (9.9m, 10.3m, 0.8", 27{deg}, 1991). Apsidal motion, U = 169 V1087 Cen |years [79126]. V1089 Cen |MinII - MinI = 0.57P. V1090 Cen |VB, several close components. V1094 Cen |O'Connell effect, MaxII 9.98m. V1095 Cen |VB A (B 12.9m, 18", 172{deg}, 1999). V1100 Cen |VB A (B 13.2m, 17", 257{deg}, 2000; C 15.5m, 11", 129{deg}, 1999). V1104 Cen |VB (A 10.2m; B 12.0m, 13", 76{deg}, 2000). According to [79236], a V1104 Cen |double-periodicity eclipsing star: EB, P = 0.876114d, and EA, P = V1104 Cen |19.11d (MinI 2451938.733 [00001]). V1105 Cen |Superposed longer-term variation: P = 438d. V1118 Cen |MinII - MinI = 0.53P. V1119 Cen |VB (9.62m, 12.8m, 3", 122{deg}, 1966). V1123 Cen |Multiperiodic, P2 = 55d. V1129 Cen |Eclipses in quiescence: Max 9.55m. Brightens to 9.1m once in about V1129 Cen |357d. V1133 Cen |VB AB (10.3m, 10.6m, 0.5", 281{deg}, 1991). V1138 Cen |P varies. V1142 Cen |MinII - MinI = 0.41P. DII = 0.10P. V1152 Cen |The mean brightness varies with a cycle about 900d. V1155 Cen |X-ray source. VB B (A = HR 4940, 4.69m, B5V; B 11", 79{deg}, 2001; V1155 Cen |C 9.16mKs, 1.6", 268{deg}, 2000). V1157 Cen |VB B (A 10.5:m; B 25", 193{deg}, 2001). The magnitude at maximum in V1157 Cen |the Table was influenced by the companion. V1159 Cen |VB A (B 14m, 15", 72{deg}, 2001). V1161 Cen |Double maxima. V1166 Cen |MinII - MinI = 0.41P. V1167 Cen |Blazhko effect? V1176 Cen |MinII - MinI = 0.59P. V1180 Cen |VB A (B 12.7m, 12", 270{deg}, 1997). V1182 Cen |VB A (B 13.6mpg, 25", 277{deg}, 1998; C 13.9mpg, 18", 32{deg}, V1182 Cen |1998). V1184 Cen |P varies, the light elements in the Table are for JD 2455200 - V1184 Cen |2456500. V1185 Cen |VB A (B 14.6m, 7", 198{deg}, 1997). V1188 Cen |Blazhko effect. V1194 Cen |VB (A 10.0m; B 10.5m, 12", 309{deg}, 1999). V1197 Cen |VB A (B 13.6m, 15", 211{deg}; C 14.1m, 14", 307{deg}; D 10.3mJ, 6", V1197 Cen |337{deg}, 2004; other components). V1202 Cen |VB A (B 11.4m, 7", 356{deg}, 2000). V1210 Cen |The light elements in the Table are for the fundamental mode. P1 = V1210 Cen |3.037d, P1/P0 = 0.7035. V1214 Cen |The light elements in the Table are for the eclipses. Pulsations: P V1214 Cen |= 0.121252d, with an amplitude of 0.04m. V1215 Cen |VB A (A 11.87mR; B 13.11mR, 17", 51{deg}, 1999). V1229 Cen |P varies. dP/dT = 1.67 x 10^(-5) d/yr. VB AB (A 10.29m; B 10.44m, V1229 Cen |0.4", 231{deg}, 1991; C 10.80m, AB-C 16", 324{deg}, 2000). AB V1229 Cen |varies; the Table presents combined ABC magnitudes. V1235 Cen |VB A (B 11.5mR, 18", 199{deg}, 2000). V1238 Cen |VB B (A = V1239 Cen; AB 6", 276{deg}, 2000). V1239 Cen |VB A (B = V1238 Cen, 6", 276{deg}, 2000). V1250 Cen |VB A (B = V1251 Cen, 6", 16{deg}, 2000). V1251 Cen |VB B (A = V1250 Cen; AB 6", 16{deg}, 2000). V1258 Cen |The light elements in the Table are for eclipses in quiescence. The V1258 Cen |range of orbital variations is 15.4m - 17.0m in outburst, 18.2m - V1258 Cen |22.2m in quiescence. V1259 Cen |Multiperiodic. V1261 Cen |VB B (A 4.23mV; AB 25", 100{deg}, 2007). V1264 Cen |The light elements in the Table are for eclipses. Pulsations: P = V1264 Cen |0.0734d, with an amplitude of 0.21m. V1265 Cen |The period in the Table is twice shorter than that suggested in V1265 Cen |[79236]. Also detected is P = 3.537421d, close to that in the Table V1265 Cen |but differing from it. V1266 Cen |VB A (AaAb speckle: Aa 8.10m, Ab 11.00m, 0.1", 76{deg}, 2008; B V1266 Cen |10.84m, 9", 283{deg}, 2000). V1307 Cen |In the open cluster NGC 5381. V1309 Cen |In the open cluster NGC 5381. V1310 Cen |In the open cluster NGC 5381. V1312 Cen |In the open cluster NGC 5381. V1313 Cen |In the open cluster NGC 5381. V1314 Cen |In the open cluster NGC 5381. V1315 Cen |In the open cluster NGC 5381. V1316 Cen |In the open cluster NGC 5381. V1317 Cen |In the open cluster NGC 5381. V1318 Cen |In the open cluster NGC 5381. V1319 Cen |In the open cluster NGC 5381. V1320 Cen |In the open cluster NGC 5381. V1321 Cen |In the open cluster NGC 5381. V1322 Cen |In the open cluster NGC 5381. V1323 Cen |In the open cluster NGC 5381. V1324 Cen |In the open cluster NGC 5381. V1325 Cen |In the open cluster NGC 5381. V1326 Cen |In the open cluster NGC 5381. V1336 Cen |In the region of the open cluster NGC 5460. V1337 Cen |VB A (B 15m, 12", 90{deg}, 1990). V1338 Cen |P varies. The light elements in the Table are for JD 2454000 - V1338 Cen |2455100. V1339 Cen |First overtone: see Table, amplitude 0.38m. Second overtone: Max = V1339 Cen |2453556.358 + 0.506888d x E, amplitude 0.06m. V1353 Cen |Blazhko effect? V1357 Cen |VB A (B 14.8m, 13", 104{deg}, 2000). The magnitude in maximum in V1357 Cen |the Table is influenced by the companion. V1358 Cen |VB A (B 13m, 15", 34{deg}, 2000). V1360 Cen |First overtone: see Table, amplitude 0.39m. Fundamental mode: Max = V1360 Cen |2454200.806 + 0.463072d x E, amplitude 0.23m. V1362 Cen |P varies, dP/dt = 0.19 x 10^(-5) d/yr. VB AB (9.6m, 12.1m, 0.8", V1362 Cen |243{deg}, 1945). V1367 Cen |VB A (B 15m, 13", 108{deg}, 1999). V1375 Cen |Porb = 0.3604d? [81150]. V1389 Cen |SB2? V1393 Cen |Double-mode pulsations. For P1, see Table. P0 = 0.1177931d, P1/P0 = V1393 Cen |0.7712. V1397 Cen |Blazhko effect, P = 146d. V1400 Cen |Modulation with P = 3.21d, probably due to star spots. One deep V1400 Cen |minimum, with secondary fadings during 54d around it, was observed. V1406 Cen |The data for 1SWASP J111501.66-361254.2 in [82030] are combined V1406 Cen |measurements for a non-variable star (V = 15.4m) near the SuperWASP V1406 Cen |position and the real variable. V1411 Cen |The data for 1SWASP J121359.79-414742.7 in [82030] are combined V1411 Cen |measurements for a non-variable star (V = 13.2m) near the SuperWASP V1411 Cen |position and the real variable. V1415 Cen |In the field of the globular cluster NGC 5139 = {Omega} Cen. V1418 Cen |P = 60.7d is superposed. V1419 Cen |P = 45.0d is superposed. V1425 Cen |P = 14.896d is superposed. V1429 Cen |A secondary wave (possibly nonradial) with P = 0.103095d. V1431 Cen |Cluster non-member. O'Connell effect. V1434 Cen |Cluster non-member. V1449 Cen |Cluster non-member. V1450 Cen |Cluster non-member. V1452 Cen |Cluster non-member. V1453 Cen |Cluster non-member. V1454 Cen |Cluster non-member. V1455 Cen |Cluster non-member. V1458 Cen |Cluster non-member. V1459 Cen |Cluster non-member. V1462 Cen |Cluster non-member. V1466 Cen |Cluster non-member. Type BY is also possible. V1467 Cen |Blazhko effect? V1469 Cen |Cluster non-member. V1473 Cen |P varies? V1475 Cen |Blazhko effect? V1486 Cen |Cluster non-member. V1487 Cen |Cluster non-member? V1491 Cen |Blazhko effect. V1499 Cen |Cluster non-member. V1514 Cen |Blazhko effect? V1519 Cen |Blazhko effect? V1522 Cen |P varies? V1527 Cen |An extreme horizontal branch star. Multiperiodic. V1528 Cen |P varies? V1536 Cen |Blazhko effect. V1537 Cen |P varies? Blazhko effect? V1543 Cen |Cluster non-member. V1550 Cen |An extreme horizontal branch star. Multiperiodic. V1553 Cen |Blazhko effect. V1560 Cen |VB, the star has a brighter companion. V1568 Cen |P varies? V1570 Cen |P varies? V1573 Cen |Blazhko effect? V1576 Cen |Cluster non-member? V1579 Cen |P varies? V1586 Cen |Brighter than other RR Lyrae stars in the cluster; unresolved V1586 Cen |blend? V1598 Cen |Cluster non-member? V1601 Cen |Cluster non-member? V1603 Cen |P varies? V1607 Cen |Blazhko effect? V1616 Cen |Blazhko effect. V1621 Cen |According to [g1072], type RR(B) (RRB01). V1631 Cen |Cluster non-member. V1635 Cen |P varies. V1636 Cen |P varies? V1642 Cen |P varies? V1645 Cen |P varies? V1646 Cen |Blazhko effect. V1659 Cen |P varies? The light curve shape varies? V1664 Cen |P varies? V1675 Cen |P varies? V1685 Cen |Blazhko effect? V1693 Cen |P varies? V1696 Cen |O'Connell effect. V1703 Cen |An extreme horizontal branch star. Multiperiodic. V1704 Cen |Cluster non-member. V1718 Cen |The light curve shape varies? V1719 Cen |Cluster non-member? Possibly associated with an X-ray source. V1724 Cen |Cluster non-member? V1725 Cen |An extreme horizontal branch star. Multiperiodic. V1733 Cen |An extreme horizontal branch star. Multiperiodic. V1735 Cen |P varies? V1739 Cen |P varies? The light curve shape varies? V1751 Cen |P varies? V1752 Cen |Cluster non-member. Possibly associated with an X-ray source. V1759 Cen |Cluster non-member. V1766 Cen |O'Connell effect. V1768 Cen |Cluster non-member. V1780 Cen |Cluster non-member? V1787 Cen |P varies. V1789 Cen |Cluster non-member. V1796 Cen |The Gaia-DR2 proper motion contradicts cluster membership. V1802 Cen |Cluster non-member? V1806 Cen |Cluster non-member? V1808 Cen |P varies? V1809 Cen |Cluster non-member? V1810 Cen |Cluster non-member. The declination in [g1071] is wrong by one V1810 Cen |degree. V1814 Cen |Cluster non-member? V1817 Cen |Cluster non-member? V1818 Cen |Cluster non-member? V1819 Cen |Cluster non-member? V1822 Cen |Cluster non-member? V1825 Cen |Cluster non-member. V1826 Cen |Type EW (EC) with a twice longer period is not excluded. V1827 Cen |Cluster non-member? V1828 Cen |Cluster non-member. V1831 Cen |Cluster non-member? O'Connell effect. V1832 Cen |Cluster non-member. V1833 Cen |P varies? V1834 Cen |Cluster non-member. V1835 Cen |Cluster non-member. V1836 Cen |Cluster non-member. V1840 Cen |The observations presented for the star in [g1068] correspond to V1840 Cen |another variable. V1847 Cen |Very crowded field. V1868 Cen |Very croeded field. V1869 Cen |Blended with a bright nearby star. V1874 Cen |The observations presented for the star in [g1068] correspond to V1874 Cen |another variable. V1893 Cen |Blended. V1895 Cen |The observations presented for the star in [g1068] probably V1895 Cen |correspond to another variable. V1896 Cen |VB B (A 16.0mG, B 16.2mG; AB 2", 344{deg}, 2000). bet Cen |VB A (B 3.95m, 0.4", 196{deg}, 2014). SB, Porb = 357.02d. Soft bet Cen |X-ray source. del Cen |VB AaAb (0.1", 118{deg}, 2008). eps Cen |Double-mode pulsations. P2 = 0.1914d. mu. Cen |Different authors suggested several periods for small-scale mu. Cen |variations. nu. Cen |Possible BCEP variations with P = 0.1750d, with an amplitude of nu. Cen |0.008m, were detected only in the Stroemgren u band [N0530]. T Cep |H2O, OH, SiO maser. U Cep |VB A (B 11.8m, 14", 63{deg}, 2015; C 12.2m, 24", 315{deg}, 2015). d U Cep |= 0.03P. The light curve shapes varies. P varies, generally U Cep |increases; the Table presents current light elements. W Cep |Speckle interferometry: VB (0.26", 88{deg}, 1997). X Cep |H2O maser. OH maser? RS Cep |d = 0.04P. P varies, the Table presents current light elements. RT Cep |SiO maser. RZ Cep |[Fe/H] = -1.77. P varies. The light curve shape varies. SS Cep |Biperiodic. P0 is presented in the Table, P1 = 100d. SX Cep |In the region of the nebula NGC 7023. SZ Cep |VB A (B 11.2m, 24", 78{deg}, 2010). VV Cep |d is about 0.04P. Semiregular variations: mean period 116d. Several VV Cep |other periods were also suspected. A strong, variable magnetic VV Cep |field. VW Cep |VB A (B 10.3m, a = 0.51", Porb = 30.45 years). P varies, the Table VW Cep |presents current light elements. The light curve shape varies. VW Cep |X-ray source. WX Cep |d = 0.008P. WZ Cep |P varies, the Table presents current light elements. XX Cep |P varies, the Table presents current light elements. XY Cep |P varies, the Table presents current light elements. ZZ Cep |VB A (9.1m; B 9.9m, A2p, 4", 202{deg}, 2016; C 10.8m, A5V, 17", ZZ Cep |224{deg}, 2016); the range in the Table is influenced by the ZZ Cep |companions. AF Cep |VB A (B 14.0mV, 9", 79{deg}, 1999). AG Cep |H2O maser. AH Cep |The light curve shape varies. P varies, the linear elements in the AH Cep |Table are valid for JD 2445500 - 2454500. Probable light-time AH Cep |effect with P= 63.0 years [N0537]. AM Cep |OH, H2O maser. AV Cep |P varies, the Table presents current light elements. BB Cep |d = 0.05P. P varies? BE Cep |P varies, the Table presents current light elements. BF Cep |SiO maser. BR Cep |P varies? BU Cep |P varies, the Table presents current light elements. CO Cep |MinII - MinI = 0.551P. CQ Cep |P varies, the Table presents current light elements. Possible CQ Cep |additional intrinsic variations. CR Cep |P varies, the Table presents current light elements. CU Cep |H2O maser. CW Cep |VB A (B 10.2m, 0.5", 246{deg}, 2007; C 12.3m, 22", 309{deg}, 2003). CW Cep |Apsidal motion, P = 43 years; the non-linear term in the light CW Cep |elements is +/-0.0250d x sin(0.0626{deg} x E - 28.3{deg}). DH Cep |In the region of the open cluster NGC 7380. DK Cep |P varies, the Table presents current light elements. DO Cep |VB B (A = NSV 14168; Porb = 44.64 years, a = 2.42", e = 0.41). DP Cep |P varies, the Table presents current light elements. DQ Cep |Multiperiodic. DX Cep |[Fe/H] = -1.83. P varies. EF Cep |P varies, the Table presents current light elements. EG Cep |P varies, the Table presents current light elements. EH Cep |In the region of the nebula NGC 7023. EK Cep |MinII - MinI = 0.535P (epoch 1991.25). Apsidal motion, P = 4700 EK Cep |years [N0541]. EM Cep |In the region of the open cluster NGC 7160. VB A (7.1mV; C A2, EM Cep |12.6mV, 21", 279{deg}, 2003; other companions). P varies, the Table EM Cep |presents current light elements. EO Cep |P varies, the Table presents current light elements. EP Cep |In the open cluster NGC 188. EQ Cep |In the open cluster NGC 188. ER Cep |In the open cluster NGC 188. ES Cep |In the open cluster NGC 188. ET Cep |In the region of the open cluster NGC 188. EZ Cep |[Fe/H] = -0.01. FH Cep |P varies, the Table presents current light elements. FL Cep |d = 0.02P. FT Cep |VB A (B 18.3m, 5", 27{deg}, 1999). In the region of the nebula NGC FT Cep |7023. FU Cep |In the region of the nebula NGC 7023. FY Cep |VB A (B 16.8m, 10", 302{deg}, 1999). GH Cep |H2O maser. GI Cep |P varies, the Table presents current light elements. GK Cep |P varies, the Table presents mean light elements. Orbital motion GK Cep |due to a third body, P = 20.5 years. GL Cep |In the region of the open cluster IC 1396 and gaseous nebulae. GM Cep |In the region of the open cluster IC 1396 and gaseous nebulae. GP Cep |In a nebula. Believed to consist of two unresolved eclipsing pairs. GP Cep |The Table presents the elements for one of them; MinII 9.03m. The GP Cep |second one: Min = 2443689.16 + 3.4696d x E, with the depth of GW Cep |P varies, the Table presents current light elements. HI Cep |P varies? The Table presents current light elements. HO Cep |Variability announced in [03905] is probably spurios; a HO Cep |high-proper-motion star. HS Cep |Not red [00001]. HZ Cep |In the region of the nebula NGC 7023. IL Cep |VB A (B 11.9m, 8", 329{deg}, 2012). According to [N0550], component IL Cep |B is an irregilar variable, 11.37mV - 12.63mV. IM Cep |P varies, the Table presents current light elements. IO Cep |P varies, the Table presents current light elements. IR Cep |VB AB (8.3m, 8.3m, 0.2", 22{deg}, 1992). IW Cep |MinII - MinI = 0.52P. P varies, the Table presents current light IW Cep |elements. IX Cep |d = 0.03P. KL Cep |d = 0.019P. KP Cep |P varies? KV Cep |VB A (B 7", 58{deg}, 2000). KY Cep |An object found in a spectrogram and believed to be a flare that KY Cep |lasted for about 65s. KZ Cep |VB AB (8.5m, 8.6m, 2", 248{deg}, 2016). LP Cep |P varies, the Table presents current light elements. LQ Cep |VB A (B 14.8m, 8", 259{deg}, 1999). MX Cep |SB, Porb = 16.03d. MY Cep |OH, H2O, SiO maser. In the region of the open cluster NGC 7419. MZ Cep |In the region of the open cluster NGC 7419. NW Cep |VB A (10.9mV; B 12.3mV, 11", 86{deg}, 1999). NY Cep |VB A (B 10.18m, 0.2", 253{deg}, 1991). SB2, e = 0.443. OQ Cep |In the region of the nebula NGC 7635. OT Cep |P varies, the Table presents current light elements. PR Cep |SiO maser. PS Cep |In the region of the open cluster NGC 7380. PV Cep |In a dark nebula. Associated with the fan nebula GM 1-29 and a PV Cep |bipolar flow. PW Cep |In the region of the nebula NGC 7023. PY Cep |SiO maser. QT Cep |In a group of stars in the nebulous patch GM 1-79. V0348 Cep |VB B (A 14.2mV; B 19.3mV, 11", 318{deg}, 1999). V0349 Cep |Blended. There are no very red stars in the field. V0351 Cep |P varies. V0359 Cep |VB (6", 328{deg}, 2000). The components of the pair are not red. V0360 Cep |VB AB (8.8m, 9.8m, 1.2", 147{deg}, 2008). V0361 Cep |In the region of the nebula NGC 7129. H2O maser. V0366 Cep |In the region of the open cluster Tr 37. V0367 Cep |X-ray source. V0369 Cep |V7 in the old open cluster NGC 188. VB B (AB 4", 313{deg}, 1999). V0370 Cep |V6 in the old open cluster NGC 188. VB B (AB 5", 292{deg}, 1999). V0371 Cep |V5 in the old open cluster NGC 188. V0372 Cep |V8 in the old open cluster NGC 188. X-ray source. V0373 Cep |In the region of the nebula NGC 7129. H2O maser. V0375 Cep |In the region of the open cluster NGC 7142. V0376 Cep |SB2. VB B (A 6.98m; B 13", 66{deg}, 2016). V0377 Cep |Multiperiodic. V0380 Cep |In the nebula NGC 7023. OH maser. V0381 Cep |VB Aa, Ab (5.90m, 7.42m, 0.1", 123{deg}, 2006; B 9.27m, B2V, 5", V0381 Cep |45{deg}, 2002). V0383 Cep |P varies? The Table presents current light elements. V0390 Cep |In the nebula IC 1396A. V0391 Cep |Associated with a small nebula. V0392 Cep |In the nebula RNO 138. V0397 Cep |In 2000, MinII - MinI = 0.573P. Apsidal motion. V0399 Cep |In the nebula and open cluster NGC 7822. V0421 Cep |P = 2.5069d is not excluded. SB, P1 = 5.4136d, P2 = 225.44d. V0425 Cep |VB AB (9.45mV, 11.19mV, 0.3", 54{deg}, 2007). V0432 Cep |In the region of the open cluster Trumpler 37. V0435 Cep |In the region of the open cluster Trumpler 37. V0436 Cep |The light curve has eclipse-like features. V0447 Cep |VB (A 8.0mV; B 8.3mV, 0.8", 234{deg}, 2014; C 11.9mV, 29", V0447 Cep |261{deg}, 2013: D 13.0mV, 29", 81{deg}, 2013). Possibly, it is the V0447 Cep |B component that actually varies. V0448 Cep |Also possible is P = 213d. SB, Porb = 7.7320d. V0453 Cep |VB A (A 7.6mV, B 9.5mV, 9", 137{deg}, 2015). V0454 Cep |Slight apsidal motion. V0458 Cep |In the open cluster Markarian 50. Assiciated with the nebula S 157. V0458 Cep |VB AB (10.50mV, B1II; 10.64mV, WN4.5, 1.4", 128{deg}, 2010; C V0458 Cep |14.3m, 11", 93{deg}, 2003). V0463 Cep |In the nebula and open cluster NGC 7822. VB AB (10.8mV, 11.0mV, 8", V0463 Cep |225{deg}, 2015). V0464 Cep |VB A (B 15.0m, 9", 68{deg}, 1999). V0465 Cep |In the open cluster NGC 6939. V0466 Cep |In the open cluster NGC 6939. V0467 Cep |In the open cluster NGC 6939. V0468 Cep |In the open cluster NGC 6939. Not red. V0469 Cep |In the open cluster NGC 6939. P = 1.165d is also possible. V0470 Cep |In the open cluster NGC 6939. V0476 Cep |VB A (B 16.6mV, 11", 332{deg}, 2000). V0488 Cep |In the region of the nebula IC 1396. V0496 Cep |SiO maser. V0497 Cep |In the open cluster NGC 7160. VB A (B 9.0m, 10", 56{deg}, 2011). V0521 Cep |VB A (B 15.9pg, 11", 85{deg}, 1989). V0527 Cep |The period is decreasing. V0554 Cep |VB (13.8mV, 13.8mV, 13", 1{deg}, 1999). V0572 Cep |Erroneously identified with GSC 4253.01889 in [76012]. The V0572 Cep |amplitude in the Table can be influenced by neighbor stars. V0584 Cep |VB A (B 13.9mpg, 10", 131{deg}, 1999). V0587 Cep |The amplitude in the Table can be influenced by neighbor stars. V0614 Cep |VB A (B 15.5mV, 3", 31{deg}). V0615 Cep |VB A (B 15.8mV, 7", 188{deg}). V0628 Cep |VB A (B 5", 284{deg}). V0632 Cep |Blended. V0637 Cep |VB A (A 13.5mV, B 14.4mV; AB 11", 162{deg}, 2000). The magnitudes V0637 Cep |in the Table are for combined brightness. V0660 Cep |VB A (B 16.5mpg, 4", 292{deg}, 1990). V0663 Cep |It is assumed that the variability announcement really referred to V0663 Cep |IRAS 22211+5821, which is GSC 3994.01126, and not to GSC V0663 Cep |3994.00911. In a nebula. V0688 Cep |The magnitudes in the Table are influenced by the neighbor, GSC V0688 Cep |3995.00495. V0698 Cep |MinII - MinI = 0.423P. V0702 Cep |In the open cluster NGC 7762. V0704 Cep |SiO maser. V0705 Cep |SiO maser. V0708 Cep |SiO maser. V0710 Cep |VB AB (7.8m, 9.4m, 0.6", 250{deg}, 2008). V0711 Cep |VB AB (9.6m, 9.9m, 5.5", 325{deg}, 2016). V0713 Cep |Eclipses in quiescence: 18.0mV - 21.0:mV. Min = 2456532.192754 + V0713 Cep |0.085418509d x E [N0567]. V0732 Cep |Multiperiodic. V0734 Cep |MinII - MinI = 0.55P. V0738 Cep |VB A (B 14.1mV, 14", 141{deg}, 2000). V0741 Cep |VB (9.2mHp, 12.7mHp, 0.7", 9{deg}, 1991). V0743 Cep |MinII - MinI = 0.53P:. SB2. V0747 Cep |MinII - MinI = 0.25P. In the open cluster NGC 7822. V0750 Cep |MinII - MinI = 0.44P:. V0757 Cep |P varies, the Table presents current light elements. V0759 Cep |In the region of the old open cluster NGC 188, probable non-member. V0760 Cep |In the region of the old open cluster NGC 188, non-member. V0761 Cep |In the region of the old open cluster NGC 188, non-member. V0764 Cep |In the region of the old open cluster NGC 188, non-member. V0771 Cep |Blended. V0777 Cep |In the region of the old open cluster NGC 188, non-member. V0789 Cep |O'Connell effect. In the region of the old open cluster NGC 188, V0789 Cep |non-member. V0790 Cep |In the region of the old open cluster NGC 188, non-member. V0791 Cep |In the region of the old open cluster NGC 188, non-member. V0792 Cep |In the region of the old open cluster NGC 188, non-member. V0793 Cep |In the region of the old open cluster NGC 188, non-member. V0796 Cep |P varies? The Table presents current light elements. V0798 Cep |MinII - MinI = 0.232P. V0800 Cep |VB A (A 13.0mV; B 16m, 9", 178{deg}, 1999). V0810 Cep |O'Connell effect. V0818 Cep |In the region of the open cluster NGC 6939, non-member. V0821 Cep |VB A (B 17.9mR, 4", 253{deg}, 2000). V0822 Cep |Type EW with a twice longer period is not excluded [00001]. V0835 Cep |Type RRC with the light elements Max = 2451511.899 + 0.2261d x E is V0835 Cep |not excluded. V0839 Cep |VB AB (9.9mV, 11.7mV, 0.2", 212{deg}, 2008). MinII - MinI = 0.511P. V0850 Cep |MinII - MinI = 0.599:P. V0855 Cep |VB AB (5", 247{deg}, 1999). V0870 Cep |P varies? The Table presents current light elements. V0873 Cep |Multiperiodic. V0874 Cep |Multiperiodic. V0880 Cep |MinII - MinI = 0.540P. V0881 Cep |MinII - MinI = 0.476:P. V0882 Cep |VB A (B 14.6mV, 7", 274{deg}, 1999). V0897 Cep |MinII - MinI = 0.518P. V0919 Cep |The Table presents current light elements (1999 - 2015). In 1999, V0919 Cep |MinII -MinI = 0.44P. Apsidal motion. V0921 Cep |MinII - MinI = 0.429P. V0922 Cep |MinII - MinI = 0.585P. VB A (A 10.6mJ; B 11.9mJ, 11", 44{deg}, V0922 Cep |1999; C 13.6mJ, 4", 76{deg}, 1999). The magnitudes in the Table V0922 Cep |might be influenced with the companions. V0930 Cep |P varies? The Table presents current light elements. V0944 Cep |MinII - MinI = 0.528P. V0947 Cep |VB A (B 7", 312{deg}, 1999; C 11", 350{deg}, 1999). V0954 Cep |O'Connell effect. V0957 Cep |MinII - MinI = 0.58P in 2012. Apsidal motion. V0961 Cep |MinII - MinI = 0.482P. V0964 Cep |VB A (B 4", 281{deg}, 1999). V0972 Cep |In the region of the open cluster NGC 6939. Cluster non-member. V1004 Cep |MinII - MinI = 0.22P. V1009 Cep |Multiperiodic. V1015 Cep |P varies, the Table presents current light elements. V1024 Cep |Eclipses: Min = 2451859.2468 + 0.14872385d x E, amplitude 1.4m. V1026 Cep |P = 76.5d is superposed. V1040 Cep |VB A (B 12.9mV, 1.0", 124{deg}, 2008). V1043 Cep |Blazhko effect, P = 140d. V1048 Cep |VB B (A 15.4mG, B 15.5mG; AB 18", 200{deg}, 2000). The A-component V1048 Cep |(V = 16.0m) contributes to the magnitudes in the Table. V1056 Cep |VB A (14.7mG; B 16.7mG, 6", 263{deg}, 2000). V1057 Cep |VB A (14.2mG; B 15.8mG, 7", 326{deg}, 2000). V1059 Cep |Min II - Min I = 0.46P. V1082 Cep |VB A (12.5mG; B 13.1 nG, 5", 61{deg}, 2000). The variability range V1082 Cep |in the Table was influenced by the companion. V1085 Cep |MinII - MinI = 0.55P. V1088 Cep |Double-mode pulsations. P0 is presented in the Table. P1 = V1088 Cep |0.079165d, P1/P0 = 0.7706. V1111 Cep |VB B (A 13.8mG, B 14.5mG; AB 6", 77{deg}, 2000; common proper V1111 Cep |motion). V1113 Cep |MinII - MinI = 0.79P. bet Cep |P varies. VB Aa (Ab 6.6mV, 0.2", 226{deg}, 2007; B 8.6m, 13.5", bet Cep |251{deg}, 2016). del Cep |P varies, the Table presents current light elements. VB A (B 6.1mV, del Cep |B7IV, 41", 2016; other companions). eps Cep |Multiperiodic. zet Cep |Radial velocity varies. mu. Cep |Multiperiodic. SiO maser. VB A (B 12.3mV, 19", 259{deg}, 2012; mu. Cep |other components). nu. Cep |Other reported periods: 170d, 190d [80268], 5d [68370]. W Cet |S5.5/2e. RR Cet |[Fe/H] = -1.26. P var. During JD2417500 - 28820 Max = 2417501.444 + RR Cet |0.55302577d*E; since JD2433180 - see Table. According to [08726], RR Cet |the graph of O - C deviations from the elements given in [03506] is RR Cet |approximately sinusoidal, with Pi = 2600d and the amplitude 0.025d. RU Cet |(k - b)2 = 0.01. {Delta}(m) var? P var [02455]. Max = 2426964.019 + RU Cet |0.5863003d*E (JD2426500 - 28430) [00181]; Max = 2434143.056 + RU Cet |0.5862676d*E (JD2433100 - 35820) [02431]; since JD2435820 - see RU Cet |Table. RV Cet |{Delta}(S) = 9. RW Cet |Min II 10.5. P var. During JD2426500 - 41000 Max = 2426585.503 + RW Cet |0.9751814d*E [00001]; since JD2441000 - see Table. RX Cet |{Delta}(S) = 5. P var. Before JD2428500 Max = 2425938.271 + RX Cet |0.5737100d*E [03506]; since JD2430000 - see Table. RZ Cet |{Delta}(S) = 6.7. P var. During JD2426585 - 28630 Max = 2426585.448 RZ Cet |+ 0.510633d*E [03506]; current elements - see Table. SS Cet |d = 0.025P. P var. Min = 2429321.250 + 2.9739509d*E (JD2427340 - SS Cet |30700) [02419]; Min = 2430698.160 + 2.973992d*E (JD2429300 - 36650) SS Cet |[03115]; since JD2440000 - see Table. SV Cet |Min II 14.9. TT Cet |Min II 11.1. TU Cet |D = 0.043P. Min II 10.9. Min II - Min I = 0.478P. According to TU Cet |[03564], the spectrum is K2. TV Cet |Min II 9.10. DII = 0.03P. Min II - Min I = 0.494P. TW Cet |Min II 11.14. P var. Min I = 2430965.595 + 0.316852d*E (JD2427650 - TW Cet |31000) [00192]; Min I = 2433611.3121 + 0.316846d*E (JD2433530 - TW Cet |615) [00001]; since JD2440000 - see Table. TX Cet |B - V: +0.34, +0.37. Min II 11.12. TY Cet |Min II 12.1. UU Cet |(k - b)2 = 0.08. P var. Blazhko effect? UV Cet |VB B (A 12.45m, dM5.5e; a = 2.1", P = 25a). VV Cet |Min II 11.0. EB type is also possible. RR type with twice shorter VV Cet |period is not excluded. VX Cet |d = 0.026P. VY Cet |Min II 11.70. VZ Cet |ADS 1778 B (B 0.61", 122{deg}; A = {omicron} Cet). Small variations VZ Cet |are also observed on the time scale of several hours, with VZ Cet |superimposed 10 - 15 minute variations and rare flares of VZ Cet |approximately 2 minute duration [06492]. A possible white dwarf VZ Cet |with an accretion disc [08926]. WW Cet |VR var (P = 0.160d) [04712]. Rapid oscillations (~10 min) of WW Cet |brightness are observed [04709]. WZ Cet |Min II 11.0. XY Cet |d = 0.02P. Min II 9.34. YY Cet |Min II 9.2. ZZ Cet |4 stable oscillations are observed simultaneously: P1 = ZZ Cet |213.132605s, P2 = 212.768427s, P3 = 274.250814s, P4 = 274.774562s. AA Cet |ADS 1581 A (B 7.7m vis, SB 2, F5, 8.5", 304{deg}). Min II 6.7:. dII AA Cet |= 0.065P. AB Cet |ADS 1849 A (B 9.30m, 12", 293{deg}). SB? (VR var, P = 2.997814d). AB Cet |The period of magnetic variations is 15.9d [08932]. AD Cet |ADS 180 A (B 10m, 3", 4{deg}). CL Cet |Type ELL: is also possible. EE Cet |The variability may be due to the fainter (B) component. EL Cet |SB2. EV Cet |The depth of MinII is 0.44. FH Cet |MinII 13.8. FL Cet |The light elements given are for the eclipses. FR Cet |A shell star of the spectral type A. FU Cet |Chomospherically active giant, photometric variations with the FU Cet |rotational period. GO Cet |Variable brown dwarf. GP Cet |Min II = 9.89. GR Cet |Min II = 11.47. P varies. dP/dt = -0.39x10^(-5) d/yr. GW Cet |Blazhko effect with a possible period about 84d. GY Cet |Pulsation periods: 595s, 335s, etc. Porb = 81.54min. GZ Cet |Porb = 0.060d. HI Cet |Min II = 13.07. HK Cet |Multiperiodic. VB A (B Sp L6, 0".3). HS Cet |Min II = 11.1. IO Cet |VB A (12.1mV; B 13mV, 14", 173{deg}, 1998). The range in the Table IO Cet |is for combined magnitudes. IQ Cet |P1 is presented in the Table; P1/P0 = 0.7438. IU Cet |P1 is presented in the Table; P1/P0 = 0.7425. IZ Cet |SB, Porb = 8.1194d. KM Cet |P1 is presented in the Table. P0 = 0.542695d. KN Cet |Eclipsing variability outside outbursts: 17.2m*-19.9m*, Min = KN Cet |2455202.5579 + 0.05298466 x E [81196]. KR Cet |P1 is presented in the Table; P1/P0 = 0.7434. KS Cet |P1 is presented in the Table. P0 = 0.564845d; P1/P0 = 0.7456. KY Cet |Period strongly varies. The light elemens in the Table are for JD KY Cet |2455600 - 56600. LN Cet |P1 is presented in the Table. P0 = 0.530534d; P1/P0 = 0.7459. LQ Cet |P1 is presented in the Table. P0 = 0.465495d; P1/P0 = 0.7433. LT Cet |Additional non-radial mode, P = 0.2820182d, or Blazhko effect, P = LT Cet |231d. LU Cet |Multiperiodic. P2 = 0.8488154d, P3 = 0.4776334d. del Cet |Nonlinear term: +2.20d*10**(-11)*E**2. omi Cet |ADS 1778 A (B = VZ Cet, 0.61", 122{deg}). Maser SiO, OH, H2O. S Cha |VB A (B 9.3mV, 22", 132{deg}, 2000). T Cha |In a dark nebula. Sometimes quasi-periodic; for example, P = 3.29d T Cha |could be detected on JD 2458500 - 2458700. Z Cha |VB A (15.7mG; B 17.2mG, 6", 79{deg}, 2000). Eclipses: Min = Z Cha |2440264.68070 + 0.0744993048d x E [N0583]. Eclipses during an Z Cha |outburst: 12.9mV - 14.5mV, D = 0.11P. Eclipses outside outbursts: D Z Cha |= 0.06P. RR Cha |Eclipses: P = 0.1401d, 18.1mV - 19.0mV, D = 0.2P; superhumps and RR Cha |quasi-periodic oscillations [10202]. Spectroscopic observations RR Cha |only at low brightness. RS Cha |According to [08403], one of the components is a DSCTC pulsator RS Cha |with the dominant period between 0.074d and 0.097d. According to RS Cha |[N0585], both components are Herbig Ae stars with non-radial RS Cha |oscillations. RV Cha |[Fe/H] = -1.66. RW Cha |P varies, light elements for JD 2458700 - 2459610 are presented in RW Cha |the Table. RX Cha |Cycle of superoutbursts: 717.9d [N0587]. ST Cha |Porb = 0.23d. SX Cha |VB AB (14.3mG, 14.7mG, 2.2", 289{deg}, 2000). In the Cha I SX Cha |association. The range in the Table is for combined brightness. SY Cha |In the Cha I association. Periodic variations: 13.0 - 13.6mV, P = SY Cha |6.1314d [00001]. SZ Cha |In the Cha I association. TW Cha |In the Cha I association. TZ Cha |VB A (15.9mG; B 17.4mG, 7", 116{deg}, 2000). UU Cha |In the region of the Cha I association. UV Cha |In the Cha I association. UX Cha |In the Cha I association. UY Cha |In the Cha I association. UZ Cha |In the Cha I association. VV Cha |VB (A 14.2mG; B = 14.8mG, 0.8", 14{deg}, 2016). In the Cha I VV Cha |association. VW Cha |VB (A 12.4mG; B = 12.8mG, 0.7", 176{deg}, 2000; other companions). VW Cha |HN Cha in the vicinity. In the Cha I association. VX Cha |In the region of the Cha I association; non-member. VY Cha |In the Cha I association. VZ Cha |In the Cha I association. WW Cha |In the Cha I association. WX Cha |In the Cha I association. WY Cha |In the Cha I association. WZ Cha |In the Cha I association. XX Cha |In the Cha I association. AN Cha |VB A (14.6mG; B 15.5mG, 13", 138{deg}, 2000). AT Cha |VB A (12.2mG; B 12.6mG, 11", 199{deg}, 2000). AY Cha |VB A (14.7mG; B 15.9mG, 14", 253{deg}, 2000). BC Cha |In the Cha II association. BF Cha |In the Cha II association. BK Cha |In the Cha II association. VB AB (14.2mG, 14.5mG, 0.8", 25{deg}, BK Cha |2016). BL Cha |VB A (15.0mG; B 16.1mG, 8.5", 308{deg}, 2000). BM Cha |In the Cha II association. BS Cha |P varies? Blazhko effect? BY Cha |VB A (15.2mG; B 16.4mG, 13", 298{deg}, 2000). CD Cha |VB A (14.8mG; B 15.4mG, 10", 126{deg}, 2000). CM Cha |In the Cha II association. CP Cha |VB A (13.6mG; B 14.8mG, 6", 327{deg}, 2000). CR Cha |In the Cha I association. CS Cha |In the Cha I association. CT Cha |In the Cha I association. CU Cha |In the Cha I association. CV Cha |In the Cha I association. VB (A = CV Cha, 10.5mG; B = CW Cha, CV Cha |14.7mG, 11", 99{deg}, 2000; other companions). CW Cha |In the Cha I association. VB (A = CV Cha, 10.5mG; B = CW Cha, CW Cha |14.7mG, 11", 99{deg}, 2000; other companions). DI Cha |In the Cha I association. VB A (10.2mG; B 15.3mG, 4.6", 202{deg}, DI Cha |2000). DK Cha |In the Cha II association. DX Cha |P = 0.02731d is also possible. EE Cha |Multiperiodic. P2 = 0.03412d. EF Cha |Multiperiodic. P2 = 0.03435d. EG Cha |In the {eta} Cha association. EH Cha |In the {eta} Cha association. EI Cha |In the {eta} Cha association. EK Cha |In the {eta} Cha association. EL Cha |In the {eta} Cha association. EM Cha |In the {eta} Cha association. EN Cha |In the {eta} Cha association. EO Cha |In the {eta} Cha association. EP Cha |In the {eta} Cha association. EQ Cha |In the {eta} Cha association. Multiperiodic, P2 = 1.24d. ES Cha |In the {eta} Cha association. ET Cha |In the {eta} Cha association. VB A (13.3mG; B 14.6mG, 6", 211{deg}, ET Cha |2000). EV Cha |VB A (12.0mG; B 13.6mG, 14", 104{deg}, 2000). FH Cha |In the region of the Cha I association, non-member. FI Cha |In the Cha I association. FK Cha |In the Cha I association. FL Cha |In the Cha I association. FM Cha |In the Cha I association. FN Cha |In the Cha I association. FO Cha |In the Cha I association. VB A (14.5mG; B 15.9mG, 12", 161{deg}, FO Cha |2000). GK Cha |VB A (13.5mG; B 16.0mG, 7", 35{deg}, 2000). GM Cha |In the Cha I association. VB B (A 10.25m; AB 10", 57{deg}, 2000). GO Cha |VB A (10.8mG; B 12.9mG, 7", 29{deg}, 2000). GP Cha |P2 = 1190d. GR Cha |In the Cha I association. GS Cha |In the region of the Cha I association. VB A (16.6mG; B 17.7mG, GS Cha |5.3", 325{deg}, 2000). GT Cha |In the region of the Cha I association. VB A (16.6mG; B 17.1mG, GT Cha |7.7", 320{deg}, 2000). GU Cha |In the Cha I association. GV Cha |In the region of the Cha I association. GW Cha |In the region of the Cha I association. GX Cha |In the Cha I association. GY Cha |In the region of the Cha I association. GZ Cha |In the Cha I association. HH Cha |In the region of the Cha I association. HI Cha |In the Cha I association. HK Cha |In the Cha I association. HL Cha |In the Cha I association. HM Cha |In the Cha I association. VB B (A 17.5mG, B 18.9mG; AB 10", HM Cha |298{deg}, 2000). HN Cha |In the Cha I association. VW Cha in the vicinity. HO Cha |In the Cha I association. VB B (A 15.4mG, B = NSV 18675, 16.2mG; AB HO Cha |16", 82{deg}, 2016). HP Cha |In the Cha I association. VB (A 10.5mG, G5e; B 12.5mG, K3, 2.5", HP Cha |286{deg}, 2000). HQ Cha |In the Cha I association. HR Cha |In the Cha I association. HS Cha |In the Cha I association. HT Cha |In the Cha I association. HU Cha |In the Cha I association. HV Cha |In the Cha I association. HW Cha |In the Cha I association. HX Cha |In the Cha I association. HY Cha |In the Cha I association. HZ Cha |In the Cha I association. IK Cha |In the Cha I association. IL Cha |In the Cha I association. IM Cha |In the Cha I association. IN Cha |In the Cha I association. IO Cha |In the Cha I association. IP Cha |In the region of the Cha I association, non-member. VB A (16.0mG; B IP Cha |17.0mG, 9", 341{deg}, 2000). IW Cha |V2 in the globular cluster E3. Considered a cluster non-member in IW Cha |[N0590], but the Gaia EDR3 proper motion suggests membership. IX Cha |V1 in the globular cluster E3. VB B (A 16.53mG, B 17.26mG; AB 2", IX Cha |165{deg}, 2000). zet Cha |SB. Y Cir |LPB pulsations: P = 1.108888d, peak-to-peak amplitude 0.06mV Y Cir |[80281]. RT Cir |VB A (14.9mG; B 15.4mG, 9", 27{deg}, 2000). RU Cir |VB B (A 11.6mG, B 13.0mG; AB 13", 57{deg}, 2000). TX Cir |VB A (11.9mG; B 13.5mG, 1.8", 105{deg}, 2000). TY Cir |VB A (10.8mG; B 12.4mG, 3.3", 35{deg}, 2000). TZ Cir |P varies? UZ Cir |Secondary minimum at phase 0.86P. YY Cir |VB A (13.3mG; B 15.4mG, 7", 166{deg}, 2000). AF Cir |VB A (12.7mG; B 14.0mG, 14", 337{deg}, 2000). AN Cir |VB A (13.4mG; B 15.0mG, 5", 329{deg}, 2000). AR Cir |VB A (B 13.7mG, 3.3", 143{deg}, 2000). AT Cir |P varies? AX Cir |SB, Porb = 6532d. AZ Cir |VB A (14.0mG; B 15.1mG, 10", 70{deg}, 2000). The variability range AZ Cir |in the Table could be influenced by the companion. BH Cir |VB A (15.7mG; B 16.3mG, 12", 87{deg}, 2000; other components). BL Cir |VB A (14.4mG; B 15.5mG, 6", 230{deg}, 2000; other components). BN Cir |MinII - MinI = 0.78P. BR Cir |Cir X-1. The star has a close companion. Drops of X-ray intensity BR Cir |with P = 16.595d accompanied with abrupt IR brightening. According BR Cir |to modern data, this period decreases. BU Cir |Multiperiodic. P2 = 0.142516d. BW Cir |X-ray outbursts in 1987 and 1997. BY Cir |Eclipses: P = 0.2816d [N0596]. BZ Cir |Porb = 0.079d. CC Cir |SB2. CL Cir |MinII - MinI = 0.43P. CQ Cir |Associated with a dark cloud. CX Cir |In the open cluster Pismis 20. VB A (8.3mV; B 10.6mV, 12.5", CX Cir |249{deg}, 2015; other components). DD Cir |Eclipses in 2002: Min = 2452426.2102 + 0.09746d x E, 19.80mV - DD Cir |20.90mV, D = 0.06P: [N0596]. DK Cir |MinII - MinI = 0.75P. DR Cir |VB A (12.9mG; B 14.9mG, 8", 42{deg}, 2000). DT Cir |VB A (13.2mG; B 15.2mG, 8", 102{deg}, 2000). DU Cir |VB A (13.1mG; B 13.5mG, 11", 41{deg}, 2016). DY Cir |VB A (15.4mG; B 15.9mG, 12", 70{deg}, 2000). EL Cir |VB B (A 11.5mG, B 13.3mG; AB 17", 299{deg}, 2000). FG Cir |VB A (12.5mG; B 13.7mG, 19", 339{deg}, 2000). FH Cir |Multiperiodic. P2 = 0.1260864. P2/P1 = 0.8279. FI Cir |VB (A 11.82mG, B 11.85mG; AB 2.3", 29{deg}, 2000; common proper FI Cir |motion). The Table presents the range for combined brightness. FP Cir |Multiperiodic. Fundamental mode: see Table. P1 = 0.0976718. P1/P0 = FP Cir |0.7706. alf Cir |Multiperiodic. P2 = 0.00474459d. gam Cir |VB (A 4.9mV, B 5.7mV, 0.8", 355{deg}, 2019). tet Cir |VB (5.9m, 5.9m, 0.1", 292{deg}, 2020). T Col |SiO maser. U Col |Min II 10.5. Y Col |V2 (NGC 1851). Z Col |V1 (NGC 1851). RS Col |Min II 9.97. dII = 0.021P. RY Col |(k - b)2 = 0.10. P var; nonlinear term: -3.38*10**(9)E**2. RZ Col |Min II 11.20. TV Col |2A 0526 - 328. VB A (B 15.79m, 10", 330{deg}). Epoch of Max of TV Col |short-term photometric variations is given. The following elements TV Col |describe, respectively, moments of Max Vr for Balmer lines and TV Col |moments of Max for the comparatively long-term photometric TV Col |variations which are due to the beat phenomenon for the photometric TV Col |and spectral periods: Max Vr = 2444227.631 + 0.228600d*E; Max = TV Col |2444191.5 + 4.024d*E. Flickering up to 0.15m B and flares up to TV Col |0.3m U are also observed [08960]. VW Col |Variability may be due to component B. AW Col |MinII - MinI = 0.79P. AY Col |Min II = 10.63. AZ Col |Min II = 11.65. P varies. dP/dt = -0.17x10^(-5) d/yr. BC Col |Min II = 13.5. BD Col |VB B (A = NSV 16739, 4.4m; AB 34", 110{deg}, 1999). BE Col |Min II = 11.55. BI Col |Type EW with a twice longer period is not excluded, having in mind BI Col |association with an X-ray source [81001]. BK Col |P varies strongly [80001]. BL Col |Blazhko effect, P = 40.5d. BQ Col |Blazhko effect, P = 15.33d? BW Col |Cluster non-member? CH Col |Blazhko effect? CM Col |Blended. CQ Col |Blended with a fainter companion. CV Col |Blazhko effect? CW Col |Blazhko effect? CY Col |Type RRC (RR1) with P about 0.333d is not excluded. DE Col |Blended. R Com |OH emission. S Com |{Delta}(S) = 8. T Com |OH, H2O emission. U Com |{Delta}(S) = 5. V Com |P var. Max = 2424518.219 + 0.46913844d*E (JD2420900 - 26900) V Com |[00218]; since JD2438100 - see Table. {Delta}(S) = 8. W Com |Radio source ON 231. X Com |Z = 0.092. Spectrum description [07415,08966]. Y Com |In the region of the globular cluster M 53 (NGC 5024). Z Com |In the region of the globular cluster M 53 (NGC 5024). RR Com |In the region of the globular cluster M 53 (NGC 5024). RS Com |In the region of the globular cluster NGC 5053. RT Com |In the region of the globular cluster NGC 5053. A var; P var. Max = RT Com |2423113.496 + 0.5651925d*E (JD2422700 - 26450) [00222]; since RT Com |JD2438535 - see Table. RU Com |In the region of the globular cluster M 53 (NGC 5024). RV Com |In the region of the globular cluster M 53 (NGC 5024). RW Com |In the region of the Comae Berenices cluster. dI = 0.04P; Min II RW Com |11.56. P var. Min I = 2433040.406 + 0.23734705d*E (JD2419680 - RW Com |34550) [00185]; since JD2439600 - see Table. RY Com |P var. Max = 2425007.450 + 0.46894835d*E (JD2425000 - 27500) RY Com |[03506]; Max = 2432674.390 + 0.4689397d*E (JD2432600 - 38110) RY Com |[03415]; since JD2438100 - see Table. (k - b)2 = 0.07. RZ Com |Possible member of the Comae Berenices cluster. Min II 11.09; dI = RZ Com |0.043P, dII = 0.039P. P var. Min I = 2433396.737 + 0.33850556d*E RZ Com |(JD2425000 - 33300) [00226]; since JD2433300 - see Table. Shape of RZ Com |the light curve varies. SS Com |Min II 11.9. ST Com |{Delta}(S) = 10. SX Com |In the region of the globular cluster NGC 4147. SZ Com |In the region of the globular cluster NGC 4147. TU Com |Shape of the light curve, A and P vary. Mean elements are given in TU Com |the Table. Possible period of Blazhko effect is 75d [03584]. [Fe/H] TU Com |= -1.43. UU Com |Member of the Comae Berenices cluster. Light variations are due to UU Com |rotation and pulsations of the star. Rotational period is 2.1953d UU Com |or 1.0256d or 0.9178d. Period of pulsations is 0.0227d (A ~0.01m). UU Com |According to [07985] there are two periods of pulsations: P1 = UU Com |0.0274d and P2 = 0.0209d (P2/P1 = 0.76). UV Com |[Fe/H] = -1.44. UW Com |[Fe/H] = -1.22. UX Com |Min II 10.13. P var; nonlinear term: -3.75d*10**(-8)*E**2. UY Com |[Fe/H] = -1.51. UZ Com |[Fe/H] = -1.44. VV Com |[Fe/H] = -1.53. VW Com |VB (12.00m, dM 3.5e; 12.3m, dM 4e, 3.0", 23{deg}, 1945). Range of VW Com |total brightness variation is given. According to [08363] the VW Com |component B is variable. However both components may be variables. VY Com |Min II 14.5. AI Com |Member of the Comae Berenices cluster. VB A (B 6.63m, 145", AI Com |251{deg}). Pulsations are possible: P = 0.052d (A = 0.02m) [08975]. AL Com |Within 8' to the south-east from the nucleus of M 88 (NGC 4501) AL Com |galaxy. AQ Com |Min II 15.7. BM Com |Min II 13.8. BS Com |P var. Max = 2434453.31 + 0.36341d*E (JD2434130 - 35230); since BS Com |JD2435590 - see Table. Shape of the light curve varies. BZ Com |[Fe/H] = -1.21. CC Com |In the region of the Comae Berenices cluster. Min II 12.09; dI = CC Com |0.03P. CD Com |[Fe/H] = -1.78. CF Com |Shape of the light curve varies. CG Com |[Fe/H] = -1.06. CI Com |RRC? CK Com |P var. Max = 2437370.71 + 0.6940159d*E (JD2437370 - 40130); Max = CK Com |2441630.35 + 0.6939080d*E (JD2440130 - 41630); since JD2441630 - CK Com |see Table. Blazhko effect. [Fe/H] = -1.68. CL Com |[Fe/H] = -1.00. CN Com |Min II 13.5. CP Com |[Fe/H] = -1.19. CT Com |In the region of the Comae Berenices cluster. CV Com |In the region of the Comae Berenices cluster. CX Com |In the region of the Comae Berenices cluster. Not member of the CX Com |cluster. DD Com |Min II 14.90. DG Com |Min II 14.6. DL Com |P var? DR Com |EW? P = 0.45184d? DS Com |[Fe/H] = -1.32. DT Com |[Fe/H] = -1.60. DU Com |[Fe/H] = -1.45. DV Com |[Fe/H] = -1.57. DW Com |[Fe/H] = -1.53. EE Com |P = 0.539533d also satisfies observations. [Fe/H] = -1.64. EF Com |[Fe/H] = -1.90. EG Com |[Fe/H] = -1.29. EI Com |[Fe/H] = -1.68. EL Com |P = 0.52362d also satisfies observations. EM Com |[Fe/H] = -1.64. EN Com |[Fe/H] = -1.19. EO Com |[Fe/H] = -1.51. EP Com |[Fe/H] = -0.98. EQ Com |Min II 15.3. ER Com |[Fe/H] = -1.51. ES Com |[Fe/H] = -2.02. EW Com |[Fe/H] = -1.77. EX Com |P = 0.558359d? [Fe/H] = -1.48. EY Com |Min II 18.0. EZ Com |P = 0.568349d? [Fe/H] = -1.16. FG Com |P = 0.3098d also satisfies observations. FK Com |Wide emission lines, H{alpha} and H, K CaII, of variable intensity. FK Com |Epoch of light minimum is given. FM Com |The member of the Comae Berenices cluster. Multiperiodicity. Cycle FM Com |of 0.0713d was observed also [08989]. FO Com |In the region of the Comae Berenices cluster. FP Com |In the region of the Comae Berenices cluster. {mu} = 0.23", P = FP Com |158{deg}. Red. FZ Com |P = 4.704864d? GM Com |In the region of the Comae Berenices cluster. GN Com |Member of the Comae Berenices cluster. P > 1d. GO Com |In the region of the Comae Berenices cluster. GP Com |{mu} = 0.38", p = 286{deg}. SB (Porb = 0.032306d). Unique object G GP Com |61-29. Consists of two interacting white dwarfs. The lower mass GP Com |star, a helium white dwarf, transfers mass to the higher mass star GP Com |surrounded by an accretion disk. Usually flares are being observed GP Com |with an amplitude about 0.2m V, 0.5m U lasting about 20 seconds GP Com |[07417,08991]. Sometimes periods of photometric activity arise when GP Com |amplitude of light variations reaches 0.6m V and sharp passages GP Com |from maxima to minima are being observed; the duration of these GP Com |minima reaches up to 0.14d [07417]. When the star is most active, GP Com |periodic light oscillations appear with P = 105 seconds and GP Com |amplitude 0.05m - 0.10m V [07062]. GQ Com |Z = 0.165. Emission H, [OIII]. Irregular light variations. B - V = GQ Com |+0.16. GT Com |Minor planet (679) Pax. HH Com |Epoch of Min in V system is given. HI Com |In the region of the Comae Berenices cluster. HK Com |In the region of the Comae Berenices cluster. HM Com |In the region of the Comae Berenices cluster. HN Com |In the region of the Comae Berenices cluster. HO Com |In the region of the Comae Berenices cluster. HP Com |In the region of the Comae Berenices cluster. HQ Com |In the region of the Comae Berenices cluster. HR Com |In the region of the Comae Berenices cluster. HS Com |In the region of the Comae Berenices cluster. HT Com |In the region of the Comae Berenices cluster. HU Com |In the region of the Comae Berenices cluster. HV Com |In the region of the Comae Berenices cluster. HW Com |In the region of the Comae Berenices cluster. MM Com |MinII 12.80. MN Com |Variable brown dwarf. MR Com |MinII 12.43. MT Com |Small-amplitude pulsations with characteristic periods 1344, 1236, MT Com |668 seconds. MW Com |Min II = 10.5. MX Com |Min II = 11.94. MZ Com |Min II = 10.2 :. NN Com |Min II = 12.67. NS Com |Min II = 13.5. NV Com |Min II = 12.15. NW Com |Multiperiodic, with several periods in the DSCTC range (one of them NW Com |tabulated) and several GDOR periods (P = 0.42779d and others). OP Com |Multiperiodic? Blazhko effect? OR Com |P varies [80001]. Blazhko effect? [80026]. OW Com |Min II = 16.3. OX Com |Min II = 16.1 :. QQ Com |P strongly varies. QU Com |P1 is presented in the Table. P0 = 0.541781d; P1/P0 = 0.7456. QW Com |P1 is presented in the Table. P0 = 0.547401d; P1/P0 = 0.7455. QX Com |P1 is presented in the Table. P0 = 0.544233d; P1/P0 = 0.7454. QY Com |P1 is presented in the Table. P0 = 0.490349d; P1/P0 = 0.7446. QZ Com |Additional non-radial mode, P = 0.2687276d; P(Blazhko) = 13.7d. V0335 Com |P1 is presented in the Table. P0 = 0.515253d; P1/P0 = 0.7460. V0336 Com |P1 is presented in the Table. P0 = 0.480562d; P1/P0 = 0.7439. V0337 Com |P1 is presented in the Table. P0 = 0.478242d; P1/P0 = 0.7439. V0338 Com |P1 is presented in the Table. P0 = 0.485204d; P1/P0 = 0.7440. V0340 Com |P1 is presented in the Table. P0 = 0.460448d; P1/P0 = 0.7425. V0341 Com |P1 is presented in the Table. P0 = 0.476173d; P1/P0 = 0.7443. V0342 Com |P1 is presented in the Table. P0 = 0.488314d; P1/P0 = 0.7447. V0343 Com |P1 is presented in the Table. P0 = 0.486854d; P1/P0 = 0.7443. V0344 Com |Blazhko effect. V0347 Com |Blazhko effect. V0350 Com |The number V020 is from [g1086], the star was not in the Catalog of V0350 Com |Variable Stars in Galactic Glogular Clusters, version September, V0350 Com |2018. The coordinates in [g1018] are wrong. V0351 Com |The light curve shape varies. V0356 Com |P varies? V0357 Com |The light curve shape varies. V0358 Com |Blazhko effect, P = 67.46d. V0360 Com |P varies? V0369 Com |VB B (A 14.1mG, B 16.8mG; AB 4", 343{deg}, 2000). V0371 Com |Blazhko effect. V0375 Com |Blazhko effect. V0376 Com |VB B (A 16.2mG, B 16.7mG; AB 2", 122{deg}, 2000). V0377 Com |Blazhko effect? V0378 Com |Multiperiodic. V0383 Com |Crowded. V0385 Com |VB B (A 17.2mG, B 18.2mG; AB 1.5", 58{deg}, 2000). V0387 Com |Blazhko effect. V0388 Com |Crowded. V0391 Com |The light curve shape varies? V0393 Com |Blend. V0394 Com |Multiperiodic. V0395 Com |Multiperiodic. Blend. V0397 Com |Multiperiodic. V0400 Com |Multiperiodic. V0402 Com |Blended. VB A (A 15.4mG, blend; B 15.8mG, 2", 0{deg}, 2000). V0403 Com |VB B (A 15.9mG, B 16.7mG; AB 1.4", 257{deg}, 2000). V0404 Com |Blend. Blazhko effect? V0406 Com |Multiperiodic. VB B (A 17.2 mG, B 18.3mG; AB 1.3", 227{deg}, 2000; V0406 Com |other companions). V0407 Com |VB B (A 16.5mG, B 16.9mG; AB 2", 74{deg}, 2000). V0408 Com |VB B (A 13.9mG, B 16.4mG; AB 1.5", 310{deg}, 2000). V0410 Com |Blended. Blazhko effect. V0411 Com |VB A (16.7mG; B 17.0mG, 1.4", 162{deg}, 2000). V0412 Com |NGC 5024 V052 (V0414 Com) np. V0414 Com |Blazhko effect. NGC 5024 V053 (V0412 Com) sp. V0416 Com |Blended. The light curve shape varies. V0418 Com |VB B (A 16.9mG, B 18.2mG; AB 1.1", 240{deg}, 2000). Photometry was V0418 Com |possibly contaminated with the neighbor. V0421 Com |VB A (16.9mG; B 17.1mG, 2", 49{deg}, 2000). Blazhko effect. V0422 Com |VB B (A 15.9mG, G 16.4mG; AB 1.4", 38{deg}, 2015.5). V0424 Com |VB B (A 15.1mG, B 16.7mG; AB 2", 38{deg}, 2000). V0425 Com |VB B (A 17.7mG, B 19.4mG; AB 1.6", 140{deg}, 2000). V0426 Com |VB B (A 17.5mG, B 19.2mG; AB 1", 192{deg}, 2000). V0428 Com |VB A (19.5mG; B 19.7mG, 2.5", 306{deg}, 2000). V0436 Com |VB B (A 19.3mG, B 19.6mG; AB 2", 214{deg}, 2000). V0438 Com |P varies? V0439 Com |Blazhko effect. V0453 Com |VB A (19.3mG; B 19.7mG, 4", 87{deg}, 2000). V0454 Com |P varies? V0459 Com |The GCVS name for this star is out of order for its cluster because V0459 Com |of a typo in right ascension. V0460 Com |P varies? V0465 Com |P varies, dP/dt = -0.28: x 10^(-6) d per year. V0466 Com |P varies. V0467 Com |P varies. V0468 Com |P varies, dP/dt = +0.17 x 10^(-6) d per year. The Table presents V0468 Com |linear light elements. VB A (16.6mG; B 16.7mG, 3", 178{deg}, 2000). V0469 Com |P = 0.03945d is also possible. V0471 Com |P varies, dP/dt = +0.48 x 10^(-6) d per year. In 1997 - 2002, P = V0471 Com |0.362868d. V0472 Com |P varies, dP/dt = -0.32 x 10^(-6) d per year. V0473 Com |P varies? dP/dt = +0.09 x 10^(-6) d per year. The Table presents V0473 Com |linear light elements. V0474 Com |P varies, dP/dt = +0.18 x 10^(-6) d per year. The Table presents V0474 Com |linear light elements. R CrA |In the head of the bright cometary nebula NGC 6729. IR excess. S CrA |VB A (B 13.5m, 1", 137{deg}). IR excess. T CrA |In the bright cometary nebula NGC 6729. IR excess. V CrA |Quasiperiodic variations (P ~75d, {Delta}(V) ~ 0.2m - 0.9m). IR V CrA |excess. RS CrA |sp of two close stars; each of them or both may be identified with RS CrA |CoD -39{deg} 13082. RW CrA |Min II 9.4. SS CrA |V1 (NGC 6541). SV CrA |The period may be twice shorter. TY CrA |VB A (B 13.3m, 4", 138{deg}; C 58", 24{deg}). In the bright nebula TY CrA |NGC 6726/27. P = 1.92d is not excluded, in that case Min II = Min TY CrA |I. On the basis of visual observations 8.7 - 12.4 v (presumably TY CrA |"spurious variability" due to the difficulties of estimates over TY CrA |the bright background of the nebula), and the star was classified TY CrA |as INSA. TZ CrA |Min II 9.72. UU CrA |Min II 11.0. UX CrA |The period may be twice shorter. UY CrA |P var? VV CrA |In the region of the bright nebula NGC 6729. IR excess. WY CrA |Apparently, variability announced in [00249] was due to WY CrA |misidentification of a high-proper-motion star. AF CrA |P var. Before JD2418060 Max = 2413710 + 483d*E; since JD2418060 - AF CrA |see Table. AL CrA |B - V: +0.65, +1.30. [A/H] = -0.2. AN CrA |P var. Nonlinear term: -0.006d*10**(-6)*E**2. AU CrA |P var. Nonlinear term: -0.026d*10**(-6)*E**2. AY CrA |Min II 15.2. BG CrA |Min II 15.1. BH CrA |P var. Nonlinear term: -0.023d*10**(-6)*E**2. CM CrA |P var. Nonlinear term: -0.007d*10**(-6)*E**2. CR CrA |Min II 15.7. CS CrA |Min II 15.2. CY CrA |P var. Nonlinear term: -0.002d*10**(-6)*E**2. DG CrA |In the region of the bright nebula NGC 6729. IR excess. DL CrA |Min II 13.6. DN CrA |P var. Nonlinear term: +0.006d*10**(-6)*E**2. DZ CrA |d = 0.02P. EE CrA |mpg var, 13.5m - 15.5m, P2 = 3000d - 5000d {Delta}(m) (P1 = 167d) EE CrA |~1.5m. EK CrA |P var. Before JD2422600 Max = 2411870 + 421d*E. FF CrA |Before JD2423000 Max = 2411530 + 140.2d*E. FK CrA |Min II 14.5. FS CrA |Min II 14.5. FW CrA |Before JD2416600 Max = 2411190 + 112.2d*E. GS CrA |Before JD2422600 Max = 2414070 + 284d*E. IT CrA |Min II 13.6. KM CrA |The chart in [06286] is wrong. KQ CrA |[A/H] = -0.7. B - V: +0.76, +1.23. KT CrA |Red. LU CrA |P = 182d is possible. MS CrA |Yellow. MT CrA |Min II 13.1. NO CrA |Reddish. QR CrA |Reddish. V0347 CrA |B - V: +0.82, +1.17. V0350 CrA |Min II 13.4. V0385 CrA |The period may be spurious. V0413 CrA |(k - b)2 = 0.11. V0428 CrA |The period may be twice shorter. V0449 CrA |[A/H] = -0.3. V0454 CrA |Min II 10.5. V0455 CrA |d = 0.05P. Min II 13.7. V0457 CrA |Epoch of Min is given. EW type is also possible, in that case the V0457 CrA |value of P should be doubled. V0465 CrA |Min II 14.2. V0467 CrA |P var? V0471 CrA |Min II 13.3. V0478 CrA |Sometimes a cycle 60d - 70d. V0480 CrA |Min II 13.9. V0490 CrA |P var? The elements represent the observations of 1944. V0493 CrA |P var? V0501 CrA |Min II 13.4. Twice shorter period is possible. V0503 CrA |d = 0.03P. V0511 CrA |Twice longer period is possible. V0512 CrA |P var? V0513 CrA |Min II 13.2. V0514 CrA |Min II 14.0. V0527 CrA |P var. V0535 CrA |P var. V0541 CrA |P var? V0545 CrA |VB. Combined brightness with a faint companion is given. V0553 CrA |P var? V0566 CrA |Min II 12.7. V0568 CrA |Sometimes a cycle 60d - 80d. V0569 CrA |Min II 13.1. EB type is possible. V0571 CrA |Min II 14.7. V0572 CrA |Min II 14.0. V0577 CrA |Min II 13.2. RR type with twice shorter period is possible. V0578 CrA |RV type with P = 118d is possible. V0580 CrA |Min II 14.4. V0595 CrA |P var. V0601 CrA |Epoch of min is given. V0603 CrA |Slightly noticeable Min II at the phase 0.5P. V0604 CrA |d = 0.03P. V0607 CrA |Min II 14.3. V0612 CrA |d = 0.03P. V0615 CrA |P var? V0622 CrA |Sometimes 55d - 60d cycles. V0633 CrA |P var. V0634 CrA |Min II 13.9. V0648 CrA |Min II is felt at the phase 0.5P. V0659 CrA |P = 189.4d is possible. V0667 CrA |In the region of the bright cometary nebula NGC 6729. The spectral V0667 CrA |type is earlier than K. V0676 CrA |RR type is possible. V0686 CrA |Max I 5.34, Min I 5.41, Max II 5.35, Min II 5.40 [08970]. V0691 CrA |4U 1822-37. Emissions CIII/NIII {lambda} 4640 - 50, He II {lambda} V0691 CrA |4686, CIV {lambda} 1550 etc. V0692 CrA |P = 0.83d is possible. V0730 CrA |MinII 9.99 [78011]. Type RRC with a twice shorter period is V0730 CrA |possible. V0731 CrA |Large scatter on the light curve. V0737 CrA |Multiperiodic, P2 = 0.156795d. V0738 CrA |Globular cluster non-member? V0739 CrA |Globular cluster non-member? V0740 CrA |Globular cluster non-member? V0741 CrA |P = 0.394d is also possible. Globular cluster non-member? V0742 CrA |Globular cluster non-member? V0743 CrA |Globular cluster non-member? V0745 CrA |Globular cluster non-member? V0756 CrA |Double-mode. P0 is given in the Table; P1 = 0.0821611d, P1/P0 = V0756 CrA |0.7665. V0778 CrA |P = 95d is superposed. V0782 CrA |VB B (A 14.0mV; AB 20", 355{deg}, 1991). The magnitude in maximum V0782 CrA |can be influenced by the companion. V0795 CrA |Blazhko effect? V0798 CrA |VB A (15.0mG; B 15.3mG, 7", 72{deg}, 2000); the range in the Table V0798 CrA |can be influenced by the companion. V0799 CrA |Blazhko effect? P varies? V0800 CrA |Blazhko effect? P varies? V0808 CrA |VB A (13.5mG; B 14.3mG, 12", 266{deg}, 2000); the range in the V0808 CrA |Table can be influenced by the companion. V0818 CrA |Cluster non-member. VB B (A 15.7mG, B 16.8mG; AB 4", 236{deg}, V0818 CrA |2000). V0819 CrA |Cluster non-member. V0820 CrA |Cluster non-member. V0822 CrA |Cluster non-member? V0834 CrA |Cluster non-member. V0835 CrA |Cluster non-member. eps CrA |Min II 4.95. R CrB |IR excess. S CrB |OH, H2O, SiO maser. T CrB |VB? A (B <= 12m, 0.2"). SB (P = 227.6d). The spectral period is T CrB |present in the photometric data of 1891 - 1917 and 1960 - 1971 T CrB |[08978]. The epoch of the first outburst JD2402734 (1866). Two T CrB |smaller outbursts were observed in UV light, JD2438030 (1963) and T CrB |2442543 (1975) [08979]. U CrB |Min II 7.72. P var. RR CrB |P2 = 377d. {Delta}(m) (P1) ~0.5m, {Delta}(m) (P2) ~0.6m. RS CrB |P2 = 69.5d [01100]. Main period oscillation: 9.1m - 11.6m. RT CrB |Nonlinear term: +2.01d*10**(-8)*E**2. Min II 10.52 (var). DII = RT CrB |0.09P. RV CrB |P var. Max = 2428285.608 + 0.3316217d*E (JD2428285 - 31610); Max = RV CrB |2431705.349 + 0.3317313d*E (JD2431705 - 32954); Max = 2433030.572 + RV CrB |0.331705d*E (JD2433030 - 36814) [05496]; Max = 2440001.453 + RV CrB |0.331569d*E (1967 - 1971) [06237]; Max = 2441451.413 + 0.331619d*E RV CrB |(1972 - 1974) [07032]. The Table gives current elements. On the RV CrB |period changes see also [03506]. Blazhko effect? RW CrB |d = 0.028P. Min II 10.29. TW CrB |Min II 11.0. TZ CrB |ADS 9979 A (B 6.72m, GIV, 6.6", 233{deg}, 1980). SB2 (P = TZ CrB |1.139789d). Epoch of Min is given. The variation presented in the TZ CrB |Table is superimposed by a second one, with the same amplitude and TZ CrB |P = 0.1d. The amplitude is given for the combined light of ADS 9979 TZ CrB |A and B, the mean magnitude is for ADS 9979 A. UU CrB |During JD2444381.73 - .76 a slow flare was observed, with maximal UU CrB |amplitude 0.30m in the IK band and 0.18m in the U band. AL CrB |Spotted rotating G-type giant. AR CrB |MinII 11.44. AS CrB |MinII 11.75. AV CrB |MinII 12.41. AW CrB |According to [78161], EW, P = 0.360920 d. AY CrB |Min II = 14.0. BD CrB |Min II = 14.6. BG CrB |VB AB (9.5m, 9.8m, 0.1", 192{deg}, 2007). BR CrB |Min II = 10.11. CT CrB |Strong Blazhko effect. CZ CrB |P strongly varies. DE CrB |P1 is presented in the Table. P0 = 0.554870d; P1/P0 = 0.7460. DG CrB |P1 is presented in the Table. P0 = 0.539078d; P1/P0 = 0.7456. DH CrB |P1 is presented in the Table. P0 = 0.551550d; P1/P0 = 0.7464. DI CrB |P1 is presented in the Table. P0 = 0.508196d; P1/P0 = 0.7452. DK CrB |MinII - MinI = 0.482P. DL CrB |Time-variable O'Connell effect. alf CrB |{lambda} eff = 7230 A: DI = 0.034P, DII = 0.018P, Min II - Min I = alf CrB |0.66P, depth of Min I 0.10m, Min II 0.025m. bet CrB |VB A (B ~ 5m - 6m, 0.2", ~130{deg}, 1978). SB (P = 3833.7d). bet CrB |Magnetic field var, P = 18.487d. The epoch of Min light is given. gam CrB |ADS 9757 (4.2m, 5.6m; A = 0.74", P = 91.0a). U Crv |VB A (B 13.5m, 0.4' p). W Crv |Min II 11.86. The light curve is asymmetrical, the maxima differ in W Crv |hight by 0.10m. Y Crv |Min II 11.7. RRC type with twice shorter period is possible. Z Crv |d = 0.06P. RV Crv |Elements do not satisfy some of the published moments of Min. RZ Crv |Min II 13.9. SX Crv |Min II 9.23. The shape of the light curve varies. Depth of Min I SX Crv |0.20m, depth of Min II 0.18m. In 1972 the system became fainter SX Crv |than in 1971 by 0.06m. TY Crv |SB2. XX Crv |P1 is tabulated; P0 = 0.54452d. XY Crv |P1 is tabulated (amplitude 0.44m); P0 = 0.484820d (amplitude XY Crv |0.28m). YZ Crv |VB B (A 16.2mpg, B 16.2mpg; AB 27", 192{deg}, 2000). The YZ Crv |coordinates in [81005] refer to the A component. AA Crv |VB B (A 12.7mpg, B 15.9mpg; AB 28", 220{deg}, 1998). The AA Crv |coordinates in [81005] refer to the brighter star. AD Crv |Additional non-radial mode, P = 0.2691307d; P(Blazhko) = 185d. AG Crv |P1 is presented in the Table. P0 = 0.537739d; P1/P0 = 0.7465. AH Crv |P1 is presented in the Table. P0 = 0.488888d; P1/P0 = 0.7450. R Crt |Periods of light constancy which last up to 250d occur every two or R Crt |there thousand days. OH, H2O maser. S Crt |H2O maser. T Crt |Mean light var, P2 = 1006d. V Crt |Min II 10.1; Min II - Min I = 0.57P. W Crt |(k - b)2 = +0.21. X Crt |(k - b)2 = +0.02. Z Crt |d = 0.016P. RR Crt |P = 293d or 146d is possible. RV Crt |Min II 9.4:. SU Crt |[Fe/H] > -0.3. SV Crt |ADS 8115 A (B 11.5m vis, 1", 220{deg}). SB2 (P = 5.90513d, apsidal SV Crt |motion, P ~700a). Epoch of Min I in B light is given. Depth of Min SV Crt |II is 0.015m. EuII and SrII in emission. AG Crt |P varies. AI Crt |Blazhko effect, P=63d. The identification with NSV 5200 suggested AI Crt |in [80153] is probably wrong. AK Crt |Min II = 11.15. The tabulated elements are for the eclipses. AK Crt |Pulsations: P = 0.067964d, with a variable amplitude up to 0.07m. AV Crt |A period about 3497d is possibly superposed. AX Crt |P1 is presented in the Table. P0 = 0.521023d; P1/P0 = 0.7454. AY Crt |P1 is presented in the Table. P0 = 0.483101d; P1/P0 = 0.7446. R Cru |In the region of the open cluster NGC 4349. T Cru |In the region of the open cluster NGC 4349. U Cru |P var. Max = 2410143 + 351.4d*E (JD2410100 - 14100) [00237]; since U Cru |JD2437600 - see Table. W Cru |Min II 9.3. SU Cru |[A/H] = -0.8. SV Cru |In the region of the open cluster Ruprecht 97. Non-member of the SV Cru |cluster. SW Cru |VB A (B 14.0m, 12"). (k - b)2 = 0.27. SY Cru |d = 0.05P? TU Cru |Min II 11.5. TW Cru |Min II 12.85:. TX Cru |It is not excluded that actually P is much shorter, close to 1d, TX Cru |for instance. TZ Cru |P = 2.091140d? UW Cru |Min II 12.9; Min II - Min I = 0.536P. UX Cru |VB A (B 10"). Min II 12.4; Min I - Min II = 0.325P; DII = 0.025P. VY Cru |Min II 13.5. VZ Cru |P = 1.125810d? WW Cru |Min II 13.0. WX Cru |d = 0.040P. Light variability in maximum is noted. WY Cru |VB A. P = 9.013290d? XX Cru |P = 3.28566d? XY Cru |Min II 11.7. XZ Cru |P = 1.6495930d? YY Cru |Min II 13.0. YZ Cru |Min II 13.1. ZZ Cru |Min II 9.8. AB Cru |Min II 8.9. AC Cru |Min II 12.1. AD Cru |VB A (B 14.5m, 10", 270{deg}). P var. Max = 2434918.160 + AD Cru |6.39844d*E (JD2423800 - 35400) [02309]; since JD2441000 - see AD Cru |Table. AE Cru |Depth of Min II 0.03m. AF Cru |Min II 9.87. AG Cru |The blue component is possible [09004]. AI Cru |In the region of the open cluster NGC 4103. Min II 9.94. AQ Cru |Min II 13.8. AT Cru |Min II 12.6. AW Cru |Min II 13.9. AY Cru |Min II 11.2. BB Cru |Min II 14.0. BC Cru |Depth of Min II 0.03m. BD Cru |Depth of Min II 0.05m. BF Cru |Min II 12.3. BH Cru |Epoch of Min I is given in the Table. The light curve like the BH Cru |light curves of R Cen and R Nor has two maxima and two minima of BH Cru |different depths. Max I 7.6m (0.22P), Min II 8.0m (0.41P), Max II BH Cru |7.2m (0.53P). BI Cru |Spectrum description [04949]. BK Cru |In Coalsack region. BM Cru |In Coalsack region. BP Cru |3U 1223-62. A unique X-system. Consists of an X-pulsar with pulse BP Cru |period 698s [09018] moving on an excentric orbit (E = 0.47) around BP Cru |the ellipsoidal B2 supergiant with orbital period of 41.51d. BP Cru |Accretion of the stellar wind from the primary star on the pulsar BP Cru |increases during the periastron passage. Therefore large X-flares BP Cru |are observed with the elements: T (X Max) = 2433158.09 + 41.51d*E. BP Cru |Optical flares are possible. BQ Cru |B - V: +1.13, +0.88. BS Cru |In the open cluster NGC 4755. BT Cru |In the open cluster NGC 4755. BU Cru |In the open cluster NGC 4755. BV Cru |In the open cluster NGC 4755. BW Cru |In the open cluster NGC 4755. DU Cru |The identification with NSV 06012 (SIMBAD) is wrong. EP Cru |MinII - MinI = 0.62P. EQ Cru |MinII - MinI = 0.48P. EW Cru |A twice longer period is also possible. FG Cru |Multiperiodic. FL Cru |Multiperiodic. bet Cru |VB A (B 11.4m, 44.3", 322{deg}; C 7.5m, 372", 23{deg}). bet Cru |Interferometric binary. Multiple periods (the total V amplitudes of bet Cru |corresponding oscillations are indicated in brackets): P0 = bet Cru |0.2365072d (0.034m), P1 = 0.160466d (0.029m), P2 = 0.121383d bet Cru |(0.01m), P02 = 0.249373d (0.016m), P13 = 0.24273d (0.024m), P24 = bet Cru |0.23931d (0.028m), P03 = 0.16342d (0.016m), P14 = 0.16171d bet Cru |(0.029m). tet 2 Cru |SB (P = 3.4380d). BCEPS, P > 1h? [08420]. lam Cru |Type ELL with P = 0.7902d is possible. Amplitude and shape of the lam Cru |light curve vary. The secondary oscillation (A = 0.007m) with the lam Cru |elements Max = 2441779.034 + 0.1793d*E is possible. R Cyg |VB A (B 9.3m, 91", 14{deg}). S4/6e - S8/6e. T Cyg |VB A (B 10.03m, 10.2", 122{deg}; C 12m, 13.6", 197{deg}). U Cyg |VB A (B 7.8m, 63.5", 51{deg}). P var. Max = 2406455 + 461.57d*E U Cyg |(JD2404590 - 13900); Max = 2414827 + 470.76d*E (JD2413900 - 19940); U Cyg |Max = 2421806 + 455.95d*E (JD2419940 - 27380); Max = 2427848 + U Cyg |472.85d*E (JD2427380 - 35750); since JD2435750 - see Table. W Cyg |There is a second oscillation with P = 235.3d. X Cyg |P var. Max = 2410190.86 + 16.3841d*E (JD2410100 - 23370) [09028]; X Cyg |since JD2417000 - see Table. There is a square term in the elements X Cyg |given in the Table: +1.01d*10**(-7)*E**2. [A/H] = 0.4. Y Cyg |Min II 7.75; E = 0.1458. Apsidal motion: P = 47.6 yr. There are Y Cyg |sinusoidal terms in the elements: +0.1391d*sin(0.06256{deg}*E) - Y Cyg |0.0076d*sin(2*(0.06256{deg}*E)); Min II = 2409454.9174 + Y Cyg |2.9963328d*E - 0.1391d*sin(0.06256{deg}*E) - Y Cyg |0.0076d*sin(2*(0.06256{deg}*E)). Z Cyg |OH, H2O emission. RR Cyg |VB A (B 12.5m, 18.1", 58{deg}). RS Cyg |VB A (B 7.09m, 132", 355{deg}; C 9.3m, 56", 106{deg}). Epoch of RS Cyg |light minimum is given. The shape of the light curve strongly RS Cyg |varies. Double maxima are sometimes observed (Min II at the phase RS Cyg |0.5P). RU Cyg |VB A (B 12.40m V, 10", 224{deg}; C 11.15m V, 19", 29{deg}). RV Cyg |VB A (B 10m, 142", 118{deg}). RY Cyg |In the region of the open cluster NGC 6883. RZ Cyg |The shape of the light curve strongly varies. Alternation of high RZ Cyg |and low maxima, as well as of shallow and deep minima is observed, RZ Cyg |as a rule: 9.8m <= Max <= 12.0m. 11.8m <= Min <= 14.1m. SS Cyg |SB2 (P = 0.27512995d [08285]). During maxima of brightness there SS Cyg |are oscillations of light and X-ray flux with amplitudes about SS Cyg |0.002m V and periods changing between 7.29s and 10.90s [06102, SS Cyg |09032]. SU Cyg |P var. Max = 2421278.503 + 3.845507d*E (JD2414250 - 29000) [01559]; SU Cyg |Max = 2433095.944 + 3.845664d*E (JD2429000 - 33150) [00921]; since SU Cyg |JD2434500 - see Table. SV Cyg |VB A (B 9.5m V, 145", 140{deg}). SW Cyg |Min II 9.30; d(V) = 0.018P; d(U) = 0.00P. P var. Min I = SW Cyg |2414782.448 + 4.572937d*E (JD2411340 - 16450); Min I = 2418440.758 SW Cyg |+ 4.5727923d*E (JD2417060 - 19740) [00063]; Min I = 2421504.489 + SW Cyg |4.572729d*E (JD2421470 - 24970); Min I = 2425185.550 + 4.5728386d*E SW Cyg |(JD2424960 - 29500); Min I = 2433160.669 + 4.5729841d*E (JD2433000 SW Cyg |- 36800) [09085]; Min I = 2438584.3081 + 4.57311736d*E (JD2438600 - SW Cyg |40560) [09085]; since JD2441160 - see Table. SY Cyg |d = 0.040P. Possible depth of Min II 0.03m. P var. Min I = SY Cyg |2411659.568 + 6.00584d*E (JD2411600 - 17100); Min I = 2420001.571 + SY Cyg |6.005716d*E (JD2418760 - 20760) [01961]; Min I = 2437069.254 + SY Cyg |6.005626d*E (JD2432800 - 37070) [05416]. Mean elements given in the SY Cyg |Table represent epochs of Min I in the interval JD2414400 - 37070 SY Cyg |up to +- 0.07d. According to [04248] the apsidal motion with the SY Cyg |period ~46 years is possible. SZ Cyg |[A/H] = 0.5. P var [02392]. Mean elements given in the Table SZ Cyg |represent epochs of Max up to +- 0.5d. According to [09029] "the O SZ Cyg |- C diagram has a sinusoidal structure as is to be expected for a SZ Cyg |member of a binary system" with P orb = 65 years. TT Cyg |VB A (B 10.8m V, 70", 213{deg}; C 11.1m V, 83", 49{deg}; D 10.7m V, TT Cyg |94", 268{deg}). TV Cyg |According to [03663] - spectrum G0. TX Cyg |[A/H] = -0.2. P var. Max = 2436793.138 + 14.708157d*E (JD2415000 - TX Cyg |37000); since JD2436700 - see Table. UU Cyg |VB A (B 10.7m V, 3.6", 351{deg}). UV Cyg |VB A (B 10.8m V, 0.9", 79{deg}). UW Cyg |P var. Min I = 2419624.501 + 3.450797d*E (JD2410000 - 20750) UW Cyg |[00526]; Min I = 2419624.501 + 3.450752d*E (JD2419620 - 33000); Min UW Cyg |I = 2433848.508 + 3.450740d*E (JD2430000 - 41800); since JD2441800 UW Cyg |- see Table. Possible depth of Min II 0.05m. UX Cyg |P var. Max = 2432444 + 560.3d*E (JD2415670 - 32450); Max = 2439352 UX Cyg |+ 578.0d*E (JD2432450 - 40500); since JD2437600 - see Table. UX Cyg |Sometimes rapid light decreases on the ascending branch near Max UX Cyg |are observed [01563,01564]. H2O, OH, SiO maser. UY Cyg |{Delta}(S) = 3.8. UZ Cyg |VB A (B 10.8m, 28", 130{deg}). d = 0.032P; Min II 10.31. VV Cyg |Min II 13.2. P var? [03665]. VW Cyg |d = 0.035P; Min II 10.31. P var. Min I = 2417377.123 + 8.4305260d*E VW Cyg |(JD2415660 - 17400); Min I = 2430444.061 + 8.4302826d*E (JD2417400 VW Cyg |- 30450); Min I = 2441116.868 + 8.4303917d*E + 4.31d*10**(-8)*E**2 VW Cyg |(JD2430450 - 41120) [07096]; since JD2440350 - see Table. VX Cyg |[A/H] = 0.2. P var. There is a square term in the elemenmts VX Cyg |+8.02d*10**(-7)*E**2. VZ Cyg |P var. Max = 2437103.945 + 4.8645598d*E(JD2416000 - 41000); since VZ Cyg |JD2434000 - see Table. WW Cyg |d = 0.008P; Min II 10.16. P var [06144]. Mean elements: Min I = WW Cyg |2416981.299 + 3.3176924d*E (JD2412000 - 31000) [00063]; since WW Cyg |JD2431000 - see Table. WZ Cyg |Min II 10.9. XX Cyg |[Fe/H] = -0.49. P var. Max = 2430671.1010 + 0.134865026*E(2416560 - XX Cyg |30000); since JD2430000 - see Table. XZ Cyg |[Fe/H] = -1.2. P var. Max = 2417201.241 + 0.4665878*E - XZ Cyg |0.000107d*10**(-6)*E**2 (JD2414000 - 35000) [02550]; Max = XZ Cyg |2438562.796 + 0.466570d*E (JD2434000 - 39800); Max = 2440445.789 + XZ Cyg |0.466497d*E (JD2439800 - 41000) [06237]; Max = 2441453.3856 + XZ Cyg |0.4664731d*E (JD2441000 - 42500) [07424]; Max = 2443028.641 + XZ Cyg |0.466438d*E (JD2442500 - 43800) [09101]; Max = 2444142.650 + XZ Cyg |0.466649d*E (JD2443800 - 44200) [09102]; since JD2444100 - see XZ Cyg |Table. Besides that the star has a strongly expressed Blazhko XZ Cyg |effect; the period of Blazhko effect varies, too [07424,07425]. XZ Cyg |0.13P <= M - m <= 0.22P; 0.90m <= A(B) <= 1.70m, 0.70m <= A(B) <= XZ Cyg |1.30m; -0.05P < O - C < +0.05; Max A = 2417025.5 + 57.401d*E XZ Cyg |(JD2417000 - 38500); Max A = 2438881.7 + 58.387d*E (since XZ Cyg |JD2438500).[09103]. After JD2444000 Blazhko effect period probably XZ Cyg |decreased to 56.3d [09102]. ZZ Cyg |VB A (B 12.63m, 8.5", 43{deg}. Total brightness variation range is ZZ Cyg |given. Min II 10.78. P var. Min I = 2417442.419 + 0.6286185d*E ZZ Cyg |(JD2415000 - 25800) [07427]; since JD2427950 - see Table. AA Cyg |S 6/3. AC Cyg |H2O maser. AD Cyg |S 5/5. AE Cyg |d = 0.039P; Depth of Min II 0.06m. AF Cyg |Light curve (1914 - 1956) [09104]. Two more independent AF Cyg |oscillations are superimposed: P2 = 175.8d, P3 = 941.2d. AK Cyg |VB A (B 11.06m, A7, 20", 85{deg}). AV Cyg |P var. Max = 2420451.9 + 87.48d*E (JD2418782 - 24823); Max = AV Cyg |2427936.3 + 89.73d*E (JD2426326 - 28745); Max = 2429440.9 + AV Cyg |87.69d*E (JD2428820 - 31260); Max = 2436413.8 + 89.63d*E (JD2434610 AV Cyg |- 37130); since JD2437450 - see Table. 0.27P <= M - m <= 0.50P. AX Cyg |VB A (B 10.2m, 18", 52{deg}). AY Cyg |In the region of the open cluster Dolidze 2. BB Cyg |P var. Max = 2426360 + 265.7d*E (JD2414900 - 26700); Max = 2433091 BB Cyg |+ 258.6d*E (JD2426700 - 35500); Max = 2438354 + 266.9d*E (JD35500 - BB Cyg |40200) [09106]; since JD2439200 - see Table. BF Cyg |P orb = 750d [05655]. Irregular light variations and sometimes BF Cyg |observed brightenings by 2m - 3m are superimposed by semiregular BF Cyg |oscillations with the cycle 755d [01039,08044]. BG Cyg |P var. Max = 2421190 + 290.35d*E (JD2421150 - 29950); Max = 2430546 BG Cyg |+ 307.3d*E (JD2429950 - 30850); Max = 2432872 + 289.5d*E (JD2430850 BG Cyg |- 34920); since JD2435100 - see Table. BI Cyg |VB A (B 9.4m, 126", 110{deg}). BO Cyg |D = 0.025P; Min II 12.0. BR Cyg |D = 0.020P; Min II 9.58. BS Cyg |SC 8/8. P var. Max = 2422655 + 420d*E (JD2422600 - 24750) [01161]; BS Cyg |Max = 2425181 + 431.4d*E (JD2424750 - 26500) [01171]; since BS Cyg |JD2437500 - see Table. BY Cyg |VB A (B 16m). BZ Cyg |[A/H] = 0.1. Double maximum. CD Cyg |[A/H] = 0.2. P var. There is a square term in the elements: CD Cyg |+1.54d*10**(-6)*E**2. CG Cyg |VB A (B 11.8m, 1.3", 306{deg}; 1979.7). 10.10 <= Min II <= 10.44. P CG Cyg |var. Min I = 2422967.4248 + 0.63114347d*E (JD2422900 - 38500); CG Cyg |since JD2439000 - see Table. Combined light range is given. Shape CG Cyg |of the light curve varies [08848]. CH Cyg |Semiregular light variations with the mean cycle 97d; mean CH Cyg |brightness varies with the cycle ~4700d [01169]. There are also a CH Cyg |cycle 725d [08849], rapid oscillations (A <= 0.25m U) and flares CH Cyg |[05350]. It is not excluded that the system is an eclipsing one CH Cyg |[06499]. CI Cyg |d = 0.084P. Depth of eclipses ~0.8m. The eclipses of B star are CI Cyg |observed. Usually there are light fluctuations near mean brightness CI Cyg |( ~12.1m). The outbursts last some dozens and hundreds days. Light CI Cyg |curves [06155,08044, 08850, 08851]. Emissions of H, He I, He II, CI Cyg |[OIII], and N III. CM Cyg |S 4/6.5e. CU Cyg |P var. Max = 2422643 + 223.8d*E (JD2422600 - 26500); since CU Cyg |JD2426500 - see Table. CV Cyg |dI = 0.06P; Min II 11.33. P var. Min I = 2424458.348 + 0.9834523d*E CV Cyg |(JD2414300 - 24500); since JD2424450 - see Table. Shape of the CV Cyg |light curve and Min I depth vary. CY Cyg |SC 2/7.5. CZ Cyg |P var. Max = 2424500 + 284d*E (JD2424500 - 33600) [03122]; since CZ Cyg |JD2432700 - see Table. DD Cyg |P var. Max = 2425465 + 148.30d*E (JD2424800 - 39000) [01149]; since DD Cyg |JD2439000 - see Table. DF Cyg |P var [01177,06107]. Mean brightness varies: Min = 2411292 + DF Cyg |780.2d*E [01571]. DG Cyg |SiO maser? DH Cyg |OH emission? DK Cyg |dI = dII = 0.04P; Min II 10.90. P var. Shape of the light curve and DK Cyg |depth of Min II vary. DL Cyg |Min II 9.9. DM Cyg |P var. Max = 2425887.560 + 0.4198557d*E (JD2415200 - 25900) DM Cyg |[03506]; Max = 2425887.5597 + 0.41985715d*E (JD2425880 - 29250) DM Cyg |[00522]; Max = 2433872.420 + 0.41985842d*E (JD2429250 - 37900) DM Cyg |[03506]; Max = 2438677.708 + 0.4198619d*E (JD2438600 - 41250) DM Cyg |[07114]; since JD2441240 - see Table. There is also Blazhko effect DM Cyg |with the elements: Max(O - C) = 2442978.97 + 26.01d*E [08853]; DM Cyg |-0.01 d< = O - C <= +0.01d. {Delta}(S) = 0. DQ Cyg |P = 180d? DT Cyg |P var. Max = 2424305.651 + 2.49913d*E (JD2424300 - 28500) [01183]; DT Cyg |Max = 2432792.893 + 2.49934d*E (JD2430000 - 36000); since JD2436000 DT Cyg |- see Table. DV Cyg |P var. Max = 2425476 + 146.7d*E (JD2415200 - 29200); since DV Cyg |JD2432800 - see Table. DW Cyg |P var. Max = 2427603 + 279.6d*E (JD2416700 - 33500); since DW Cyg |JD2433500 - see Table. DX Cyg |Min II 14.2; Min II - Min I = 0.515P; DI = 0.22P, DII = 0.12P. DY Cyg |VB A (B 3", 218 {deg}, 2002). Slow oscillations are superimposed by DY Cyg |rapid ones with A = 0.3m [03662]. According to [03148] type EB? Min DY Cyg |= 2436659.531 + 0.6990d(:)*E (JD2436600 - 37000) [03148]. EE Cyg |Min II 14.5. EF Cyg |142d <= P <= 175d. EH Cyg |P var. Max = 2427608 + 276.90d*E (JD2416200 - 27610); since EH Cyg |JD2427800 - see Table. EI Cyg |Epoch of Max I is given; heights of Max I and Max II differ EI Cyg |strongly, the depths of Min I and Min II are almost equal. Max I - EI Cyg |Min I = 52d. EK Cyg |Observations are represented by the elements in the interval EK Cyg |JD2425200 - 37900 only. EM Cyg |Mean cycle varies in the range 19d - 33d [04248,09111]. Depth of EM Cyg |eclipses 0.25m V; elements of eclipsing system light variations: EM Cyg |Min = 2437882.8595 + 0.29090950d*E - 21d*10**(-12)*E**2 [08854]. EM Cyg |Sometimes there are light oscillations with periods 14.6s - 21.2s EM Cyg |and an amplitude up to 0.4% [06102,09112]. EN Cyg |d = 0.012P. P var. Min = 2425181.311 + 2.2148998d*E (JD2424880 - EN Cyg |29600) [00332]; since JD2433500 - see Table. ES Cyg |P var. Max = 2425146 + 157d*E (JD2425000 - 29300) [00332]; since ES Cyg |JD2432800 - see Table. EV Cyg |P var. Max = 2427740 + 259.1d*E (JD2425100 - 29100); since EV Cyg |JD2433500 - see Table. The position of the star in the chart in EV Cyg |[00530] is wrong [00782]. EZ Cyg |P var? Shape of the light curve and the amplitude strongly vary; EZ Cyg |0.40P < = M - m < = 0.48P. FF Cyg |S 5.5/6-e. FG Cyg |P var. Max = 2426955 + 456.0d*E (JD2416000 - 27000) [00001]; Max = FG Cyg |2426955 + 458.8d*E (JD2426900 - 34300) [03122]; since JD2439200 - FG Cyg |see Table. FM Cyg |P var. Max = 2425313 + 274d*E (JD2425300 - 29200) [00332]; since FM Cyg |JD2429200 - see Table. FN Cyg |P var. Max = 2429137 + 314.6d*E (JD2416200 - 29200) [00001]; since FN Cyg |JD2432800 - see Table. FO Cyg |A var. P var. Max = 2425193 + 156.6d*E (JD2425000 - 29200) [00332]; FO Cyg |since JD2432500 - see Table. FR Cyg |Min II 14.0; d = 0.03P. FT Cyg |P var. Max = 2425184 + 156.7d*E (JD2425100 - 29200) [00332]. 83d <= FT Cyg |P <= 187d (JD2432500 - 38000). FY Cyg |P var. Max = 2425172 + 194.d*E (JD2425100 - 29300) [00332]. 130d <= FY Cyg |P< = 189d (JD2432500 - 38000). GG Cyg |d = 0.079P; Min II 12.1. GM Cyg |P var. Min = 2428754.305 + 4.745772d*E (JD2413200 - 33500) [01209]; GM Cyg |since JD2433500 - see Table. GN Cyg |P var. Max = 2425448 + 156d*E (JD2425400 - 27400) [01155]; since GN Cyg |JD2427500 - see Table. GO Cyg |Min II 8.73. P var. Intrinsic light variability of the components GO Cyg |is possible [01210]. GS Cyg |P = 195d? GT Cyg |Depth of Min II 0.05m? P var? GY Cyg |Secondary oscillation with P = 4000d and A(V) = 0.5m is possible. GZ Cyg |Red. HL Cyg |d = 0.02P. HV Cyg |VB (Northern component). HY Cyg |P var. Max = 2425334 + 344d*E (JD2425300 - 29200) [00332]; since HY Cyg |JD2432760 - LB? II Cyg |P var. Max = 2425150 + 82d*E (JD2425120 - 25550), Max = 2425475 + II Cyg |94d*E (JD2425550 - 29250) [00332]; since JD2432500 77d <= P <= 99d. IK Cyg |P var. Max = 2425199 + 77.3d*E (JD2425000 - 29200) [00332]; since IK Cyg |JD2432500 - see Table. IT Cyg |P var. Max = 2425305 + 67.4d*E (JD2425300 - 850) [00332]; since IT Cyg |JD2432500 - see Table. IU Cyg |B - V: +0.90, +1.45. P var. Max = 2429157.6 + 31.22266d*E IU Cyg |(JD2417800 - 29250); Max = 2433601.3 + 31.1550d*E (JD2432700 - IU Cyg |35400); since JD2435400 - see Table. IV Cyg |P var. Max = 2425470.406 + 0.33432871d*E (JD2425300 - 33120) IV Cyg |[03506]; Max = 2434122.519 + 0.33433895d*E (JD2432700 - 40200) IV Cyg |[04248]; since JD2440200 - see Table. Shape of the light curve IV Cyg |varies: 0.10P <= M - m <= 0.20P. IX Cyg |P var. Max = 2425173 + 172d*E (JD2425000 - 25900) [00332]; since IX Cyg |JD2428000 - see Table. KL Cyg |P var. Max = 2437906 + 536.8d*E (JD2418500 - 38000) [00001]; since KL Cyg |JD2438000 - see Table. KP Cyg |{Delta}(S) = 0. KR Cyg |Min II 9.37. KU Cyg |Min II 11.15; d = 0.047P. Shape of the light curve varies. KV Cyg |Min II 11.9. KY Cyg |H2O, OH maser. LN Cyg |Min II 14.3. LO Cyg |Min II 13.3. LX Cyg |P var. Max = 2432775 + 460.0d*E (JD2415000 - 33300) [01159]; since LX Cyg |JD2437900 - see Table. SC 7/9-e - SC 8/8.5e. MQ Cyg |VB A (B 17.5m B, 4.5", 122{deg}). P var. Max = 2432737 + 428.5d*E MQ Cyg |(JD2414300 - 33300) [01229]; since JD2440000 - see Table. MR Cyg |Min II 9.12; d = 0.030P; DII = 0.19P. MU Cyg |Min II 14.4. MY Cyg |Min II 8.99. Min II - Min I = 0.5021P. MZ Cyg |P var. Max = 2427641.914 + 21.162460d*E + 0.10575d*10**(-3)*E**2 MZ Cyg |(JD2414900 - 37900) [03689]; since JD2443600 - see Table. Probably MZ Cyg |it is an RV Tau type variable, and then the period should be MZ Cyg |doubled [08862]. [A/H] = 0.1. NQ Cyg |EW type is possible. Close to V736 Cyg. NU Cyg |Min II 14.9. NZ Cyg |Min II 14.2. OS Cyg |P var. OU Cyg |Min II 15.6. OY Cyg |Star 23 - 30 [01321]. PP Cyg |Star G in the chart for VV245 [07749]. PR Cyg |Star 24 - 40 [01321]. PT Cyg |Star 23 - 55 [01321]. PU Cyg |Star 25 - 56 [01321]. PX Cyg |Star 35 - 78 [01321]. PY Cyg |Min II 15.2. QS Cyg |Min II 13.3. QT Cyg |Depth of Min II 0.04m. QU Cyg |Min II 15.1. QW Cyg |Min II 14.1. QX Cyg |Min II 14.5. V0339 Cyg |np component of a close binary. V0340 Cyg |Min II 14.5. V0343 Cyg |[A/H] = -0.2. V0346 Cyg |Companion 13.8m, 0.4' sf. Min II 11.9. P var. Min I = 2427270.241 + V0346 Cyg |2.743345d*E (JD2415000 - 32000); since JD2432000 - see Table. V0348 Cyg |According to [07516] EW type variable with large irregularities: V0348 Cyg |Min = 2441567.177 + 0.285768d*E (JD2441567 - 95). V0355 Cyg |Min II 14.3. V0360 Cyg |P var [06107]. Min I = 2429187.4 + 70.449d*E (JD2414600 - 34000) V0360 Cyg |[00580]; since JD2426000 - see Table. V0366 Cyg |Min II 10.2. V0367 Cyg |VB A (A 0.1", 50{deg}; B 13.7m, 2.3", 255{deg}). Min II 7.16. Shape V0367 Cyg |of the light curve and the radial velocity curve vary. V0368 Cyg |According to [00204] EB type (12.8m - 13.8m pg) with the elements: V0368 Cyg |Min I = 2425808.10 + 0.47586d*E (JD2425805 - 853). V0369 Cyg |P var. Max = 2438199 + 104.46d*E (JD2426000 - 38200); since V0369 Cyg |JD2438200 - see Table. V0370 Cyg |Min II 11.9. P var. Min I = 2425096.429 + 0.77453979d*E (JD2414400 V0370 Cyg |- 30000); since JD2430000 - see Table. V0371 Cyg |Min II 12.5. V0374 Cyg |d = 0.03P. V0380 Cyg |Min II 5.76; Min II - Min I = 0.418P (1963). There are periodic V0380 Cyg |terms in the elements: +0.8916d*sin(38.8{deg} + 0.0082{deg}*E) - V0380 Cyg |0.0796d*sin(77.6{deg} + 0.0164{deg}*E) + 0.0088d*cos(26.4{deg} + V0380 Cyg |0.0246{deg}*E); Min II = 2441262.266 + 12.425612d*E - V0380 Cyg |0.8916d*sin(38.8{deg} + 0.0082{deg}*E) - 0.0796d*sin(77.6{deg} + V0380 Cyg |0.164{deg}*E) - 0.0088d cos (26.4{deg} + 0.0246{deg}*E). Apsidal V0380 Cyg |motion is possible with P = 1490 years. V0382 Cyg |VB A (B 11.5m, 11", 332{deg}). Min II 9.12. Shape of the light V0382 Cyg |curve and depth of Min II vary. P var. Min I = 2427992.458 + V0382 Cyg |1.885497d*E (JD2413480 - 29500) [01253]; since JD2428000 - see V0382 Cyg |Table. V0385 Cyg |Min II 12.4. V0387 Cyg |Min II 11.6. V0388 Cyg |Min II 9.15; d = 0.06P. P var. Min I = 2433584.540 + 0.8590507d*E V0388 Cyg |(JD2427600 - 37200); since JD2437200 - see Table. V0389 Cyg |VB A (B 8.0m, 3.4", 305{deg}, 1980). SB (P = 3.313168d); Turns V0389 Cyg |around the invisible third companion with P = 154.09d. According to V0389 Cyg |[01256] the light varies with two alternate periods P1 and P2. The V0389 Cyg |first oscillation (P1) with A = 0.19m satisfies the elements: Max = V0389 Cyg |2423298.460 + 1.12912d*E, the second (P2) with A = 0.05m - the V0389 Cyg |elements: Max = 2429162.080 + 1.19328d*E. each of them continues V0389 Cyg |for 1 - 3 weeks. At the transition from one oscillation to the V0389 Cyg |other irregular light variations are sometimes observed or almost V0389 Cyg |constant brightness. At the renewal of each oscillation its phase V0389 Cyg |remains unchanged, experiencing no shift. According to [08909] in V0389 Cyg |1975 - 1977 periodicity was not observed. V0393 Cyg |d = 0.02P. V0401 Cyg |Min II 11.13. P var. Min I = 2432881.277 + 0.582717d*E (JD2428800 - V0401 Cyg |34000); since JD2434000 - see Table. V0402 Cyg |VB A (B 20", 90{deg}). V0407 Cyg |VB A (B 14.0m, 8", 190{deg}). Light variations of the Mira type V0407 Cyg |variable are superimposed by the outburst of the probable nova V0407 Cyg |which occured near JD2428400 (1936) with the consequent slow light V0407 Cyg |decrease. Combined spectrum. V0411 Cyg |P var. Max = 2421075 + 321d*E (JD2421000 - 31100) [01262]; since V0411 Cyg |JD2431100 - see Table. V0416 Cyg |Red. V0425 Cyg |Description of the spectrum and its variations [02685,03149]. V0427 Cyg |P var. Max = 2425471 + 143d*E (JD2425400 - 5950) [01155]; since V0427 Cyg |JD2433850 - see Table. V0429 Cyg |In the region of the open cluster NGC 6883. V0430 Cyg |In the region of the open cluster NGC 6883. Max = 2425544 + 258d*E V0430 Cyg |(JD2425500 - 27400) [01155]. V0432 Cyg |In the region of the open cluster Dolidze 3. V0439 Cyg |In the region of the open cluster Berkeley 87 = OCL 161. V0441 Cyg |Epoch of Min I is given. V0442 Cyg |Min II 10.4:, d = 0.01P:. According to [08721] the period given in V0442 Cyg |[00525] must be doubled. V0443 Cyg |There is a periodic term in the elements: -0.016d*sin(0.00105*E). V0444 Cyg |In the H II region S 109. Min II 8.06; D II = 0.10P. P var. Min I = V0444 Cyg |2430856.453 + 4.21238d*E (JD2415000 - 30000) [00007]; since V0444 Cyg |JD2430000 - see Table. V0445 Cyg |P var. Min = 2425527.391 + 1.947833d*E (JD2425500 - 34700) [01155]; V0445 Cyg |since JD2434700 - see Table. V0447 Cyg |In the region of the open cluster NGC 6871. V0448 Cyg |In the region of the open cluster NGC 6871. Min II 8.40. V0450 Cyg |The light curve resembles that of DQ Her. V0453 Cyg |In the region of the open cluster NGC 6871. Min II 8.68; d = 0.03P; V0453 Cyg |Min II - Min I = 0.5077P. [07518]. According to [07518] there is V0453 Cyg |apsidal motion with P = 71 years. V0454 Cyg |Min II 12.3. In the region of the open cluster IC 4996. V0455 Cyg |Min II 10.9. P var. Min I = 2431151.908 + 8.7689331d*E (JD2426800 - V0455 Cyg |33950) [01286]; since JD2436800 - see Table. V0456 Cyg |Min II 11.4; Min II - Min I = 0.518P. P var? V0457 Cyg |Min II 13.9. V0458 Cyg |Min II 14.2. V0461 Cyg |PB ~7000d? [08251]. V0462 Cyg |P var. Max = 2428540 + 376.0d*E (JD2416000 - 35200); since V0462 Cyg |JD2435200 - see Table. V0463 Cyg |Min II 10.65; Min II - Min I = 0.514P. V0465 Cyg |There is a close companion of 17.5m. V0466 Cyg |Min II 11.4. V0469 Cyg |Min II 12.9; Min II - Min I = 0.57P. V0470 Cyg |Min II 8.545. V0471 Cyg |S 5.5/5.5. V0473 Cyg |P var. Max = 2430615 + 218.5d*E (JD2418000 - 31000) [00346]; since V0473 Cyg |JD2442300 - see Table. V0474 Cyg |d = 0.014P. V0477 Cyg |Min II 8.69; D II = 0.09P; d = 0.003P. P var. Min I = 2429194.309 + V0477 Cyg |2.3470011d*E (JD2410000 - 29200) [00001]; Min I = 2437317.2695 + V0477 Cyg |2.3469943d*E (JD2429200 - 39700) [08919]; since JD2439700 - see V0477 Cyg |Table. Apsidal motion with Pi = 349 years; E = 0.302 [06175]. V0477 Cyg |0.331P (1965 - 1970) <= Min II - Min I < = 0.460P (1904). V0478 Cyg |VB A (B 12.8m, 4", 259{deg}. Min II 9.02; Min II - Min I = 0.5072P. V0482 Cyg |VB A (B 14.4m V, M4 III, 8", 225{deg}). V0483 Cyg |Min II 11.9. V0484 Cyg |Min II 13.6. V0486 Cyg |Min II 14.3. V0488 Cyg |Min II 13.0. V0490 Cyg |Min II 13.5; Min II - Min I = 0.47P. V0491 Cyg |Min II 14.7. V0493 Cyg |Min II 12.9. V0494 Cyg |Min II 13.6. V0496 Cyg |Min II 12.5. V0498 Cyg |Min II 10.27. V0500 Cyg |VB B (A 11.5m; 18", 45{deg}). Min II 12.0. V0501 Cyg |Min II 13.1; d = 0.02P. V0502 Cyg |Min II 14.2. V0505 Cyg |Min II 12.0. V0509 Cyg |d = 0.05P. V0512 Cyg |Min II 11.5. There is a periodic term in the elements: V0512 Cyg |+0.065d*sin(0.2105263{deg}*(E + 538)). V0513 Cyg |Min II 12.6. V0519 Cyg |Min II 13.4. V0520 Cyg |VB A (B 15", 135{deg}). V0525 Cyg |d = 0.03P:. V0526 Cyg |Min II 13.1. In the region of the open cluster TGC 7039. V0532 Cyg |P var. Max = 2434618.158 + 3.283651d*E (JD2427900 - 35000); Max = V0532 Cyg |2436817.694 + 3.282792d*E (JD2435000 - 38700); since JD2438700 - V0532 Cyg |see Table. V0536 Cyg |d = 0.010P. V0538 Cyg |B - V: +1.17, +1.50. V0539 Cyg |P2 = 1500d. V0541 Cyg |Min II 10.9; DII = 0.012P; Min II - Min I = 0.453P. V0544 Cyg |P var? V0546 Cyg |Min II 15.2:; Min II - Min I = 0.48P; d = 0.077P. In the dark V0546 Cyg |nebula Barnard 144. V0547 Cyg |B - V: +1.27, +1.73. In the dark nebula Barnard 144. V0548 Cyg |Min II 8.62. P var. Min I = 2442279.3838 + 1.80524695d*E (JD2430800 V0548 Cyg |- 42300) [08930]; since JD2442300 - see Table. V0563 Cyg |P var. Max = 2427590 + 295.4d*E (JD2426000 - 30250); since V0563 Cyg |JD2430250 - see Table. V0567 Cyg |d = 0.036P. V0581 Cyg |Red. V0586 Cyg |In the region of the open cluster NGC 7039. V0588 Cyg |VB A (B 18m, 15", 0{deg}). Very Red. V0589 Cyg |VB. V0606 Cyg |P var. Max = 2428376.7 + 50.245d*E (JD2427950 - 31330) [01262]; V0606 Cyg |since JD2437100 - see Table. V0612 Cyg |Cycles of 50 - 100d (JD2427950 - 31330) [01262]; since JD2437100 - V0612 Cyg |see Table. V0614 Cyg |Min II 14.5. V0618 Cyg |In the region of the open cluster TGC 7092. V0622 Cyg |In the region of the open cluster NGC 7092. V0628 Cyg |Min II 12.5. V0635 Cyg |Min II 13.5. V0643 Cyg |P var. Elements given in the Table are valid in the interval V0643 Cyg |JD2427950 - 31330. V0644 Cyg |VB A (B 15.6m, 6", 141{deg}; C 16.3m, 6", 141{deg}). V0645 Cyg |Observed as the bright nebular condensation with ~2" diameter V0645 Cyg |scattering light of an O8 star associated with it but invisible V0645 Cyg |because of absorption. A part of strongly polarized bipolar nebula V0645 Cyg |with diameter about 10". There are strong emission lines of H, Fe V0645 Cyg |II, [OI], [SII], etc. In the spectrum [08942,09129]. H2O maser V0645 Cyg |source. Infrared source CRL 2789. V0651 Cyg |Min II 14.7. V0652 Cyg |Min II 12.1. V0664 Cyg |d = 0.05P. V0666 Cyg |P var. Max = 2427965 + 236d*E (JD2427950 - 31350) [01262]; since V0666 Cyg |JD2433400 - see Table. V0670 Cyg |sp component of a close binary. V0680 Cyg |Min II 10.3. V0685 Cyg |VB. V0687 Cyg |Min II 10.4. P var? V0688 Cyg |d = 0.029P. V0690 Cyg |d = 0.021P. V0691 Cyg |d <= 0.034P. V0692 Cyg |Min II 14.9? V0693 Cyg |Min II 14.4? V0694 Cyg |d = 0.017P. V0695 Cyg |31 Cyg. Probably enters a common system with V1488 Cyg (32 Cyg). VB V0695 Cyg |A (B 13.0m, 36.8", 332{deg}; C 6.99m, 107.0", 174{deg}; D 5.0m, V0695 Cyg |338", 323{deg}). d = 0.0151P. Interferometric binary eclipsing V0695 Cyg |system (A = 0.08", E = 0.15 [01582]; 0.035", 141.8{deg}, 1980.4). V0695 Cyg |The epoch of eclipse of the component of the spectral type B4 by V0695 Cyg |the component of the type K4 is given in the Table. The amplitude V0695 Cyg |strongly varies depending upon the wavelength: A({lambda} 6560 A) = V0695 Cyg |0.03m, A({lambda} 3530 A) = 1.80m [09131]. V0696 Cyg |Mean magnitude varies with P = 1600d. V0700 Cyg |Min II 12.3. P var. Min I = 2432028.863 + 0.340047d*E (JD2431700 - V0700 Cyg |37500) [05352]; since JD2437500 - see Table. V0704 Cyg |Min II 14.2. V0706 Cyg |Min II 13.9. V0713 Cyg |Min II 15.1. V0720 Cyg |P var. Min I = 2427611 + 332d*E (JD2429450 - 32000) [00798]; since V0720 Cyg |JD2432500 - see Table. V0726 Cyg |Min II 12.8; d = 0.018P. V0728 Cyg |P var. Min = 2425760.475 + 2.0601256d*E (JD2425500 - 35000) V0728 Cyg |[00164]; since JD2439700 - see Table. V0729 Cyg |VB A (B 13.5m, 1.5", 65{deg}). Min II 9.29. P var. Min I = V0729 Cyg |2434264.638 + 6.597700d*E (JD2428700 - 37900) [00001]; since V0729 Cyg |JD2439750 - see Table. V0731 Cyg |VB. V0735 Cyg |Depth of Min II 0.04m. V0736 Cyg |Min II 16.5. Close to NQ Cyg. V0737 Cyg |Star 23 - 50 [01321]. V0739 Cyg |Star 36 - 81 [01321]. V0741 Cyg |d = 0.03P. V0742 Cyg |P var. Max = 2429409.448 + 0.93979d*E (JD2428420 - 30700) [08977]; V0742 Cyg |Max = 2431489.580 + 0.94010d*E (JD2430250 - 32350); Max = V0742 Cyg |2433282.014 + 0.93979d*E (JD2432350 - 33650); since JD2433650 - see V0742 Cyg |Table. According to [08977] since JD2430700 the observations are V0742 Cyg |better represented by the elements: Max = 2432943.701 + V0742 Cyg |0.93977897d*E - 1.067d*10**(-7)*E**2. V0747 Cyg |The intervals between maxima of brightness are 2000 - 4000d. Not V0747 Cyg |red. V0751 Cyg |In the region of the nebula IC 5070. SB (P = 0.25d [09132]). Rapid V0751 Cyg |small variations near maximum of brightness (B - V = +0.25) are V0751 Cyg |superimposed sometimes by deep minima lasting for some hundreds V0751 Cyg |days [02699]. Soft X-ray source [09133]. Spectrum description V0751 Cyg |[02698,09132]. V0752 Cyg |B - V = +0.77, U - B = -0.47. V0753 Cyg |d = 0.12P. P = 0.952374d? V0757 Cyg |Red. V0758 Cyg |P = 400d? V0759 Cyg |P var. Max = 2434513.427 + 0.36001476d*E (JD2414430 - 34570) V0759 Cyg |[03506]; since JD2434500 - see Table. Blazhko effect. V0779 Cyg |Type RR? V0781 Cyg |P var? V0783 Cyg |P var. Max = 2433261.029 + 0.62069487d*E (JD2424690 - 34000); since V0783 Cyg |JD2438970 - see Table. V0786 Cyg |Usually in minimum brightness, with rapid brightenings by 0.5m - V0786 Cyg |1.0m. In the interval JD2427692 - 697 the brightness was 13.5m. V0789 Cyg |P var? [Fe/H] = -0.91. V0795 Cyg |sf component of a close pair. V0796 Cyg |Min II 11.4. V0797 Cyg |Min 15.4. V0799 Cyg |P var. V0801 Cyg |There is a square term in the elements: +1.93d*10**(-10)*E**2. V0802 Cyg |P var. Max = 2432779.9342 + 0.59560377d*E (JD2425480 - 35170) V0802 Cyg |[02775]; Max = 2439415.263 + 0.5955638d*E (JD2435950 - 40000) V0802 Cyg |[09266]. Max = 2440036.409 + 0.595447d*E (JD2440000 - 41000); Max = V0802 Cyg |2441517.498 + 0.595635d*E (JD2441000 - 42500); since JD2442500 - V0802 Cyg |see Table. Shape of the light curve varies (0.13P <= M - m <= V0802 Cyg |0.50P); period variations are accompanied sometimes by strong V0802 Cyg |variations of amplitude (in the interval JD2440000 - 41000; 0.3m <= V0802 Cyg |A <= 1.7m). V0803 Cyg |Min II 14.5. V0806 Cyg |Min II 15.0; DII = 0.061P. V0807 Cyg |Min II 14.9. V0808 Cyg |Brightness in maximum varies. V0809 Cyg |Min II 13.6; DII = 0.069P. V0810 Cyg |d = 0.050P. Depth of Min II 0.05m. P var? V0817 Cyg |sp component of the pair. V0818 Cyg |Shape of the light curve and period vary. V0821 Cyg |Min II 15.6. V0822 Cyg |Min II 13.0. V0824 Cyg |Min II 14.3. V0825 Cyg |Min II 16.9. Min II = 2433871.915 + 7.709015d*E. V0826 Cyg |Min II 14.7. V0828 Cyg |Min II 10.12. V0832 Cyg |VB A (B 9.43m, 20", 352{deg}; C 11.62m, 27", 141{deg}; D 12.72m, V0832 Cyg |38", 220{deg}). description of spectral variations [09135]. V0836 Cyg |Min II 8.77. P var. Min I = 2426547.5224 + 0.65341090d*E (JD2425500 V0836 Cyg |- 42000) [03869]; since JD2441200 - see Table. Shape of the light V0836 Cyg |curve varies. V0840 Cyg |LS II 28.3{deg} [08090]. Cycles 250 - 300d. V0841 Cyg |Min II 11.2. V0842 Cyg |Min II 14.1. V0844 Cyg |VB A (B 17.8m, 2.9", 50{deg}). V0850 Cyg |Min II 11.8. P var. Min I = 2430587.263 + 4.5578d*E (JD2428750 - V0850 Cyg |30590) [04253]; since JD2434330 - see Table. V0851 Cyg |d = 0.017P? V0852 Cyg |Min II 14.9. V0853 Cyg |Min II 14.2. V0856 Cyg |Depth of Min II 0.05m. V0857 Cyg |Depth of Min II 0.03m. V0859 Cyg |Min II 12.1. V0865 Cyg |Min II 14.6. V0866 Cyg |Min II 13.9. V0869 Cyg |Min II 14.8. Shape of the light curve varies. V0870 Cyg |Min II 15.8. V0871 Cyg |Min II 14.9. V0873 Cyg |Min II 14.7. Min II - Min I = 0.48P. V0874 Cyg |Min II 13.8. V0877 Cyg |Min II 12.9. V0880 Cyg |Min II 14.1; Min II - Min I = 0.506P; d = 0.02P. V0881 Cyg |{Delta}(S) is small [09037]. V0882 Cyg |[Fe/H] = -1.42. V0884 Cyg |np component of a pair. Min II 14.2. V0885 Cyg |Min II 10.2. V0886 Cyg |Min II 14.1; Min II - Min I = 0.515P. V0887 Cyg |Depth of Min II 0.03m. V0888 Cyg |Min II 15.9. V0889 Cyg |Min II 10.4. V0891 Cyg |Min II 9.4. V0892 Cyg |Min II 15.5. nf component of a close pair. V0900 Cyg |Min II 15.2. V0902 Cyg |d = 0.02P. Depth of Min II 0.05m. V0906 Cyg |Min II 15.7. V0907 Cyg |Min II 14.9. According to [04427] Min I = 2435066.257 + V0907 Cyg |0.54138554d*E. V0908 Cyg |nf component of a close pair. Depth of Min II 0.04m. V0909 Cyg |Min II 9.66. V0910 Cyg |Min II 14.2; d = 0.02P. V0911 Cyg |Min II 14.6. P var? Min I = 2432120.251 + 3.42262215d*E (JD2415500 V0911 Cyg |- 37900) [04761]; since JD2437100 - see Table. V0912 Cyg |Depth of Min II 0.05m. V0913 Cyg |VB A (B 17m, 0{deg}). V0920 Cyg |A var. Blazhko effect? V0922 Cyg |d = 0.02P:. V0924 Cyg |P var. Max = 2435706.776 + 5.5709816d*E (JD2432760 - 38000) V0924 Cyg |[08053]; since JD2438000 - see Table. V0925 Cyg |Min II 16.0. V0927 Cyg |Epoch of Min brightness is given. V0928 Cyg |Min II 15.4. V0931 Cyg |Min II 14.5. V0932 Cyg |Depth of Min II 0.04m. V0934 Cyg |Min II 13.7. V0936 Cyg |Depth of Min II 0.05m. V0939 Cyg |Min II 12.5. V0940 Cyg |Min II 15.1. V0941 Cyg |Min II 13.2. V0942 Cyg |VB A (B ~10{deg}, C ~110{deg}). V0944 Cyg |np component of pair. V0947 Cyg |Min II 15.0. V0948 Cyg |Min II 15.2. V0949 Cyg |Red. V0955 Cyg |Min II 15.3. sp component of a close pair. V0956 Cyg |Min II 15.1. sp component of a close pair. V0957 Cyg |Min II 12.6. V0958 Cyg |P = 199d? V0959 Cyg |Min II 11.4; Min II - Min I = 0.52P; DII = 0.16P:. sp component of V0959 Cyg |a close pair. V0961 Cyg |Min II 12.4; Min II - Min I = 0.505P. V0962 Cyg |d = 0.02P:. V0964 Cyg |Min II 14.4. V0965 Cyg |Min II 14.9. Type RRC? P = 0.32028628d? V0970 Cyg |Min II 14.8. V0974 Cyg |Min II 12.5; Min II - Min I = 0.462P. Min II = 2435373.398 + V0974 Cyg |3.204418d*E. V0979 Cyg |Min II 14.7. V0981 Cyg |Min II 15.0. V0982 Cyg |Red. V0997 Cyg |[Fe/H] = -0.77. V1004 Cyg |Min II 13.0. V1007 Cyg |Depth of Min II 0.04m. V1008 Cyg |Min II 16.0. V1010 Cyg |Depth of Min II 0.03m. V1011 Cyg |Depth of Min II 0.04m. V1012 Cyg |Min II 15.4. V1016 Cyg |Before the outburst in 1964 the brightness changed between 15.0m V1016 Cyg |and 17.5m pg [05701], the spectral type was late Me {alpha} V1016 Cyg |[01222]. In the 1964 - 67 the brightness increased from 16.0m to V1016 Cyg |11.2m B. In 1967 - 69 the brightness steadily increased to 10.05m V1016 Cyg |B, being constant in V system (10.5m). In the infrared it changes V1016 Cyg |in the limits 6.9 - 8.4 J, 4.7 - 5.8 K with the period 470d V1016 Cyg |[07174,09141]. High excitation emission spectrum with strong IR V1016 Cyg |excess resembles that of symbiotic variables [09142]. X-ray and V1016 Cyg |radio source. V1018 Cyg |Min II 11.6. V1021 Cyg |Min II 14.3. V1023 Cyg |Min II 12.9; d = 0.03P:. DII = 0.14P. Min II - Min I = 0.495P. V1024 Cyg |Depth of Min II 0.04m. V1030 Cyg |Elements given in the Table are valid in the interval JD2426600 - V1030 Cyg |32300. V1033 Cyg |P var. V1034 Cyg |Min II 9.9. V1035 Cyg |P var? V1037 Cyg |Min II 14.8. V1038 Cyg |VB B (9.4", 215{deg}, 1963). Min II 15.5. V1039 Cyg |Min II 15.6. V1042 Cyg |VB A (B 10m, 53", 110{deg}). In HII region S 109. V1044 Cyg |Min II 16.5. V1045 Cyg |Min II 16.0. V1047 Cyg |d = 0.02P. V1053 Cyg |d = 0.05P. V1057 Cyg |In the dark nebula, in the region of the North America nebula (NGC V1057 Cyg |7000). In 1969 - 70 (JD2440400 - 830) the outburst from 16.5m to V1057 Cyg |10.3m occured. Brightness maximum was observed at JD2440830 V1057 Cyg |(spectrum - B3). Before the outburst the light changed in the range V1057 Cyg |15.5m - 16.5m, the spectral type was Ke with characteristic V1057 Cyg |features of T Tau type stars [02698,06415]. After the outburst the V1057 Cyg |brightness began to weaken monotonouosly and in 1982 reached 13.1m V1057 Cyg |B (the spectral type about G2 - G5 Ib). Strong H{alpha} emission V1057 Cyg |appeared in 1971. There are also small rapid light fluctuations. V1057 Cyg |Description of light variations [06504,07115, 07754, 08996]. The V1057 Cyg |star is associated with a luminous arc-shaped reflection nebula. V1057 Cyg |This nebula with length of about 3' appeared in 1971 and its V1057 Cyg |brightness is gradually decreasing simultaneously with the fading V1057 Cyg |of the star. V1061 Cyg |Min II 9.5. V1063 Cyg |P var. Max = 2428260 + 339d*E (JD2428260 - 30700); since JD2433500 V1063 Cyg |- see Table. V1064 Cyg |Min II 15.3. V1068 Cyg |Min II 11.2; d = 0.070P. A migrating wavelike distorsion with an V1068 Cyg |amplitude ~0.1m V is being observed outside eclipses [08999]. V1073 Cyg |Min II 8.57. V1074 Cyg |Min II 14.8. V1083 Cyg |Min II 11.2. V1085 Cyg |Observations given in [07010] contradict the elements given in V1085 Cyg |[07193]: Min = 2437856.592 + 2.8089d*E. V1096 Cyg |d = 0.03P. V1102 Cyg |Radio-quiet N galaxy. Absorption spectrum without emission lines; z V1102 Cyg |= 0.0272. V1111 Cyg |Blazhko effect is possible. V1122 Cyg |Blazhko effect is possible. V1130 Cyg |Min II 12.9. V1136 Cyg |Min II 13.2. Eccentric orbit (E = 0.3). Apsidal motion is possible V1136 Cyg |[08051]. V1141 Cyg |Min II 11.8. V1142 Cyg |Min II 13.4. V1143 Cyg |Min II 6.06; Min II - Min I = 0.743P; d = 0.002P. V1157 Cyg |Min II 13.6. V1158 Cyg |d = 0.02P; Depth of Min II 0.04m. V1161 Cyg |d = 0.01P. V1162 Cyg |Only one Max was observed (see Table). Thereafter - either V1162 Cyg |invisible, or fairly constant (17.6m - 17.8m). Bluish. V1171 Cyg |VB A (B 11.0m, 0.34", 71.2{deg}; 1979.5). Min II 10.3. V1175 Cyg |Min II 16.5. P var. Min I = 2434629.545 + 1.3330d*E (JD2426620 - V1175 Cyg |34630); since JD2434635 - see Table. V1176 Cyg |VB. Variable is probably the northern red component. V1187 Cyg |In the nebula IC 1318B. Min II 11.19. P = 3.7675d? V1188 Cyg |Min II 14.3. V1189 Cyg |Min II 13.7. P var. Min I = 2437906.516 + 1.041908d*E (JD2426620 - V1189 Cyg |31240); since JD2437906 - see Table. V1191 Cyg |In the nebula IC 1318B. VB A (B 13m, 11", 299{deg}; C 13m, 11", V1191 Cyg |284{deg}). Min II 11.11. Shape of the light curve varies. V1193 Cyg |Min II 14.3. V1196 Cyg |Depth of Min II 0.05m. V1200 Cyg |Min II 16.1:. V1210 Cyg |Red. V1212 Cyg |Red. V1218 Cyg |VB A (B 17m, sf). V1225 Cyg |VB A (B 16m V, B - V = +1.3m, 1.2", 270{deg}; C 15.0m V, B - V = V1225 Cyg |+0.5m, 2.4", 270{deg}); P var? Max = 2428250 + 384.2d*E (JD2428200 V1225 Cyg |- 38250) [03160]; since JD2438500 - see Table. V1236 Cyg |Red. V1255 Cyg |Brightness in Max varies in the range 15.2m - 16.0m with possible V1255 Cyg |elements: Max = 2439382.281 + 0.28619537d*E. V1256 Cyg |Min II 14.1. V1273 Cyg |Min II 16.5. V1275 Cyg |In the region of the open cluster NGC 6819. V1281 Cyg |Min II 15.4. V1285 Cyg |Red. V1302 Cyg |Depth of Min II 0.05m. V1305 Cyg |Min II 11.5m - 11.7m (var). V1307 Cyg |Considerable dispersion of mean light curve points. V1315 Cyg |Min II 15.3. V1316 Cyg |(P) > 100d. V1318 Cyg |LkH {alpha} 225. Associated with a cometary nebula. V1321 Cyg |P = 0.7281802d? V1322 Cyg |In the region of the open cluster NGC 6913. V1326 Cyg |Min II 11.8; Min II - Min I = 0.53P. V1327 Cyg |Very red. V1329 Cyg |In 1891 - 1964 light variations in the range 14.2m - 15.5m with V1329 Cyg |deep minima to 18m; the minima are satisfied by the elements given V1329 Cyg |in the Table; D = 0.1p; spectral type M [07235]. In 1964 - the V1329 Cyg |outburst up to 12.1m. Then gradual brightness decrease superimposed V1329 Cyg |by periodical variations with an amplitude near 1m. Light minima as V1329 Cyg |before are satisfied by the elements given in the Table but the V1329 Cyg |character of eclipses changed (probably because of appearance of a V1329 Cyg |dense envelope ejected by one of the components of the system). V1329 Cyg |After the outburst high excitation emission spectrum with IR excess V1329 Cyg |is observed similar to the spectrum of symbiotic variables. V1331 Cyg |Associated with a cometary nebula. V1334 Cyg |VB A (B 7.9m, B5 - B8, 0.13", 26.1{deg}, 1975). V1336 Cyg |According to [07010], RR? P = 0.5d? V1341 Cyg |Cyg X-2. SB1. Halo object ({nu} = -220 km/s). Strong reflection V1341 Cyg |effect changes the spectral type of the F component. Spectral line V1341 Cyg |profiles vary. The lines of He II, KCa II, C III,and N III are in V1341 Cyg |emission. The system has low and high states. During the low state V1341 Cyg |the mean light curve is a double wave with the range 15.1m - 15.4m V1341 Cyg |B. Epoch of Min I given in the Table corresponds to the F star in V1341 Cyg |superior conjunction; Min II 15.4. The eclipse of the accretion V1341 Cyg |disk at the phase 0.5P in partial. Rapid light variability by 0.1m V1341 Cyg |in 10 minutes and by 0.5m in several hours is superimposed. In the V1341 Cyg |high states lasting for ~10d the mean light increases by 0.5m. V1341 Cyg |Radio source at 8085 MHz, source of soft and hard X-ray emission V1341 Cyg |from 0.1 to 60 KeV. V1345 Cyg |Min II 15.0:. V1354 Cyg |Depth of Min II 0.04m. V1356 Cyg |Min II 10.4. V1357 Cyg |Cyg X-1. SB1. The epoch of the inferior conjunction of the optical V1357 Cyg |component is given in the Table. Min II 8.88. The shape of the V1357 Cyg |light curve varies; Min II sometimes are not observed. The V1357 Cyg |periodicity in the light curve variations as well as in V1357 Cyg |polarization changes is possible with P = 78.4d [09021,09022]. V1357 Cyg |Rapidly variable X-ray source in wide range up to 3 MeV V1357 Cyg |characterized by the change of high and low states. Light and X-ray V1357 Cyg |variation with P = 294d is also detected [09154,09156]. Variable V1357 Cyg |and flare radio source at 2695 and 8085 MHz. V1372 Cyg |P2 = 360d?. V1374 Cyg |Min II 17.7. V1384 Cyg |In the region of the open cluster NGC 6913. V1396 Cyg |VB AB (10.26m V, 12.3m V; A = 0.1127", P = 29.33 Y [09026]); {mu} = V1396 Cyg |0.67", P = 113{deg}; A-SB 2 (mAb - mAa = 0.6m, P = 3.275631d V1396 Cyg |[09025]). Probably all the three components of the system are V1396 Cyg |variables of the UV Cet type, and according to [05716] also of the V1396 Cyg |BY Dra type. The range of combined brightness of the system is V1396 Cyg |given in the Table. Really the flare of AB component was observed V1396 Cyg |in the spectrograms [09025]. V1401 Cyg |Min II 13.6. V1410 Cyg |P > 400d. V1411 Cyg |P = 1.553478d? V1412 Cyg |Min II 15.5. V1414 Cyg |Northern component of a close pair; d = 0.04P. V1416 Cyg |Min II 14.7. V1417 Cyg |Min II 13.1. V1421 Cyg |In the region of the planetary nebula NGC 6857 = K3 - 50. V1425 Cyg |Depth of Min II 0.31m. V1427 Cyg |In the region of the open cluster M39. V1429 Cyg |Min II 15.3. V1430 Cyg |Min II 15.0. V1436 Cyg |Min II 15.9, D II = 0.08P; Min II - Min I = 0.48P. V1437 Cyg |Min II 16.0. V1440 Cyg |In the region of the open cluster NGC 6819. V1465 Cyg |Resembles an eclipsing variable. V1478 Cyg |VB A (B 17m:, 3", 80{deg}). Compact radio source. extended V1478 Cyg |structure centered at the star is observed at 5 Ghz. Bq [] star V1478 Cyg |with the excess of infrared radiation of dust at T = 300{deg}K. V1478 Cyg |Description of the spectrum [07080,07081, 07523, 09159, 09160]. V1479 Cyg |In the region of the nebula IC 5070. V1481 Cyg |Min II 12.5. In the region of the open cluster NGC 7128. V1485 Cyg |Identical to VES 28, as it follows from latter star's coordinates V1485 Cyg |and magnitudes in [7095], but the star is actually invisible in the V1485 Cyg |chart in [7095], where a faint companion, to 0.4'N of the variable, V1485 Cyg |is erroneously marked. Similarly, it is identical to +29{deg} 104, V1485 Cyg |judging from the latter star's photometry and spectral type from V1485 Cyg |[4732]; however, the star is plotted slightly offset (by 0.8' to E) V1485 Cyg |in the chart in [4732]. V1488 Cyg |32 Cyg. Probably enters a common system with V695 Cyg (31 Cyg). D = V1488 Cyg |0.015P, 0 < d < 0.011P. P var. Min I = 2420670.0 + 1140.1d*E V1488 Cyg |(JD2411400 - 29700). Since JD2429700 - see Table. The epoch of the V1488 Cyg |eclipse of the B4 type Component by the K5 type component is given. V1488 Cyg |There is also small physical light variability of the K component V1488 Cyg |[08896,09161]. Depth of eclipses depends of {lambda}: 0.04M V, V1488 Cyg |0.13m B, 0.27m ({lambda} 4243A),0.90m ({lambda} 3552A). V1489 Cyg |NML Cyg. 17.0m: - 18.0m V, B>21M; I - K = +8.17. Very large IR V1489 Cyg |exess due to expanding gaseous-dust envelope. In the area 2.5"*3.5" V1489 Cyg |around the star the system of about 60 discrete sources of OH V1489 Cyg |emission is detected [07461]; source of OH, H2O, SiO maser V1489 Cyg |emission. Light variations are periodical (see also [09163]). The V1489 Cyg |object may be a protostar being observed at the end of condensation V1489 Cyg |process. The late spectrum arises probably in the extending V1489 Cyg |envelope [09165,09166]. V1490 Cyg |In the region of the nebula IC 5070. V1491 Cyg |In the region of the nebula IC 5070. V1492 Cyg |In the region of the nebula IC 5070. V1493 Cyg |In the region of the nebula IC 5070. V1707 Cyg 10.5"P. V1494 Cyg |In the region of the nebula IC 5070. V1495 Cyg |In the region of the nebula NGC 7000. V1497 Cyg |In the region of the nebula NGC 7000. V1498 Cyg |In the region of the nebula NGC 7000. V1500 Cyg |In August 1975, before the very rapid increase of light, the V1500 Cyg |brightness of the Nova gradually increased from 17.6m to 13.5m B V1500 Cyg |(JD2442632 - 653.2). After Max almost monotonous decay of V1500 Cyg |brightness is superimposed by light variations with the amplitude V1500 Cyg |of 0.03m - 1.0m V; the period of these variations in the interval V1500 Cyg |JD2442656 - 43100 changed in the range 0.1415d [09167, 09168] - V1500 Cyg |0.137d [09169,09170]. Since JD2443100 Min = 2443696.4827 + V1500 Cyg |0.1396133d*E. Some investigators (see, for instance, [09173]) adopt V1500 Cyg |double value of this peiod. A month after the light maximum of the V1500 Cyg |Nova the radio emission was registered at 2695 and 8085 MHz V1500 Cyg |[09171]. V1507 Cyg |The epoch of a broad Min I (superior conjunction of the B V1507 Cyg |component) is given; Min II 7.01; D II = 0.20P, Min II - Min I = V1507 Cyg |0.29P; e = 0.39. Unusual light curve [08213,09049]. Shape of the V1507 Cyg |light curve and depths of Min vary. Gaseous streams And expAnding V1507 Cyg |envelope. V1508 Cyg |Min II 13.3. V1509 Cyg |VB A (B 11.7m, 55", 106{deg}). V1511 Cyg |V - K = 13.6m. V1513 Cyg |SB. V1515 Cyg |In a dark nebula, near the nebula NGC 6914. Connected with nebular V1515 Cyg |appendage like a Comma. Light increase was observed from 1944 till V1515 Cyg |1958. Since 1958 the star is in Max. Slow light variations with A V1515 Cyg |<= 1.6m. The absorption line Li I {lambda} 6707A is seen in the V1515 Cyg |spectrum. V1521 Cyg |Cyg X-3. Peculiar infrared X-ray source. V > 23m. Flare radio V1521 Cyg |source. In the K band short and slow flares on the time scale about V1521 Cyg |2 minutes and 1-2 hours, irregular variations and longperiodic V1521 Cyg |variability are observed [07752]. These variations are accompanied V1521 Cyg |by periodical oscillations of infrared, X-ray and gamma radiation V1521 Cyg |with the elements: Min = 2440949.8986 + 0.1996830d*E + V1521 Cyg |1.25d*10**(-10)*E**2 [09187]. Usually the amplitude of these V1521 Cyg |variations A(K) = 0.5m, but sometimes they disappear completely. V1531 Cyg |LkH {alpha} 142. VB A (B = V1532 Cyg, 2.5", 90{deg}). In the region V1531 Cyg |of the nebula IC 5070. Combined brightness and spectrum are given. V1532 Cyg |LkH {alpha} 143. VB B (A = V1531 Cyg; B 2.5", 90{deg}). In the V1532 Cyg |region of the nebula IC 5070. Combined brightness and spectrum are V1532 Cyg |given. V1535 Cyg |In the region of the nebula IC 5070. V1536 Cyg |In the region of the nebula NGC 7000. V1538 Cyg |In the region of the nebula NGC 7000. V1539 Cyg |In the region of the nebula NGC 7000. V1540 Cyg |In the region of the nebula NGC 7000. V1546 Cyg |In the region of the nebula NGC 7000. V1548 Cyg |VB A (B 16.7m, 6.2", 131{deg}). V1554 Cyg |VB A (B 14.7m, 3.5", 214{deg}). V1577 Cyg |In the cluster and nebula IC 5146. V1578 Cyg |In the cluster and nebula IC 5146. VB A (B 15m, 5", 45{deg}; C 17m, V1578 Cyg |5", 225{deg}). Associated with a reflecting nebula. V1580 Cyg |There is a periodic term in the elements: -0.027d*sin(0.045{deg}) V1580 Cyg |(JD - 2439000). V1581 Cyg |G 208 - 44. VB A (B = G 208 - 45, 15.97m V, M6Ve; 7.9", 106{deg}, V1581 Cyg |1954; 8.2", 96{deg}, 1974). {mu} = 0.71", P = 140{deg}. The flare V1581 Cyg |was observed during spectroscopic observations [09175]. The V1581 Cyg |companion may be also a UV Cet type variable. The range of combined V1581 Cyg |brightness variation of the system is given. V1584 Cyg |Epoch of min brightness is given. V1597 Cyg |In the region of the nebula IC 5070. V1598 Cyg |In the region of the nebula IC 5070. V1600 Cyg |In the region of the nebula IC 5070. V1608 Cyg |In the region of the nebula NGC 7000. V1610 Cyg |Infrared source CRL 2688, the star of the spectral type F5Ia, V1610 Cyg |associated with a bipolar reflection nebula (the so-called Egg V1610 Cyg |nebula). The northern component of the nebula is 4" to the north V1610 Cyg |from the source. Since 1920 to 1958 the integrated light of this V1610 Cyg |component increased from 15.2m to 13.4b B and after that does not V1610 Cyg |vary [08735]. Light of the faint (16.2m B) southern component (5" V1610 Cyg |to the south from the source) varies by 0.6m B [09176]. The V1610 Cyg |radiation of the nebula is strongly polarized (46%, {theta} = V1610 Cyg |106{deg} in V system). There are C3 absorption features as well as V1610 Cyg |Na, C2, and [SII] emission in the spectrum. Probably the object is V1610 Cyg |a precursor of a planetary nebula [09178]. V1611 Cyg |In the region of the nebula NGC 7000. V1624 Cyg |A var. In 1957 out of a B star turned into Be star. Probably must V1624 Cyg |be referred also to GCAS type. V1661 Cyg |VB A (B 11.14m, 20", 174{deg}). V1668 Cyg |There are sinusoidal light variations with A(V) = 0.15m and V1668 Cyg |elements Min = 2443767.475 + 0.4392d*E in the descending branch of V1668 Cyg |the light curve after JD2443765 [09179]. Infrared light curves (1.6 V1668 Cyg |- 10 mkm) have a secondary maximum (JD2443815) due to the formation V1668 Cyg |of the dust envelope. At 10 mkm this secondary maximum is brighter V1668 Cyg |than the primary one [09069]. V1669 Cyg |d = 0.036P. V1671 Cyg |{Delta}(U) = 0.06. V1674 Cyg |VB (B 15m, 5"). The range of combined brightness variation is V1674 Cyg |given. It is not excluded that it is the component B that is V1674 Cyg |variable. Slow variations of mean brightness in the range 10.555m - V1674 Cyg |10.570m B are superimposed by sinusoidal periodikal ones with P1 = V1674 Cyg |1.3608d (A1 = 0.0037m) and P2 = 0.8055d (A2 = 0.0032m). V1676 Cyg |In the open cluster NGC 6871. ADS 13374 A (B 12.0m, 6.5", 64{deg}; V1676 Cyg |C 11.0m, 9.5", 28deg D 9.5m, B3V, 11.4", 301{deg}; E 11.42m, 28.1", V1676 Cyg |109{deg}; F 7.36m, B1IA, 35.9", 29{deg}); SB2 (P = 112.7d). V1696 Cyg |SB1 (Porb = 4.3174d). Epoch of Min brightness is given. The eclipse V1696 Cyg |of the accretion disc around the compact object formed in the V1696 Cyg |outburst of a Supernova in a binary system about 5*10**6 years ago V1696 Cyg |is possible [03619]. V1701 Cyg |In the region of the nebula IC 5070. V1702 Cyg |In the region of the nebula IC 5070. V1703 Cyg |In the region of the nebula IC 5070. V1704 Cyg |In the region of the nebula IC 5070. V1706 Cyg |In the region of the nebula IC 5070. V1707 Cyg |In the region of the nebula IC 5070. V1493 Cyg 10.5"f. V1711 Cyg |In the region of the nebula NGC 7000. V1716 Cyg |In the region of the nebula NGC 7000. V1719 Cyg |Shape of the light curve varies. V1720 Cyg |Min II 7.79. V1721 Cyg |P var.Min I = 2442605.497 + 2.724370d*E (JD2442311 - 928); since V1721 Cyg |JD2442928 - see Table. V1722 Cyg |Min II 14.6? V1726 Cyg |Possible member of an anonimous open cluster. V1727 Cyg |4U 2129 +47. Lx/Lopt ~10. Emissions in the spectrum: NeII {lambda} V1727 Cyg |4686A, CIII - NIII {lambda} lambda 4640 - 50A. V1735 Cyg |In the complex of dark nebulae associated with the open cluster and V1735 Cyg |the nebula IC 5146. Lights up a reflecting nebula. Became brighter V1735 Cyg |by 5m at least from 1952 to 1965. V1737 Cyg |B - V = +3.7. V1738 Cyg |B - V = +5.5:. V1739 Cyg |B - V = +4.5:. V1744 Cyg |Epoch of Max in U system is given. V1746 Cyg |Sometimes P = 0.21d is observed. V1747 Cyg |P > 100d. B - V = +4.0. V1748 Cyg |In the nebula IC 1318a. V1751 Cyg |In the nebula IC 1318c. V1761 Cyg |Close companion? Elements are not certain. V1860 Cyg |The chart in [68103] is wrong. V2105 Cyg |Variability type and spectral type (F8Iab:) do not agree. V2121 Cyg |Strong Blazhko effect. V2150 Cyg |Type RR: is also possible. V2174 Cyg |SB, Porb = 225.162d. V2175 Cyg |X-ray source. V2312 Cyg |Erroneously called HD 192776 in [77190]. V2324 Cyg |Possible brightening trend over 6 years, maybe due to dissipating V2324 Cyg |dust envelope, plus quicker variations. V2363 Cyg |The depth of MinII is 0.13. V2364 Cyg |MinII 11.73. O'Connell effect. V2374 Cyg |The classification suggested in [78276] is EB?, with a twice longer V2374 Cyg |period. V2375 Cyg |The depth of MinII is 0.20. V2376 Cyg |The depth of MinII is 0.50. V2380 Cyg |The depth of MinII is 0.35. V2381 Cyg |The depth of MinII is 0.20. V2383 Cyg |The depth of MinII is 0.15. V2385 Cyg |The depth of MinII is 0.30. V2386 Cyg |The depth of MinII is 0.50. V2388 Cyg |The depth of MinII is 0.40. V2389 Cyg |The depth of MinII is 0.35. V2390 Cyg |The depth of MinII is 0.05. V2394 Cyg |The depth of MinII is 0.16. V2409 Cyg |MinII 14.1. V2414 Cyg |MinII 10.22, the phase of MinII is about 0.3 P. Pulsations possibly V2414 Cyg |overlapped. V2417 Cyg |Cool companion, slow variations. V2421 Cyg |MinII 14.20. V2422 Cyg |The depth of MinII is 0.47. V2428 Cyg |In quiescence, Max = 2440749 + 774 * E. V2456 Cyg |MinII 11.6. V2473 Cyg |VB AB (12.7mV, 14.3mr, 4", 267{deg}, 2000; C 14.4mV, 18", 188{deg}, V2473 Cyg |2000). V2474 Cyg |A possible different classification is RV [79100]. V2478 Cyg |VB A (B 17.1mpg, 12", 149{deg}, 1993). V2486 Cyg |VB A (B 11.5m, 21", 248{deg}, 1998). V2498 Cyg |Multiperiodic, P2 = 0.094d. V2500 Cyg |Multiperiodic, P2 = 0.0677332d. V2517 Cyg |VB A (B 14.1m, 5", 84{deg}, 1998). V2533 Cyg |Multiperiodic, P2 = 0.162486d, P3 = 0.148877d. V2534 Cyg |Multiperiodic, P2 = 0.171077d, P3 = 0.239556d. VB A (B 12.0, 3", V2534 Cyg |165{deg}, 2003; C 12.5, 10", 112{deg}, 2003; D 13.1, 16", V2534 Cyg |2931{deg}, 2003). V2536 Cyg |VB B (A 9.7m; AB 7", 270{deg}, 2003). V2541 Cyg |A twice longer period is also possible. V2544 Cyg |Apsidal motion detected. The tabulated elements are for MinI. MinII V2544 Cyg |= 2455005.5824 + 2.093799d x E. V2547 Cyg |SB. V2566 Cyg |Multiperiodic, P2 = 0.422d. Porb = 55.03d. V2581 Cyg |Multiperiodic. P2 = 0.2486d, P3 = 0.09029d. V2583 Cyg |VB A (B 19.4m, 0.6", 0{deg}, 2002). V2608 Cyg |Multiperiodic. P2 = 0.091463d. V2618 Cyg |MinII - MinI = 0.57P. V2625 Cyg |VB A (B 5", 32{deg}, 1998). V2642 Cyg |Total eclipses of the white dwarfs plus occasional small flares. V2643 Cyg |O'Connell effect. V2647 Cyg |MinII - MinI = 0.334P. V2669 Cyg |The one-day alias, P = 0.334285d, is also possible. V2690 Cyg |Porb = 0.492d. V2693 Cyg |VB B (A 14.08m; B 2.5" sf). V2699 Cyg |Multiperiodic. V2700 Cyg |Multiperiodic, 3 main frequencies. V2709 Cyg |Possible non-radial pulsations of a white dwarf. P2 = 0.017070d. V2737 Cyg |O'Connell effect. V2740 Cyg |O'Connell effect. V2760 Cyg |VB (3"). P=1.4088d is also possible. V2761 Cyg |O'Connell effect. V2762 Cyg |Porb = 12.7d; Pspin = 358.6s. V2764 Cyg |O'Connell effect. V2777 Cyg |O'Connell effect. V2786 Cyg |Blazhko effect. V2797 Cyg |P = 1.656d is also possible. V2800 Cyg |The light curve shape varies. V2813 Cyg |MinII - MinI = 0.64P. V2838 Cyg |Multiperiodic? P2 = 0.13564d is possible [81213]. V2848 Cyg |The Table presents light elements for eclipses. Multiperiodic V2848 Cyg |small-amplitude DSCT pulsations [82003]. V2850 Cyg |Multiperiodic, P2 = 0.11153d. V2855 Cyg |Multiperiodic, P2 = 0.0983128d. V2860 Cyg |Light elements for ELL type variability are presented in the Table. V2860 Cyg |Multiperiodic DSCTC oscillations with an amplitude of 0.02m are V2860 Cyg |superposed. The main harmonic: P = 0.058028d. V2863 Cyg |Multiperiodic. V2864 Cyg |VB A (13.7mG; B 15.4mG, 3", 99{deg}, 2000). V2871 Cyg |VB B (A 10.9mV; B 11.2mV, 17", 299{deg}, 2016); the range in the V2871 Cyg |Table is for combined brightness. V2879 Cyg |VB A (12.5mG; B 13.3mG, 13", 213{deg}, 2000). V2883 Cyg |Crowded, several close companions. V2887 Cyg |VB A (15.9mG; B 17.0mG, 4", 50{deg}, 2000). V2888 Cyg |VB B (A 14.35mG, B 15.2mG; AB 13", 271{deg}, 2000). V2896 Cyg |VB A (B 10.40mV, 6", 130{deg}, 2015). V2897 Cyg |VB B (A 13.5mG; B 14.0mG, 5", 210{deg}, 2000). The range in the V2897 Cyg |Table is for combined brightness. V2917 Cyg |Double-mode pulsations. P0 is presented in the Table. P1 = V2917 Cyg |0.073937974d, P1/P0 = 0.7719. V2925 Cyg |A twice longer period is also possible. V2926 Cyg |A twice longer period is also possible. V2932 Cyg |A twice longer period is also possible. V2934 Cyg |VB (15.1mG, 16.0mG, 2.5", 131{deg}, 2000). V2941 Cyg |VB B (A 13.8mJ, B 14.1mG; AB 4", 281{deg}, 2000). V2942 Cyg |VB A (16.2mG; B 16.5mG, 2.5", 146{deg}, 2000). V2945 Cyg |VB A (16.1mG; B 16.8mG, 4", 305{deg}, 2000). The variability range V2945 Cyg |in the Table can be influenced by the companion. V2949 Cyg |Multiperiodic; the second period is P = 0.11972d. VB B (13.0mG; A V2949 Cyg |12.0mG; AB 15", 45 {deg}, 2000). V2954 Cyg |VB B (A 16.0mG; B 16.3mG, 6", 222{deg}, 2000). V2962 Cyg |VB A (15.9mG; B 17.3mG, 5", 214{deg}, 2000; other companions). V2964 Cyg |VB A (13.9mG; B 14.0mG, 3", 271{deg}, 2000). The variability range V2964 Cyg |in the Table is for combined light. V2965 Cyg |VB A (14.7mG; B 17.6mG, 4", 54{deg}, 2000). V2972 Cyg |A twice longer period is also possible. V2975 Cyg |A twice longer period is also possible. V2979 Cyg |Multiperiodic; the second period is P = 0.12126d. V2980 Cyg |Multiperiodic; the second period is P = 0.13658d. V2981 Cyg |Long-term brightness variations are superposed. V2985 Cyg |MinII - MinI = 0.24P (?). V2994 Cyg |O'Connell effect [82207]. V2995 Cyg |Multiperiodic; the second period is P = 0.05356d. V3001 Cyg |VB B (A 15.8mG, B 16.0mG; AB 6", 218{deg}, 2000). V3005 Cyg |A twice longer period is not excluded. V3011 Cyg |VB A (14.1mG; B 15.2mG, 6", 79{deg}, 2000). V3014 Cyg |P = 38.0d is superposed. V3015 Cyg |MinII - MinI = 0.41P. V3018 Cyg |VB A (10.4mG; B 12.5mG, 14", 92{deg}, 2000). V3020 Cyg |O'Connell effect. V3023 Cyg |VB A (13.8mG; B 16.4mG, 4.5", 94{deg}, 2000). V3024 Cyg |O'Connell effect. V3029 Cyg |VB A (15.1mG; B 17.0mG, 5", 18{deg}, 2000). V3038 Cyg |A twice longer period is not excluded. V3041 Cyg |Multiperiodic; the second period is P = 0.15328d. V3042 Cyg |Eccentric orbit? V3043 Cyg |MinII - MinI = 0.61P. V3048 Cyg |A twice longer period is not excluded. V3051 Cyg |O'Connell effect. V3052 Cyg |VB B (A 16.40mG, B 16.44mG; AB 3.5", 29{deg}, 2000). A twice longer V3052 Cyg |period is not excluded. V3072 Cyg |VB A (15.0mG; B 16.6mG, 8", 348{deg}, 2000). V3073 Cyg |VB A (B 13.08mV, 26", 254{deg}, 2015). V3076 Cyg |Mira type and range 14.4 - <17.0mV are not excluded. V3079 Cyg |VB A (13.2mG; B 13.5mG, 15", 110{deg}, 2000). V3083 Cyg |P = 85.7d is superposed. V3097 Cyg |VB A (12.9mG; B 14.3mG, 12", 241{deg}, 2000). V3101 Cyg |Porb = 0.05352d. V3124 Cyg |Double-mode pulsations. P2 is presented in the Table. P1 = V3124 Cyg |0.105302d, P2/P1 = 0.8342. V3127 Cyg |P = 65.6d is superposed. V3130 Cyg |VB A (13.9mG; B 15.8mG, 10", 297{deg}, 2000). MinII - MinI = V3130 Cyg |0.40P:. V3131 Cyg |VB A (16.0mG; B 16.4mG, 13", 260{deg}, 2000). V3134 Cyg |VB A (8.55mV; B 10.08mV, 14.5", 208{deg}, 2016; C 9.01mV, 22.5", V3134 Cyg |201{deg}, 2016). V3137 Cyg |VB A (11.9mG; B 14.7mG, 14", 58{deg}, 2000). V3139 Cyg |VB A (10.8mG; B 12.7mG, 13", 302{deg}, 2000). V3142 Cyg |VB A (10.8mG; B 12.6mG, 3", 27{deg}, 2000). V3143 Cyg |P varies? V3144 Cyg |VB A (13.3mG; B 16.0mG, 16", 335{deg}, 2000; C 16.6mG, 14", V3144 Cyg |329{deg}, 2000). V3145 Cyg |P = 60.4d is superposed. V3147 Cyg |VB A (14.4mG; B 15.2mG, 5", 73{deg}, 2000; C 16.3mG, 8", 119{deg}, V3147 Cyg |2000). The variability range in the Table can be influenced by the V3147 Cyg |companions. V3148 Cyg |Type SRB with P = 175.0d is also possible. V3154 Cyg |P = 810d is superposed. V3155 Cyg |VB A (9.88mV; B 12.89mV, 26", 332{deg}, 2017; C 13.80mV, 14", V3155 Cyg |89{deg}, 2015). V3156 Cyg |Possibly, P = 27.4d is superposed. V3168 Cyg |VB A (B 12.1mG, 8", 135{deg}, 2000). V3171 Cyg |VB B (A 11.4mG, B 11.7mG; AB 5", 75{deg}, 2000). The magnitude at V3171 Cyg |maximum in the Table is for combined brightness. alf Cyg |VB A (B 11.4m, 75.3", 106{deg}). tau Cyg |VB A (B 6.44m, G1V, A = 0.88", P = 49.80yr; C 12.20m, 29", tau Cyg |230{deg}). 0.083d <= P <= 0.125d. The range of total light tau Cyg |variation is given. ups Cyg |VB A (B 10.2m, 15.2", 220{deg}; C 10.2m, 21.5", 180{deg}). khi Cyg |VB A (B 10.8m, 158", 254{deg}). S 6 + %1e (Tc). SiO maser. P khi Cyg |var.Max = 2393559 + 405.88d*E (JD2337150 - 94000); since JD2394000 khi Cyg |- see Table. P Cyg |The appearance of the star was firstly noted in 1600, when its P Cyg |brightness was 3m. Since the XVIII century the light of the star P Cyg |varies in the range 4.6m - 5.6m vis. Radio source at the millimetre P Cyg |and centimetre wavelengths. Q Cyg |In minimum brightness varies periodically with the amplitude 0.5m: Q Cyg |Max = 2440495 + 54.99d*E; P = 64.81d is also possible. Mean level Q Cyg |of brightness varies in the range 15.2m - 15.9m B. S Del |VB A (B 56", 342{deg}). Double maxima are sometimes observed. U Del |Mean brightness var, P = 1100d. According to [08993], the period U Del |value 160d - 180d is more likely than 110d. W Del |d = 0.017P. Min II 9.79. P var. Since JD2433000 - see Table. The W Del |light curve shape var. RZ Del |VB (A var; B var, 17", 137{deg}) [03771]. TT Del |P var. Since JD2435000 - see Table. TW Del |{Delta}(m) var (0.5m + 3.4m). The light curve resembles that of RV TW Del |Tau, with Min I and Min II; the epoch of Min I is given. Min I = TW Del |2432171.1 + 118.4d*E (1947 - 1952); Min I = 2435386.8 + 115.9d*E TW Del |(1955 - 1963); during 1964 - 1970 - see Table. TX Del |P var. P = 6.166585d (JD2428000 - 36600); since JD2436600 - see TX Del |Table. TY Del |Min II 9.8. P var.Min = 2428020.399 + 1.191121d*E (JD2428000 - TY Del |38000) [00279]; since JD2438000 - see Table. TZ Del |Epoch of Min is given. VV Del |Depth of Min II 0.05m. YY Del |Min II of the depth ~0.05m is possible. P var. Min = 2425795.488 + YY Del |0.7930856d*E (JD2425000 - 34000) [01329]; since JD2434000 - see YY Del |Table. AL Del |Min II 12.4. BG Del |Min II 13.8. BK Del |P var? BR Del |Emission. BX Del |{Delta}(S) = 0. BY Del |Min II 11.8. CE Del |[Fe/H] = -0.68. CF Del |The light curve shape var? CH Del |[Fe/H] = -1.23. According to [09037], P = 0.315D. CN Del |Min II 14.6. CR Del |Min II 13.7. CS Del |[Fe/H] = -0.92. CU Del |Abrupt phase chande was noted. CW Del |P var.P = 0.58209d (JD ~2427100), P = 0.58211D (JD ~2428800); CW Del |During JD2429800 - 30600 - see Table. DG Del |The elements should be checked. DK Del |Min II 14.2. DM Del |Min II 8.80. DT Del |Epoch od Min is given. The elements are valid during JD2425480 - DT Del |6260. DX Del |[Fe/H] = -0.11. EG Del |P var. Max = 2425535.42 + 0.3248545d*E (JD2425478 - 30619) [00911]; EG Del |abrupt change near JD2432578, since then see Table. EI Del |The mean brightness var, P ~600d. EK Del |B - V: +0.29, +0.53. ES Del |Epoch of Max from [03715], [07527] contradict the given elements. ET Del |Min II 12.7. EW Del |Min II 15.5. EX Del |Min II 13.3. FI Del |Min II 14.5. FK Del |Min II 14.5. FM Del |{Delta}(S) = 0. FP Del |[Fe/H] = -1.44. FR Del |Min II 15.3. FT Del |Blazhko effect? GG Del |Min II 12.6. P var? GN Del |P var? {Delta}(m) var? GY Del |VB B (A = BD +15{deg} 4134A, SP A - F). HR Del |Porb = 0.170920d. The brightness began to increase on JD ~2439653. HR Del |Waves with maxima on JD2439752 (4.55m), 2439799 (4.64m), followed HR Del |by a sharp main Max, flat max on JD2439981 (4.09m) and final HR Del |decline. Radio source. HU Del |{mu} = 0.685", {theta} = 79{deg}. Astrometric binary (semiamplitude HU Del |of deviations 0.118", Porb = 1.52yr). II Del |[Fe/H] = -1.30. IO Del |A single outburst was observed (JD2439378 - 388). IV Del |D ~0.1d. LS Del |Min II 8.76. OO Del |MinII 18.03. A cluster foreground star. OP Del |MinII 17.33. A cluster foreground star. OR Del |VB AB (4" - 6"), SB2 Aa, Ab. OX Del |A twice longer period is not excluded. V0362 Del |P = 173d is superposed. V0369 Del |P = 642d is superposed. V0374 Del |P = 55.7d is superposed. V0376 Del |According to [g1102], P = 0.574280d. V0377 Del |VB A (16.9mG; B 17.0mG, 6", 74{deg}, 2000). V0382 Del |Blazhko effect. V0383 Del |Blazhko effect. V0386 Del |VB A (16.8mG; B 17.0mG, 2", 68{deg}, 2000). Blazhko effect. V0387 Del |VB B (A 16.2mG, B 16.7mG; AB 3", 294{deg}, 2000). V0389 Del |VB B (A 16.4mG, B 16.9mG; AB 2", 284{deg}, 2000). Blazhko effect. V0390 Del |VB B (A 16.4mG, B 16.8mG; AB 3", 97{deg}, 2000). V0391 Del |Crowded. V0393 Del |P varies? V0395 Del |Crowded. According to [g1102], P = 0.502578d. V0397 Del |Crowded. V0400 Del |VB B (A 15.7mG, B 16.9mG; AB 4", 21{deg}, 2000). V0401 Del |VB C (16.8mG; A 15.0mG, AC 3.6", 120{deg}, 2000; B 16.4mG, BC 3.1", V0401 Del |324{deg}, 2000). V0403 Del |Blended. V0404 Del |VB A (16.9mG; B 17.1mG, 3", 189{deg}, 2000). V0408 Del |Crowded. According to [g1102], P = 0.518445d. Blazhko effect? V0412 Del |VB C (17.0mG; A 15.6mG, AC 2.8", 159{deg}, 2000; B 16.5mG, BC 2.9", V0412 Del |5{deg}, 2000). According to [g1101], P = 0.528068d. V0416 Del |Blazhko effect. V0418 Del |VB B (A 12.8mG, B 16.8mG; AB 10", 154{deg}, 2000). Blazhko effect. V0421 Del |P varies. dP/dt = -0.15 x 10^{-6} d per year. V0422 Del |P varies. dP/dt = -0.19 x 10^{-6} d per year. V0423 Del |P varies? dP/dt = +0.06 x 10^{-6} d per year. V0424 Del |P varies? dP/dt = +0.04 x 10^{-6} d per year. V0425 Del |P varies? dP/dt = +0.04 x 10^{-6} d per year. V0428 Del |P varies. dP/dt = -0.13 x 10^{-6} d per year. V0429 Del |P varies? dP/dt = -0.04 x 10^{-6} d per year. V0430 Del |P varies. dP/dt = +0.04 x 10^{-6} d per year. V0431 Del |P varies. dP/dt = +0.65 x 10^{-6} d per year. V0432 Del |Close VB, the magnitudes in the Table are influenced by the V0432 Del |companion. V0433 Del |P varies? dP/dt = -0.05 x 10^{-6} d per year [g1105]. Blazhko V0433 Del |effect? [g1001]. V0435 Del |VB B (A 18.7mG, B 18.8mG; AB 3", 348{deg}, 2000). P varies. dP/dt = V0435 Del |+0.23 x 10^{-6} d per year. V0436 Del |P varies. V0437 Del |P varies? dP/dt = +0.17 x 10^{-6} d per year. V0439 Del |P varies? dP/dt = +0.04 x 10^{-6} d per year. V0440 Del |P varies? dP/dt = -0.05 x 10^{-6} d per year. V0441 Del |Brighter than other RR variables in NGC 7006; a blend? V0442 Del |P varies. dP/dt = +0.06 x 10^{-6} d per year. V0444 Del |Crowded. P varies? dP/dt = +0.04 x 10^{-6} d per year. V0445 Del |P varies? dP/dt = +0.03 x 10^{-6} d per year. V0447 Del |Crowded. The Gaia DR2 proper motion does not seem realistic. V0448 Del |P varies. dP/dt = +0.04 x 10^{-6} d per year. V0450 Del |P varies? dP/dt = -0.03 x 10^{-6} d per year. V0451 Del |P varies. dP/dt = +0.26 x 10^{-6} d per year. V0453 Del |Crowded. V0456 Del |Crowded. V0457 Del |P varies? dP/dt = -0.08 x 10{-6} d per year. V0458 Del |P varies? dP/dt = -0.04 x 10^{-6} d per year. Blended. V0459 Del |P varies? dP/dt = +0.03 x 10^{-6} d per year. V0460 Del |P varies? dP/dt = +0.04 x 10^{-6} d per year. V0461 Del |P varies? dP/dt = -0.06 x 10^{-6} d per year. V0464 Del |P varies? dP/dt = +0.06 x 10^{-6} d per year. V0466 Del |P varies. dP/dt = +0.36 x 10^{-6} d per year. V0468 Del |P varies. dP/dt = -0.12 x 10^{-6} d per year. del Del |(k - b)2 = 0.19. SB2 (Porb = 40.58d; e = 0.7). Spectra of both SB del Del |components show Am features; Fe, Ca, Sc deficiency, Sr, Y, Zr, Ba, del Del |Ce, La, Eu excess. Both components are DSCT variables; the period del Del |of the main component pulsation is 0.158d, that of the secondary is del Del |0.134d [07528]. Any of the oscillations may occasionally dominante del Del |in the combined brightness: according to [07529], Max = del Del |2439338.4444 + 0.135547d*E; according to [07530], P = 0.154991d. R Dor |VB A (B 11.9m, 34", 10{deg}; C 11.0m, 35", 130{deg}, 1933). H2O, R Dor |SiO, HC3N emission. S Dor |VB A (B 12.1m, 13"). The member of the large magellanic cloud. In S Dor |the cluster NGC 1910 and a diffuse nebula. One of the absolutely S Dor |brightest stars. Deep Min: 1891, 1900, 1930, 1940, 1955, 1964. T Dor |VB A (B 12.0m vis, 5", 13{deg}.) V Dor |At the edge of the Large Magellanic Cloud. RR Dor |In the region of the Large Magellanic Cloud. Min II 14.5. RW Dor |In the region of the Large Magellanic Cloud.Cloud non-member. P var RW Dor |[09036]. Min II 11.2. RX Dor |In the region of the Large Magellanic Cloud. Cloud non-member? SW Dor |In the region of the Large Magellanic Cloud. Cloud non-member. P SW Dor |var [09036]. SX Dor |In the region of the Large Magellanic Cloud, Cloud non-member. SX Dor |{Delta}(m) var. SY Dor |In the region of the Large Magellanic Cloud. According to [09036], SY Dor |variability is doubtful. SZ Dor |In the region of the Large Magellanic Cloud, cloud non-member. TY Dor |In the region of the Large Magellanic Cloud, cloud non-member. UU Dor |In the region of the Large Magellanic Cloud,cloud non-member. UV Dor |In the region of the Large Magellanic Cloud,cloud non-member. UX Dor |In the region of the Large Magellanic Cloud, cloud non-member. XX Dor |In the region of the Large Magellanic Cloud, cloud non-member. XX Dor |[Fe/H] ~-1.3. ZZ Dor |In the region of the Large Magellanic Cloud, cloud non-member. AA Dor |d = 0.02P. Min II 11.21. BE Dor |In the field of the Large Magellanic Cloud. BF Dor |Min II = 13.2. alf Dor |VB A (B 4.3m, A = 0.2125", P = 13.00yr.) The range of combined alf Dor |brightness variations is given. bet Dor |P var. Current elements are given. T Dra |ADS 10937 A (B = UY Dra, optical, 16", 222{deg}). U Dra |P var. Mean elements are given. W Dra |P var. Max = 2416748 + 257.11d*E (JD2416750 - 21390); Max = 2430826 W Dra |+ 262.11d*E (JD2421390 - 30820); Max = 2439962 + 268.87d*E W Dra |(JD2430820 - 40490); since JD2440490 - see Table. Y Dra |According to visual observations, 7.8m - 15.0m. Z Dra |Min II 11.0. P var. Min = 2430973.314 + 1.3574176d*E (JD2428460 - Z Dra |33300); Min = 2433268.708 + 1.357440d*E (JD2433300 - 43500); since Z Dra |JD2443500 - see Table. RR Dra |d = 0.015P. Min II 10.1. P var. Before JD2439000 Min I = RR Dra |2433390.458 + 2.83123d*E [01001]; since JD2440000 - see Table. RS Dra |During JD2436012 - 37584 P = 145.3d. {Delta}(m) and the light curve RS Dra |share vary strongly. RW Dra |P var. Mean elements are given. Composite Blazhko effect; Pi = RW Dra |93.95P = 41.61d; Pi1 = 280P; Pi2 = 6140P; Pi3 = 3400P [01585]. RW Dra |0.11P <= M - m <= 0.32P. {Delta}(S) = 3. RX Dra |Min II 10.3, d II = 0.009P. RZ Dra |Min II 10.38. P var. Min = 2429448.787 + 0.55087668d*E (1907 - RZ Dra |1968) [03822]; since 1968 - see Table. SU Dra |P var. Before 1955 Max hel = 2420605.762 + 0.66041890D; since 1955 SU Dra |- see Table. [Fe/H] = -1.39. SW Dra |{Delta}(S) = 3.5. SX Dra |d = 0.035P. Min II 10.0. P var. Min I = 2432273.276 + 5.1692d*E SX Dra |(JD2432000 - 38000); since JD2442000 - see Table. TT Dra |P2 = 198d. TW Dra |ADS 9706 A (B 9.5m vis, 23{deg}, 3.6"). d = 0.02P; Min II 8.1. P TW Dra |var. Min I = 2433888.452 + 2.806870d*E (JD2433000 - 40000) [03825]; TW Dra |since JD2440000 - mean elements in the Table. TX Dra |Mean magnitude var, P2 = 654d. UU Dra |Mean magnitude var, P2 = 960d. UX Dra |According to [09086], the light curve may correspond to the type E; UX Dra |SB, P ~340d. UZ Dra |d = 0.01P; Min II 10.6. Possibly P = 1.65d [03827]. VW Dra |According to photoelectric observations, 6.28m - 6.32m V. WW Dra |Nonlinear term: -4.98d*10**(-9)*E2. ADS 10152A (B 9.67m, 8.2", WW Dra |5{deg}). Depth of Min II 0.08m. WZ Dra |{Delta}(m) var strongly. XY Dra |Min II 13.7. XZ Dra |P var. Before JD2438000 Max = 2427985.648 + 0.4764944d*E [00188]. XZ Dra |Epochs after JD2438000 are represented dy the elements in the Table XZ Dra |only on average. Blazhko effect; according to [01474], Pi = 78d. XZ Dra |[Fe/H] = -0.57. ZZ Dra |P var. Max = 2434509 + 274.5d*E (JD2416350 - 34600); since ZZ Dra |JD2437100 - see Table. AE Dra |{Delta}(S) = (4). AF Dra |VR var; SB? AG Dra |A soft X-ray source. Elements in the Table represent maxima in U AG Dra |band in 1974 - 1979 [09113]. AI Dra |Min II 7.16, D II = 0.17P. AP Dra |Twice shorter period is possible. AQ Dra |H{beta} spectral line is probably filled in by emission. AR Dra |Min II 11.63. AS Dra |{mu} = 0.486", P = 289{deg}. SB. {Delta}(m) var. Large spatial AS Dra |velocity. The brightness varies with the phase of the orbital AS Dra |motion. Phases of Max and Min vary from cycle to cycle. The Table AS Dra |gives Porb [03075] and the epoch of the conjunction (G4 - star is AS Dra |behind). AW Dra |P var. since JD2430500 - see Table. AX Dra |Min II 11.0. BE Dra |Min II 11.5. The spectral type is late B. BH Dra |ADS 12019A (B Am, 9.25m, 10.8", 58{deg}). Min II 8.58. BK Dra |P var.Max = 2415150.817 + 0.592019d*E (JD2414900 - 16150) [00001]; BK Dra |since JD2416940 - see Table. {Delta}(S) = 8 in Max light. BP Dra |Min II 14.7. BS Dra |Min II 9.84. BV Dra |ADS 9537 A (B = BW Dra, 16.3", 358{deg}, 1980; C 12.69m). Min II BV Dra |8.40. BW Dra |ADS 9537 B (A = BV Dra; C 12.69m). Min II 9.02. BY Dra |SB2 (Porb = 5.9750998d, e = 0.36). {mu} = 0.365", P = 150{deg}. BY Dra |Quasiperiodic variability : DM var, P var, (differential rotation), BY Dra |phase jumps. Flares up to {Delta}(U) = 1.07m. CM Dra |VB A (B SP = DC, 15.7m pg, 25.7", 22{deg}, common {mu}). {mu} = CM Dra |1.619", p = 317{deg}, {pi} = 0.068", V {nu} = -118.6km/s. Min II CM Dra |13.63. BY type variability: {Delta}(M) ~<= 0.05mV, P ~Porb. Flares: CM Dra |{Delta}(m) ~0.05. CR Dra |{mu} = 0.50", p = 168{deg}, {pi} = 0.048". CX Dra |SB, Porb = 6.69612d (with this period {Delta}(V) = 0.04m). CX Dra |Long-term cyclic variations: P ~2400d, {Delta}(V) ~0.2m. Flares CX Dra |~0.1m. An X-ray source; the reflection effect is observed. DE Dra |d = 0.017P. DG Dra |Depths respective to Max I (Phase = 0.25); Min II 0.17m; Max II DG Dra |0.01m. DK Dra |Porb = 64.44d. Epoch of Min is given. Both components show H and K DK Dra |CaII in emission. DL Dra |VB A (B 9.2m, 3.9", 318{deg}, 1982). P1 = 0.0825d, A1 = 0.028m; P2 DL Dra |= 0.0837d, A2 = 0.026m. DN Dra |P = 109S. {mu} = 0.32", P = 153{deg}. MU Dra |MinII 12.08. NO Dra |A twice shorter period is not excluded. VB (8.4mHp, 9.6mHp, 0.1", NO Dra |128{deg}, 1991). NS Dra |Min II = 11.43. MinII - MinI = 0.630: x P. NT Dra |Min II = 13.09. NU Dra |Min II = 11.06. NV Dra |Min II = 13.3 :. NW Dra |Min II = 13.45. NX Dra |Min II = 12.80. O'Connell effect. OO Dra |Min II = 11.55. Overlaid oscillations with an amplitude up to OO Dra |0.04mB and a cycle about 0.027d. OP Dra |Min II = 15.00. OQ Dra |Min II = 14.1. OR Dra |Multiperiodic, P2 = 0.0826918d. VB AB (7.88, 8.81mHp; 0.1", OR Dra |313{deg}, 1991). OV Dra |The star has a spectrum of a cataclysmic variable. OX Dra |Min II = 12.50. OZ Dra |The tabulated light elements are for eclipses. Flickering. PQ Dra |Min II = 14.05. PR Dra |Min II = 13.55. PS Dra |Min II = 13.3. PT Dra |Min II = 14.9 :. PU Dra |Min II = 12.25. PV Dra |Min II = 13.7. PX Dra |Min II = 6.88. VB A (B 10.8m, 18", 19{deg}, 2007). PZ Dra |Min II = 12.8. QS Dra |Biperiodic, P0 is tabulated. P1 = 0.0730446d. QU Dra |Min II = 14.6. QY Dra |Other possible periods: 0.603d; 1.205d (type EB). V0338 Dra |Min II = 13.8. V0339 Dra |Min II = 13.9. V0341 Dra |Min II = 10.24. V0342 Dra |Min II = 13.00. V0343 Dra |Min II = 12.6. V0344 Dra |Min II = 14.0. V0354 Dra |A magnetic white dwarf with unusual properties. Variations are V0354 Dra |probably related to spots and axial rotation. V0363 Dra |Fundamental period: see Table. First overtone: P1 = 0.40320d. V0366 Dra |Multiperiodic, P = 0.0015926d is also excited. V0368 Dra |Near the Draco dwarf galaxy; non-member. V0372 Dra |O'Connell effect. V0381 Dra |The tabulated light elements are for eclipses. Oscillations with P V0381 Dra |= 0.04407d and amplitudes 0.04mR, 0.05mV, 0.07mB, also present at V0381 Dra |both minima. V0386 Dra |VB B (A 13.5mF; B 14.0mF, 8", 16{deg}, 2000); the tabulated range V0386 Dra |is for combined brightness. V0388 Dra |O'Connell effect. V0410 Dra |VB A (B 11.7mV, 8", 37{deg}, 2006). V0413 Dra |VB AB (A 7.4m var, SB; B 10.2m, 0.5", 34{deg}, 2008). V0414 Dra |Type ELL with a twice longer period is also possible. V0416 Dra |Eclipses of about 0.2m in depth, Min = 2452368.53243 + 0.189109d x V0416 Dra |E. V0425 Dra |MinII - MinI = 0.547:P. V0432 Dra |MinII - MinI = 0.698P. V0441 Dra |A twice shorter period is not excluded. V0458 Dra |The light elements could not be confirmed [81001] using the V0458 Dra |Catalina Surveys data. V0462 Dra |P = 0.21157d is not excluded. V0472 Dra |VB B (A 13.7m; B 14.5m, 19", 199{deg}, 1999). The tabulated V0472 Dra |variability range is influenced with the companion. V0485 Dra |Type ELL is not excluded. V0486 Dra |The coordinates in [81005] refer to a neighbor star. V0506 Dra |P varies. V0534 Dra |VB A (14.4mV; B 16.1m*, 5", 359{deg}, 2000). V0546 Dra |P0 is presented in the Table. P1 = 0.351671d; P1/P0 = 0.7438. V0552 Dra |Double-mode pulsations, also P = 0.0475034d. V0555 Dra |P1 is presented in the Table. P0 = 0.551274d; P1/P0 = 0.7461. V0556 Dra |O'Connell effect. V0557 Dra |P1 is presented in the Table. P0 = 0.510745d; P1/P0 = 0.7459. V0558 Dra |P1 is presented in the Table. P0 = 0.472239d; P1/P0 = 0.7436. V0560 Dra |P1 is presented in the Table. P0 = 0.469194d; P1/P0 = 0.7432. V0561 Dra |P1 is presented in the Table. P0 = 0.484660d; P1/P0 = 0.7447. V0581 Dra |VB A (11.1mV; B 14.8mV, 1".1, 137{deg}, 2014; C 18.3mV, 6", V0581 Dra |112{deg}, 2012). kap Dra |IR excess. phi Dra |ADS 11311 ({Delta}(m) = 1.7m, 0.3", 288{deg}, 1967). A:SB, P = phi Dra |26.768d. The epoch of Max U light is given. S Equ |Min II 8.11. P var. Before JD2427000 Min = 2423746.490 + S Equ |3.4360050d*E [01140]; Min = 2437968.345 + 3.436072d*E (JD2427000 - S Equ |41000) [03432]; since JD2441000 - see Table. Gaseous streams; in S Equ |Min light H{alpha} is in emission. W Equ |Min II 12.4. P var. Z Equ |A nearby star: 12.1m. RT Equ |P var strongly. RW Equ |Strong Blazhko effect. RZ Equ |Min II 12.2:. SU Equ |Min II 16.4. SV Equ |Depth of Min II 0.16m. SW Equ |Min II 15.6. VV Equ |Porb = 0.057083d. VY Equ |Double-mode pulsations. Fundamental mode: see the Table. First VY Equ |overtone: P1 = 0.1407792d. P1/P0 = 0.7978. WW Equ |Period varies strongly, the Table presents the mean period for JD WW Equ |2454500 - 2457300. ZZ Equ |P1 is presented in the Table. P0 = 0.475184d, P1/P0 = 0.7442. gam Equ |ADS 14702A (B 11.6m, 2", 268{deg}; C 12.6m, 48", optical). The gam Equ |Table gives the pEriod of oscillations. Data on the periodicity of gam Equ |the rotational variability of light, spectrum and magnetic field gam Equ |are contradictory (17.492d, 314d, 1785.7d, 72yr). V Eri |Mean magnitude var, P2 = 1209d. W Eri |SiO, OH, H2O maser. Z Eri |P2 = 746.4d. RU Eri |Min II 9.62. RX Eri |[Fe/H] = -1.32. RY Eri |d = 0.025P. RZ Eri |d = 0.018P. The depth of Min II 0.04m pg. SV Eri |[Fe/H] = -1.83. P var. P = 0.71365272d (JD2414000 - 21000); P = SV Eri |0.71370172d (JD2421000 - 26000) [00862]; Max = 2426590.319 + SV Eri |0.7137406d*E (JD2426000 - 34000) [09195]; since JD2434000 - see SV Eri |Table. TT Eri |(B - V)Max = +0.255m. TV Eri |(B - V)Max = +0.53m. TZ Eri |d = 0.015P. P var. Min = 2426066.198 + 2.606097d*E (JD2426000 - TZ Eri |33500) [01490]; since JD2438200 - see Table. UX Eri |Min II 11.01. P var? Before JD2438500 Min I = 2434368.570 + UX Eri |0.4452820d [02494]; since JD2438500 - see Table. UY Eri |The shape of the light curve var. [A/H] = -1.6. VW Eri |Alternating P1 = 83.4d, P2 = 93.3d. Halo population. WW Eri |Min II 11.2. YY Eri |Min II 8.72. P var. Min I = 2433617.5198 + 0.321496212d*E YY Eri |(JD2433000 - 41500) [03850]; since 2441500 - see Table. X-ray YY Eri |source. ZZ Eri |Min II 14.4. AN Eri |Min II 14.9. AO Eri |d = 0.04P. AS Eri |Min II 8.42. X-ray source. BB Eri |(k - b)2 = 0.13. BC Eri |Min II 11.26:. BK Eri |{Delta}(S) = 8. P var. BL Eri |The elements should be checked. BM Eri |P > 20000d; D = 321d; d = 270d. Only one Min was observed. Outside BM Eri |Min, according to [05828], {Delta}(V) = 0.2m, Max = 2440643.0 + BM Eri |30d*E. BQ Eri |Min II 10.9. BV Eri |Min II 8.42. dII = 0.06P. BW Eri |Min II 9.72. BY Eri |(k - b)2 = 0.06. BZ Eri |Min II 9.21. CC Eri |SB. {mu} = 0.310", P = 169{deg}, Pi = 0.083". Photometric P is CC Eri |close to Porb. X-ray source. CI Eri |VB (9.9m, 11.2m, 2", 106{deg}). CO Eri |Min II 9.1. CS Eri |(k - b)2 = 0.03. CT Eri |Min II 10.27. CW Eri |Min II 8.86, DII = 0.10P. DL Eri |P0 - see Table; P1 = 0.118795d [09206]; P2 = 0.0968d [09207]. DM Eri |ADS 3380 (5.1m, 5.4m, 0.3", 161{deg}). Duplicity was observed only DM Eri |in 1877 and 1923. DO Eri |Epoch of Min is given. Oscillations with P ~6.14 Min, 7 different DO Eri |frequencies have been found. Beat phenomenon, PB = 12.25d +-0.47d. DO Eri |Max of the oscillation amplitude almost coincides with Max of the DO Eri |magnetic field, the amplitude varies with Prot. Combined amplitude DO Eri |of oscillations 0.062m B. DS Eri |Min II 10.3. P var. Min = 2423147.25 + 0.827737d*E (JD2414869 - DS Eri |23150); during JD2423150 - 31320 - see Table. DW Eri |ADS 3409 B (A 6.72m, G8III; B 9", 317{deg}). DY Eri |ADS 3093 C (A 4.43m V, K1V; B 9.51m V, DA, 82", 105{deg}; BC A = DY Eri |7", Porb = 252.1yr). {mu} = 4.05", P = 212{deg}. X-ray source. DZ Eri |Epoch is given for Max (y), Min (He I). P = 3.67d is possible. EF Eri |2A0311 - 227. VB A (B 15.8m, 18", 260{deg}). Epoch of narrow Min in EF Eri |IR light is given. The complex phenomenon of eclipses is described EF Eri |in [04041]. Oscillations with P ~20.2 and 13.7 Min. [09211]. EF Eri |Flickering. EG Eri |Epoch of Min in Y light is given. EH Eri |ADS 3305 A (B 10.8m, 1.45", 60{deg}, 1917). HV Eri |Type RRC: is also possible. KP Eri |A twice shorter period is not excluded. VB (A 9.3m; B 9.6m, 0.8", KP Eri |154{deg}, 1991). KS Eri |O'Connell effect. KU Eri |Multiperiodic. SB. KV Eri |Min II = 12.92. P varies. dP/dt = -0.20x10^(-5) d/yr. KW Eri |Min II = 13.85. KX Eri |Min II = 13.5. KZ Eri |Min II = 11.54. LL Eri |Amplitude(Min II)= 0.09mag. LR Eri |Blazhko effect, P = 122d [80153]. LT Eri |Eclipses with an amplitude about 1.6m. LU Eri |Min II = 17.7. LW Eri |Min II = 12.8. MM Eri |SB2, Porb = 13.5601d. VB AB (11.0m, 11.2m, 0.8", 79{deg}). MQ Eri |Min II = 12.7. NN Eri |Blazhko effect, P = 335.29d. NP Eri |Blazhko effect [81005]. NX Eri |P0 is presented in the Table; P1 = 0.354824d. OX Eri |Repeated outbursts in 2014, with intervals increasing approximately OX Eri |from 10 to 20 days. gam Eri |ADS 2904 A (B 12.4m, 53", 242{deg}). lam Eri |Shell features are sometimes present in the spectrum. mu. Eri |SB, Porb = 7.35886d. Pulsational or rotational variations: P = mu. Eri |1.62592d, multiperiodic. nu. Eri |SB? P2 = 0.1735079d. Beat effect. omi 1 Eri |P0 - see Table. P1 = 0.1291d. tau 4 Eri |ADS 2472 A (B 9.9m, 6", 288{deg}; C 11m, 40", 99{deg}). tau 9 Eri |SB1 (Porb = 5.954d). P = 1.2135d is not excluded. S For |VB (9.2m, 9.3m, 0.28", 358{deg}, 1964). Found unusually bright only S For |on one night by three experienced observers in europe; harvard S For |photographs of the same night show it in normal brightness. V For |(B - V)Max = +0.26. W For |Min II is observed. RX For |(k - b)2 = 0.06. RY For |(B - V)Max = +0.535. SS For |(k - b)2 = 0.09. SW For |{Delta}(S) > 10:. SY For |SB2 [M+ pec(eq)]. TZ For |SB2. Possible P values: 37.805d; 44.18d; 50.46d; 75.61d. DI = 1d. AV For |VB AB (A 8.8m; B 10.0m, 1.5", 24{deg}, 1962; C 10.8m, 35", AV For |102{deg}, 1931). AZ For |P0 is tabulated. P1 = 0.58823d. BF For |VB A (B 11.0m, 2", 170{deg}, 1991). BI For |P varies? Light elements for JD 2454000 - 2455165 are presented in BI For |the Table. R Gem |VB A (B 11.4m pg, 173", 200{deg}, 1910). S 3.5/6e- S 6.5/6-. S Gem |VB A (B 11.1m, 70", 122{deg}). T Gem |S 3/4e. U Gem |Min = 2437638.82685 + 0.17690602d*E + 5.4d*10**(-12)*E**2 [09215]. U Gem |Depth of Min 0.5m - 1.0m. Spectrum description [09216]. V Gem |P var. Max = 2407750 + 276.2d*E (JD2407700 - 15500); Max = 2415729 V Gem |+ 278.3d*E (JD2415600 - 21600); Max = 2421839 + 269.8d*E (JD2421700 V Gem |- 26500) [00458]; Max = 2432580 + 281.3d*E (JD2427500 - 32600); Max V Gem |= 2434739 + 269.8d*E (JD2432600 - 35800); since JD2435800 - see V Gem |Table. W Gem |P var. Max = 2429815.990 + 7.914553d*E (JD2413200 - 31700); since W Gem |JD2431700 - see Table. [A/H] = 0.2. There is possibly faint blue W Gem |companion. RR Gem |P var. Max = 2415219.734 + 0.39729235d*E (JD2412000 - 18000); Max = RR Gem |2418278.900 + 0.39727274d*E (JD2418000 - 21000); Max = 2422865.229 RR Gem |+ 0.39724027d*E (JD2421000 - 25000) [09217]; Max = 2427150.267 + RR Gem |0.3972596d*E (JD2426200 - 27850); Max = 2434806.289 + 0.3973103d*E RR Gem |(JD2428200 - 34900) [02392]; since JD2436000 - see Table. Blazhko RR Gem |effect, PB = 48d [03618], PB = 37d [09221]. {Delta}(S) = 3. RW Gem |VB A (B 11.04m, 20", 105{deg}; C 11.84m, 100", 120{deg}). Min II RW Gem |9.74; d = 0.02P. RX Gem |VB A (B 12.65m, 45", 215{deg}). Min II 9.28; d = 0.004P. P var. Min RX Gem |I = 2417970.0 + 12.20868d*E (JD2415000 - 27500) [07534]; since RX Gem |JD2427600 - see Table. There is a square term in the elements given RX Gem |in the Table: +2.25d*10**(-7)*E**2. Luminous gaseous ring surrounds RX Gem |the primary component of the system [07535]. RY Gem |VB A (B 12.30m, 45", 240{deg}). Min II 8.75; d = 0.023P. P var. Min RY Gem |I = 2418015.333 + 9.300876d*E (JD2418000 - 33000) [08653]; since RY Gem |JD2433000 - see Table. Component of A type is surrounded by a RY Gem |luminous gaseous ring. RZ Gem |VB. P var. Max = 2429632.453 + 5.529716d*E (JD2415000 - 32400); RZ Gem |since JD2432400 - see Table. SS Gem |9.9m <= Min II <= 10.7m. SU Gem |P var. Min I = 2429204 + 50.12d*E (JD2429200 - 355) [00310]; Min I SU Gem |= 2437772.5 + 50.39d*E (JD2437739 - 39850); Min I = 2439856.6 + SU Gem |50.10d*E (JD2439850 - 40680); since JD2440680 - see Table. Mean SU Gem |brightness varies with the elements: Min = 2437953 + 680d*E; M - m SU Gem |= 264d. Amplitude of shortperiodical variations is 0.3m - 0.9m. SW Gem |Min brightness epoch is given. SX Gem |Min II 11.3; d = 0.05P:. TX Gem |Depth of Min II 0.04m; d = 0.017P:. UV Gem |VB A (B 19.5m, 7", 285{deg}). WW Gem |Min II 10.3. WY Gem |May be an eclipsing system similar to VV Cep. Atmospheric eclipse WY Gem |began probably in 1960 - 61, the mean phase of it being in 1968 WY Gem |[05730]. Variable magnetic field [01591,04498]. Intrinsic WY Gem |variability of blue component is also possible [07536]. YY Gem |VB C (A 1.99m, B 2.85m, a = 6.06", P = 306.3 y; C 73", 165{deg}, YY Gem |1925). Min II 9.59; Min II - Min I = 0.50P; D = 0.000P. X-ray YY Gem |source. P const [08655]. Both components are probably UV Cet type YY Gem |variables. Flare amplitude in the integrated light of the system YY Gem |reaches 0.3m V, or 1.8m U [09227]. AA Gem |[A/H] = 0.0. AC Gem |Min II 11.3. P var. Min I = 2433649.30 + 1.661795d*E (JD2415000 - AC Gem |36000) [01530]; since JD2430100 - see Table. AF Gem |VB A (B 14.8m, 2", 0{deg}). Min II 10.67. There is a square term in AF Gem |the elements given in the Table: -1.71d*10**(-10)*E**2. AH Gem |Min II 14.8:. AI Gem |Min II 14.0. AL Gem |Min II 9.85. AN Gem |Min II 13.3:; d = 0.037P. AU Gem |OH emission. AV Gem |Min II 12.8:. AY Gem |Min II 10.9. AZ Gem |Min II 12.4. BB Gem |VB A (B 12m, 25", 270{deg}). BP Gem |P var. Max = 2434120 + 243.9d*E (JD2418700 - 36600); since BP Gem |JD2436600 - see Table. BT Gem |Min II 14.0:. CI Gem |UG? CM Gem |Min II 15.0. DL Gem |VB A (B 13.1m, 18", 180{deg}). DN Gem |VB A (B 13.5m, 12", 16{deg}; C 12.0m, 80", 99{deg}). DP Gem |Min II 14.0. RRC? P = 0.2792d? DX Gem |P var. Max = 2433182.876 + 3.136226d*E (JD2425000 - 34000); Max = DX Gem |2435554.199 + 3.136955d*E (JD2434000 - 36500) [08300]; since DX Gem |JD2436500 - see Table. EF Gem |P var. Min = 2428108.49 + 6.10222d*E (JD2428500 - 42800) [00407]; EF Gem |since JD2442800 - see Table. EL Gem |Min II 13.6. EN Gem |Min II 13.8. EW Gem |P var. Max = 2428495.686 + 0.523750d*E (JD2428100 - 30780); since EW Gem |JD2430780 - see Table. EY Gem |Min II 13.0. FT Gem |Min II 14.1. GP Gem |Min II 13.5. GR Gem |15.6 <= Min II <= 15.9. GW Gem |Min II 10.68. GX Gem |Min II 11.3. GZ Gem |P = 1.225290d? HH Gem |Min II 13.8. HR Gem |Min II 11.7. HY Gem |Min II 17.5. II Gem |P = 223d? IP Gem |Min II 14.5. IR Gem |In supermaxima there are superhumps with P = 102 Min [09232]. IZ Gem |D >= 0.24d. KN Gem |The minor planet (123) Brunhild. KQ Gem |Min II 14.6. KU Gem |d = 0.05P. KV Gem |Epoch of Min of brightness is given. EW type is possible according KV Gem |to the spectrum [09037]. KZ Gem |The cycle may be 129d. LM Gem |d = 0.02P. LX Gem |Red. MO Gem |Red. MP Gem |VB. MU Gem |Min II 14.9. MZ Gem |Min II 16.7. NQ Gem |In the spectrum of the carbon star the hydrogen emission lines and NQ Gem |ultraviolet continuous emission appeared in February 1970 [06348]. NY Gem |HD 47396 (Pec) = S 5438 = CSV 798 = CSV 6468. In the chart in NY Gem |[00156] the position of the variable is wrong. OS Gem |Oscillations with the period P1 given in the Table are superimposed OS Gem |by oscillations with the period P0 = 0.070d and smaller amplitude. OS Gem |P1/P0 = 0.78. V0345 Gem |The variability may be due to the fainter (B) component. V0371 Gem |Erroneous identification with HD 256211 in the literature is due to V0371 Gem |large positional errors in the HD catalogue for this field. V0372 Gem |The depth of MinII is 0.22. V0373 Gem |MinII 9.39. V0375 Gem |MinII 13.4. V0383 Gem |VB A (B 15.2mV, 12", 212{deg}, 1998; more companions at larger V0383 Gem |distances). The tabulated amplitude was influenced by the V0383 Gem |companions. V0396 Gem |Min II = 10.37:. V0399 Gem |Min II = 10.44. V0400 Gem |Min II = 11.90. V0401 Gem |Min II = 12.55. V0402 Gem |Min II = 12.35. V0403 Gem |Biperiodic, second period 0.1534d. V0404 Gem |Min II = 12.9. V0405 Gem |Min II = 10.97. V0409 Gem |Min II = 13.9. V0410 Gem |Min II = 11.06. V0411 Gem |The depth of MinII is 0.26 mag (*). V0412 Gem |The depth of MinII is 0.5 mag (*). V0413 Gem |The depth of MinII is 0.40 mag (*). V0414 Gem |Min II = 10.71. V0415 Gem |Min II = 12.8. V0416 Gem |Min II = 13.1. V0418 Gem |Intermediate polar. Porb is tabulated, Pspin = 480.7080s. V0421 Gem |Min II = 15.3. V0422 Gem |Min II = 8.28. V0425 Gem |Min II = 12.78. V0428 Gem |Min II = 11.07. V0432 Gem |Type EW with a twice longer period is also possible. V0435 Gem |The depth of MinII is 0.35 mag (*). O'Connell effect. V0439 Gem |A twice longer period is not excluded. V0455 Gem |Multiperiodic. V0483 Gem |P0 is presented in the Table. P1 = 0.1173070d; P1/P0 = 0.7685. V0487 Gem |The magnitude range in the Table is for BY-type brightness V0487 Gem |variations. Five flares were also detected. V0506 Gem |P1 is presented in the Table. P0 = 0.551687d; P1/P0 = 0.7465. V0512 Gem |The ephemeris of eclipses is presented in the Table. Pulsations: V0512 Gem |peak-to-peak amplitude 0.36mV, P = 0.08494573d, M - m = 0.40P. V0514 Gem |VB A (B 10.33m, 8", 358{deg}, 2012). V0517 Gem |P1 is presented in the Table. P0 = 0.481358d; P1/P0 = 0.7452. V0520 Gem |P1 is presented in the Table. P0 = 0.540394d; P1/P0 = 0.7468. zet Gem |VB A (B 11.46m, 87", 84{deg}; C 7.56m, 97", 350{deg}). P var. Max = zet Gem |2410640.42 + 10.15477d*E (JD2394600 - 2407150); Max = 2422366.187 + zet Gem |10.15288d*E (JD2407150 - 22300); Max = 2426802.918 + 10.15172d*E zet Gem |(JD2422300 - 34500) [02392]; since JD2434500 - see Table. All the zet Gem |observations are satisfied also by the elements: Max = 2443785.444 zet Gem |+ 10.150135d*E - 5.24d*10**(-7)*E**2 [09029]. May by a DCEPS type zet Gem |variable. eta Gem |VB A (B 8.8m, GO III - IV, 1.60", 269.4{deg}, 1977). SB1 (P = 2983d eta Gem |[09236]). Epoch of Min brightness is given. The deepest minima eta Gem |(corresponding to the middles of the descending branches of the eta Gem |radial velocity curve) are satisfied by the elements: Min = 2429355 eta Gem |+ 2984d*E [01551]. mu. Gem |VB A (B 9.8m, 122", 141{deg}). sig Gem |VB A (B 10.8m, 182", 316{deg}); SB1 (P = 19.603d [09238]). There is sig Gem |a Min II on the light curve; Min II sometimes disappears and sig Gem |sometimes becomes deeper then Min I. Min II - Min I = 0.5P. U Gru |Depth of Min II 0.05m. d = 0.011P. W Gru |P var. Nonlinear term: +7.84d*10**(-9)*E**2. Min II 10.0. X Gru |d = 0.008P. Min II 10.69. P var. Current elements are given. Z Gru |{Delta}(S) = 12:. The shape of the light curve and P are strongly Z Gru |variable. RS Gru |(k - b)2 = 0.22. RT Gru |(k - b)2 = 0.02. Blazhko effect. RV Gru |(B - V)Max = +0.93. Min II 11.4. RW Gru |{Delta}(S) = 10. Blazhko effect. RX Gru |Min II 10.7. RY Gru |Superposition of irregular variations? During JD2434513 - 517 RY Gru |precalculated minima were not observed. RZ Gru |A description of light changes [02809]. UW Gru |[Fe/H] = -1.6. VW Gru |P >= 260d? VY Gru |P > 160d. VZ Gru |RR type is also possible. AK Gru |Elements should be checked. AP Gru |P var. Mean elements JD2427992 - 36848 - see Table. during AP Gru |JD2434250 - 36848 Max = 2434337.337 + 0.5082945d*E. AR Gru |Min II 10.6. AV Gru |P >= 160d is possible. AW Gru |Min II? JD2436818. BC Gru |Min II 10.3. RRC type is possible. BD Gru |Min II 14.9. BH Gru |Min II 15.2:. DV Gru |A twice longer period is not excluded. DW Gru |VB (A 11.8mV; B = GSC 8449.00117, 13.0mB, 13", 334{deg}, 1999; DW Gru |component A varies? [79063]). Combined magnitudes are tabulated. DW Gru |MinII - MinI = 0.44P. EN Gru |P varies. dP/dt = +0.55 x 10^(-5) d/yr. ER Gru |Blazhko effect. ES Gru |Period varies? EX Gru |The coordinates in [81005] are wrong. FH Gru |The range and elements in the Table are for ASAS-SN data (JD FH Gru |2456779 - 2458753). During JD 2451875 - 2455119 (ASAS-3 data), P = FH Gru |274.0d, 8.97mV - 11.91mV. FO Gru |Double-mode pulsations. P0 is presented in the Table. P1 = FO Gru |0.0889176d, P1/P0 = 0.7731. pi. 1 Gru |VB A (B 10.9m, G0V, 2.7", 202{deg}). T Her |VB A (B 10m, 67", 321{deg}). U Her |SiO, OH, H2O maser. W Her |ADS 10121 A (B 14.2m, 6", 334{deg}). X Her |P2 = 746d. Z Her |VB A (B ro > 10"). Min II 8.18. nonlinear term: Z Her |-6.19d*10**(-10)*E**2. RU Her |SiO maser. The spectrum in Min light is composite; a companion? RU Her |[03502]. RX Her |Min II 7.74. SW Her |B - V; +0.12, +0.40. P var. Before 1921 Max = 2416687.018 + SW Her |0.4928864d*E. SX Her |[Fe/H] = -1.8. SY Her |On period variations see [08699]. SZ Her |Min II 10.10. P var. Min = 2430766.8390 + 0.818096d*E + SZ Her |0.0165d*sin(0.010465{deg}*E + 180{deg}) [05749]. The Table gives SZ Her |current elements satisfac - tory after JD2438000. TT Her |Min II 9.89. The light curve shape var. P var. Before JD2430000 Min TT Her |= 2425433.627 + 0.9120846D [02389]; Min = 2434525.2572 + TT Her |0.9120800d*E (JD2430000 - 40000) [03504]; since JD2440000 - see TT Her |Table. TU Her |d = 0.022P. P var. Before JD2435000 Min = 2424381.416 + TU Her |2.2671303d*E - 854d*10**(-11)*E**2 [09240]; Min = 2437462.3909 + TU Her |2.2669718d*E (JD2435000 - 38000) [09241]; Min = 2443324.70097 + TU Her |2.2669385d*E (JD2438000 - 44000) [08593]; since JD2444000 - see TU Her |Table. TW Her |[Fe/H] = -0.47. TX Her |Min II 8.97, DII = 0.11P. P var; periodic term: TX Her |+0.0081d*sin(0.042{deg}*(E + 7255)). UU Her |[Fe/H] = -1.27. There was alternation of periods 90d and 71d UU Her |[00310]; the period 45d [03507] was also noted. During JD2443611 - UU Her |44161 - see Table. Epoch of Min is given. UX Her |Min II 9.11. P var. Before JD2429000 Min = 2419876.467 + UX Her |1.5488598d*E [00279]; Min = 2429987.420 + 1.5488513d*E (JD2429000 - UX Her |38000) [03671]; since JD2438000 - see Table. VW Her |VB A (B 17.3m, 18", 120{deg}. VX Her |{Delta}(S) = 5. P var; nonlinear term: -0.00745d (E:10000)**2. VX Her |According to [03369], a member of an eclipsing binary system. VZ Her |[Fe/H] = -0.9. P var. P = 0.44031880d (JD2415000 - 22000) [05738]; VZ Her |Max = 2425004.4590 + 0.44032394d*E (JD2422000 - 27000); Max = VZ Her |2425004.4456 + 0.44032631d*E (JD2427000 - 36000) [03506]; since VZ Her |JD2436000 - see Table. WW Her |VB A (B 15.6m, 7.4", 148.5{deg}, white). WX Her |Twice longer P is not excluded. AC Her |P var. The Table gives current elements valid since JD2442000. Mean AC Her |P = 75.4619d [01754]. The magnitude in Max varies with {Delta}(m) = AC Her |1.6m [00368]. AD Her |VB A (B 11.97m, 5", 189{deg}). d = 0.033P. Min II 9.79. AF Her |P var. Before JD2426950 P = 0.630336d; since JD2426950 - see Table. AF Her |The shape of the light curve var. AG Her |P var. Max = 2422935.584 + 0.6494378d*E (JD2418210 - 26952); since AG Her |JD2426952 - see Table. AH Her |Porb = 5.9d:. Oscillations during outbursts: 24s <= P <= 39s, AH Her |{Delta}(m) <= 0.003m [09251]. Flicckering in Max And Min up to 0.4m AH Her |in 2 - 8 minutes [09252]. AK Her |ADS 10408 A (B 12.0m, 5", 323{deg}). Min II 8.64. Min II - Min I = AK Her |0.505P. dII = 0.07P. P var. Before JD2421200 Min = 2421200.549 + AK Her |0.42152207d*E; Min = 2421200.549 + 0.42152083d*E (JD2421200 - AK Her |24950); Min = 2424949.555 + 0.42152061d*E (JD2424950 - 30000) AK Her |[01760]; Min = 2430939.368 + 0.42152362d*E (JD2430000 - 41500); AK Her |since 2441500 - see Table. The shape of the light curve var. AM Her |3U 1809 +50. Lx(soft)/Lopt ~15. Emissions of H and KCaII, H, HeI, AM Her |HeII, etc. In the spectrum. Epoch of Min I in V light is given. The AM Her |period shows complex variations. The phase of Min I in U light is AM Her |0.30p, in B 0.15P, in R 0.05P. Min I is probably due to an eclipse AM Her |of a hot spot and the gas flow near the surface of the white dwarf AM Her |by the white dwarf itself. The depth of Min I is up to 0.7m. Min II AM Her |with the depth up to 0.4m (sometimes absent), Min II - Min I = AM Her |0.55P. Min II coincides in phase with the X-ray eclipse. High and AM Her |low states (b ~13.0m and B ~15.0m on average); in the high state AM Her |there are variations with {Delta}(m) ~0.3m on the time scale >= AM Her |200d; the duration of low states is 130d - 700d [09258] or less. AM Her |During low states the depth of minima is small. Flickering up to AM Her |0.8mV in several minutes or dozens of seconds; X-ray flickering on AM Her |the time scale of ~10s not correlating with optical flickering. The AM Her |magnetic field ~1*10**7 G at the equator, ~2*10**7 G on poles. AM Her |Variable circular (from +3% to -9%) and linear (up to 7%) AM Her |polarization. IR excess at {lambda} 10 mkm. AP Her |P var strongly. P = 10.400d (JD2415000 - 19000:); P = 10.3970d AP Her |(JD2423700 - 24700:); P = 10.4260d (JD2424700 - 25300); P = AP Her |10.4338D (JD2425800 - 27000); P = 10.3945d (JD2427000 - 27400); P = AP Her |10.4277d (JD2433000 - 33850); P = 10.3898d (JD2433850 - 34850); P = AP Her |10.4209d (JD2434850 - 35600); P = 10.3715d (JD2435600 - 37200); AP Her |DURING JD2437200 - 43800 - see Table. The light curve shape var. AP Her |[A/H] = -0.8. AR Her |P var in a complicated way. Max = 2424794.274 + 0.4700234d*E (1905 AR Her |- 1954) [06535]; Max = 2439692.683 + 0.469975d*E (1954 - 1967) AR Her |[05274]; since 1967 - see Table. Blazhko effect, Pi = 31.5489d AR Her |[03555], {Delta}(m) var (0.9m -: 1.8m pg) [02168], (M - m) var. AR Her |{Delta}(S) = 6. AT Her |The star is bright on one plate (JD2418209). Besides that, 11.8m - AT Her |12.25m. AW Her |VB A (B 10" - 20"). d = 0.03P. BB Her |P var. P = 7.507696D (JD2418924 - 30700); since JD2430700 - see BB Her |Table. [A/H] = +0.3. BC Her |P var. Before JD2432000 Min = 2426242.372 + 3.08752d*E [09262]; BC Her |since JD2436000 - see Table. BD Her |P var. P = 0.4739135d (JD2426540 - 29620); P = 0.4739057d BD Her |(JD2429620 - 30570); Max = 2430495.404 + 0.4739126d*E (JD2430570 - BD Her |before 1948) [09263]; since 1948 - see Table. {Delta}(S) = 0.8. BL Her |P var. P = 1.3074604d (JD2415000 - 35000); since JD2435000 - see BL Her |Table. Another possible representation: Max = 2434999.402 + BL Her |1.307457d*E - 3.9d*10**(-10)*E**2 (JD2415000 - 42000). [Fe/H] = BL Her |0.0. BO Her |d = 0.015P. Min II 10.8. P var? CC Her |P var. Min = 2426120.415 + 1.7340314d*E (JD 2425790 - 31265); Min = CC Her |2431265.288 + 1.7340460d*E (JD2431265 - 36000) [02389]; Min = CC Her |2439668.342 + 1.73398d*E (JD2436000 - 39600); since JD2439600 - see CC Her |Table. CD Her |The chart in [06286] is wrong. CE Her |[A/H] = -1.8. CK Her |P var? Max = 2429231.234 + 0.519201d*E (JD2429231 - 877) [00332]; CK Her |during JD2436041 - 37955 - see Table. CO Her |P2 = 600d. Sometimes does not vary for 150d. CP Her |Superimposed waves, 50d - 100d. CT Her |The depth of min II 0.05m. P var. Min = 2430904.431 + 1.786337d*E CT Her |(JD2426480 - 35000) [03567]; Min = 2439355.666 + 1.7863645d*E CT Her |(JD2435000 - 39500) [00001]; Min = JD2441499.3307 + 1.7863891d*E CT Her |(JD2439500 - 42500) [08593]; since JD2442500 - see Table. DE Her |P var. Max = 2425754 + 171.2d*E (JD2425754 - 30890); Max = 2430889 DE Her |+ 175.3d*E (JD2430890 - 36150); during JD2436150 - 38140 - see DE Her |Table. DF Her |Elements are valid since JD2425900. DH Her |d = 0.024P:. Min II 9.5. DI Her |Min II 8.95, DII = 0.03P, Min II - Min I = 0.77P (1966 - 1978). DI Her |Apsidal motion: P = 29000yr +- 4000yr; Min II = 2442241.4602 + DI Her |10.5501751d*E. A considerable discrepancy between the observed and DI Her |the theoretical rate of apsidal motion. DK Her |P var. DL Her |Blazhko effect, Pi = 33.6d, 11.0m <= m Max <= 11.3m. P var. DL Her |{Delta}(S) = 5. DO Her |Close to V362 Her. DQ Her |VB A (B 18.17m, F, 3.5", 132{deg}, optical?). Nebula, R = 10.5" DQ Her |(H{alpha}, 1981). After the main Max of the Nova a deep Min 13.0m DQ Her |(JD2426925) and a flat secondary Max 6.7m (JD2427065) were DQ Her |observed. Eclipsing variability: 14.61m - 18.08m, Min HeI = DQ Her |2434954.9445 + 0.193620877d*E [09280]. D = 0.20P, d = 0.000P. The DQ Her |light curve shape and {Delta}(M) var. Oscillations: Max HeI = DQ Her |JED2434954.785868 + 8.22521640d*10**(-4)*E - 2.8048d*10**(-16)*E**2 DQ Her |[08722], 0 <= {Delta}(m) <= 0.08m. Polarization changes with double DQ Her |oscilation period. Flickering: {Delta}(m) = 0.15m. DY Her |P var, nonlinear term: -18.6d*10**(-13)*E**2. EI Her |Red. EN Her |P var. Before JD2427000 P = 160d. ES Her |Min II 13.7. ET Her |The elements are valid earlier than JD2427200 EX Her |Red. EZ Her |The elements are valid earlier than JD2427400. FN Her |P var? FW Her |Min II 14.6. FY Her |According to the spectrum, EW type is possible. GL Her |P var? GU Her |d = 0.010P. Min II 11.8. Min II - Min I = 0.513P. GV Her |[Fe/H] = -1.41. P var. Max = 2427543.360 + 0.2914606d*E (JD2427543 GV Her |- 29728) [00152]; during JD2436041 - 38170 - see Table. GY Her |P var. Max = 2428219.623 + 0.524347d*E (JD2428219 - 727) [00152]; GY Her |during JD2436370 - 38170 - see Table. HS Her |d = 0.025P. Min II 8.63. P var; since JD2438240 - see Table. HS Her |Apsidal motion: Pi ~130yr [06538]. HV Her |d = 0.008P:; Min II 12.9:. HZ Her |Her X-1 = 4U 1656 + 35. Lx/Lopt = 2 - 60. The Table gives elements HZ Her |for light minima due to eclipsing variability and the reflection HZ Her |effect. Min I coincides with the X-ray eclipse. Shallow Min II may HZ Her |be present. The reflection effect causes variations with {Delta}(m) HZ Her |up to 1.5m. A cycle of 34.875d duration is observed in X-ray band; HZ Her |the source is faint during two thirds of the cycle. The optical HZ Her |light curve changes are observed during the 35d cycle [09283]. HZ Her |According to [06539], during JD2427543 - 657 and JD2428630 - 29789 HZ Her |the strong reflection effect was absent; the star was still varying HZ Her |with P = 1.7d and had {Delta}(m) ~0.5m, Min I = Min II. In [06546] HZ Her |it is stated that such intervals with no reflection effect, of 8d HZ Her |to 7a duration, took place for almost half the time since 1890. The HZ Her |light changes during such intervals are in the range 14.7m - 15.2m HZ Her |pg. Since 1957 intervals without the reflection effect were not HZ Her |observed. In June - July 1983 the predicted phases of high X-ray HZ Her |flux did not take place, but the reflection effect did not HZ Her |disappear [09284]. Secondary light variations: P1 = 1.0977d HZ Her |({delta}(B1) = 0.33m), P2 = 0.871173d*E ({delta}(B2) = 0.10m), P3 = HZ Her |1.623846d*E ({delta}(B3) = 0.17m) [09285]. X-ray pulsar, P = HZ Her |1.2377991s (JD2443357), dP/dt/P = (-2.9 +- 0.2)*10**(-6)/yr HZ Her |[09286], sometimes noticeable also in the optical range [06543]. HZ Her |Rapid brightness flickering. IK Her |d = 0.030P? IQ Her |Superposition of variations with shorter P and small {Delta}(m) IQ Her |[06645]. IT Her |According to the spectrum, EW type is possible. KL Her |Min II 14.7. KV Her |The light curve is characteristic of Mira Ceti stars but strongly KV Her |varies. Many irregularities. O - C: -96d, +73d. LR Her |Min II 15.4:. LS Her |The light curve shape var. LT Her |d = 0.02P. Min II 10.79. LV Her |P var? During JD2428429 - 31342 - see Table. MM Her |VB A (B 13.50m, 18", 120{deg}). Min II 9.7. {Delta}(m) of the MM Her |distorsion wave up to 0.12m. MP Her |[Fe/H] = -1.18. MS Her |Min II 13.3. MT Her |Min II 12.30. MV Her |The chart in [00156] identifies the variable erroneously; real MV MV Her |Her is marked as "C". MW Her |P var. P = 503d (1976) [09290]. During JD24668 - 29172 - see Table. MX Her |Moments of Min after JD2444000 published by different groups of MX Her |observers contradict each other. NQ Her |According to [03882], EA, 8.0 - 8.6 pg, Min II 8.4, Min I = NQ Her |2426894.433 + 0.870218d*E (JD2426894 - 34250). NR Her |Waves, P = 2.8d - 5.5d. OQ Her |Epoch of min is given. OS Her |B - V: +0.12, +0.48. OU Her |Spectral type is given according to [02198]; in BSD-G7. OX Her |{Delta}(S) = 6:. PW Her |Min II 10.1; DII ~0.3P(!). V0338 Her |Min II 10.13. P var. Before JD2437000 Min = 2433771.38 + V0338 Her |1.305732d*E [03115]; Min = 2441864.379 + 1.3057515d*E (JD2437000 - V0338 Her |43400) [08593,00001]; since JD2443400 - see Table. V0342 Her |Min II 10.7. V0347 Her |P var. Max = 2415288.21 + 0.5373619d*E (JD2415288 - 18596); since V0347 Her |JD2429495 - see Table. V0359 Her |P var. Min = 2416046.476 + 1.755754d*E (JD2416000 - 26500) [00001]; V0359 Her |Min = 2435693.47 + 1.755775d*E (JD 2426500 - 36000) [01040]; since V0359 Her |JD2443500 - see Table. V0362 Her |Close to DO Her. V0365 Her |Blazhko effect: Pi = 40.64d. P var. During JD2429037 - 36840 - see V0365 Her |Table. V0373 Her |P = 0.33d or 0.50d is possible. V0384 Her |P ~0.33d is possible. V0387 Her |Min II 13.2. V0394 Her |P var? V0395 Her |Z = 0.0643. V0396 Her |Z = 0.175. V0403 Her |Min II 16.0:. V0412 Her |Min II 15.2. V0422 Her |P var? During JD2434131 - 35991 - see Table. V0423 Her |Min II 15.0. V0426 Her |Min II 15.8. V0431 Her |P var. V0436 Her |The elements are uncertain. V0441 Her |IR excess, evidence for a circumstellar envelope. Possibly V0441 Her |non-radial pulsation. V0442 Her |P var. Max = 2434223.375 + 0.4421143d*E (JD2417447 - 36083); since V0442 Her |JD2435730 - see Table. The shape of the light curve varies. V0446 Her |Before the outburst 16.2m - 18.8m [03607]. V0451 Her |ADS 10310 A (B 10.70m, 19", 239{deg}). The epoch of Min U light is V0451 Her |given. V0458 Her |[Fe/H] = -1.65. V0463 Her |P = 54.4d is possible. V0477 Her |Min II 15.4. V0482 Her |Possibly eclipsing. V0499 Her |Blazhko effect. V0502 Her |Min II 13.5? V0510 Her |P var? V0511 Her |P var? V0513 Her |Min II 15.7. V0516 Her |Min II 17.1. V0523 Her |Elements are valid during JD2430940 - 990. V0524 Her |Twice shorter P is possible. V0527 Her |Max = 2430938.451 + 0.5188d*E (JD2430938 - 990); during JD2436308 - V0527 Her |318 - see Table. V0529 Her |Epoch of Min is given. According to [04217], P = 120d. V0533 Her |VB A (B 16m, 9.5", 0{deg}). oscillations: Max = 2443717.730281 + V0533 Her |0.0007364941d*E, A ~1% [04162]. V0551 Her |P = 4.00d/n is possible. V0552 Her |P = 3.04d/n is possible. V0554 Her |P = 4.01d/n is possible. V0557 Her |P = 8.00d/n is possible. V0570 Her |P = 0.5d or 0.33d is possible. V0578 Her |Red. V0581 Her |Several close companion. V0582 Her |VB. Red. V0583 Her |Red. V0588 Her |Possibly eclipsing. V0600 Her |SB, Porb - see Table. Variability of Vr possibly caused by BCEP V0600 Her |type pulsations: P - 0.18d. V0601 Her |Elements are valid since JD2439184. V0604 Her |Red. V0608 Her |Blazhko effect. V0615 Her |Red. V0618 Her |P var? V0624 Her |VB A (12.04m, 40"). Min II 6.35. SB2. V0637 Her |ADS 10227 A (BC 9.2m, 9.2m, 1.7", 18{deg}, 1975; BC: A = 0.28", V0637 Her |Porb = 56.56yr). V0639 Her |{pi} = 0.087". VB B (A = V647 Her, 11.36m var, dM4e; B 16", V0639 Her |268{deg}). Flares in the bands U and M pg. V0640 Her |VB A (B 14.9m, 8.5", 217{deg}; C 13.9m, 23", 221{deg}). V0641 Her |L or ISB type is also possible. V0644 Her |SB (Porb = 11.859d). V0645 Her |P ~3h - 10h, a cycle of 40d. V0647 Her |VB A (B = V639 Her, 16", 268{deg}); {pi} = 0.087". V0652 Her |P var; nonlinear term: -45.80d*10**(-10)*E**2. {Delta}(m) var. V0652 Her |Resembles PV TEL type stars but is a helium rich subdwarf. Epoch of V0652 Her |Max is given. Secondary hump at the phase 0.5P. V0654 Her |{Delta}(m) = 0.15m in white light. V0655 Her |ADS 10407 A (B 9.2m, 4.1", 144{deg}, 1971). V0657 Her |According to [02610], CST?, 11.0m. V0662 Her |Less probable P values: 0.56629d, 0.56710d, 0.56881d, 0.56970d. V0685 Her |Min II 15.8. V0687 Her |Min II 14.9. V0691 Her |Possible P values: 0.927d, 0.637d. V0697 Her |H2O, OH maser. V0699 Her |Min II 16.0:. V0717 Her |Blazhko effect? V0718 Her |Min II 14.3. V0719 Her |EW type with twice longer P is not excluded. V0720 Her |Blazhko effect? V0721 Her |Blazhko effect? V0722 Her |Min II 15.7. V0723 Her |Min II 15.5. V0728 Her |Min II 11.4. V0731 Her |Min II 13.8. Twice shorter P is not excluded. V0732 Her |Min II 13.8. V0733 Her |Min II 14.3:. V0737 Her |Blazhko effect? V0740 Her |Min II 14.4. V0741 Her |Blazhko effect? V0742 Her |Min II 14.4. V0744 Her |Vr var, P = 86.7221d (SB1? nonradial pulsatiob?). Rapid spectral V0744 Her |variability is possible: P = 2.5552d, 0.78906d. V0749 Her |P = 465s. V0771 Her |Epoch of max U light is given. V0772 Her |VB AB (7.4m, G0V; 8.5m, G8V:; A = 0.27", E = 0.97, P = 20.0yr, C V0772 Her |10.62m, 28"). One of the components (probably B) is SB1, P = V0772 Her |0.879511d [04056]. The same component must be the eclipsing system. V0772 Her |Faint X-ray source. V0774 Her |Both flares and "antiflares" (abrupt fadings) of comparable V0774 Her |amplitude are observed. V0946 Her |Not Wolf 688, a large-proper-motion star, which is at 17h19m28s.9, V0946 Her |+33{deg}05'10" (epoch and equinox 2000.0). V0973 Her |Suspected rapid brightness variations. V0994 Her |The secondary component of the double system may also vary. V1088 Her |MinII 14.1. V1091 Her |MinII 12.27. V1092 Her |The depth of MinII is 0.46. VB B (B GSC 02073-00504, 14"). V1093 Her |Multi-mode pulsations at a time scale of hours. V1094 Her |MinII 13.08. V1095 Her |MinII 12.40. V1099 Her |Multi-mode pulsations of an sdB star at a time scale of hours. V1101 Her |MinII 12.47. V1102 Her |MinII 14.27. V1103 Her |MinII 12.37. V1106 Her |MinII 12.9. DSCT type with a twice shorter period is also possible V1106 Her |[264,040]. V1108 Her |VB B (A 1" sf). The finding chart in [78247] is incorrect. V1117 Her |Flat waves near maximum and deep fadings. IR excess. V1124 Her |Blazhko effect? P(Bl) = 38.4d:. A pulsation period of 0.3551d is V1124 Her |not excluded. V1131 Her |The tabulated amplitude can be too low because of a neighboring V1131 Her |star. V1135 Her |The light elements in the Table are for eclipses. Pulsations: V1135 Her |amplitude up to 0.3m, Max=2451413.280+4.2243dxE. V1137 Her |Min II = 14.7. V1138 Her |Min II = 14.0. V1140 Her |Min II = 14.1. V1141 Her |Multiperiodic, three close, nearly equidistant frequencies. P1 is V1141 Her |tabulated (semi-amplitude 0.105m); P2 = 0.320340d (0.053m); P3 = V1141 Her |0.314355d (0.040m). V1143 Her |Min II = 11.7. V1144 Her |Min II = 15.4 :. V1146 Her |Min II = 11.45:. V1158 Her |Type RRC with a twice shorter period is possible. V1211 Her |Multiperiodic. V1227 Her |Porb = 0.06319d. V1231 Her |VB A (B 12.9mV, 12", 289{deg}, 1999). V1236 Her |VB AB (10.2m, 11.2m, 1.3", 331{deg}, 2009). V1239 Her |Eclipsing variability in quiescence: 17.4m - 19.1mV, Min = V1239 Her |2453648.236507 + 0.10008215d x E, D = 0.1P. V1250 Her |Ultraviolet flare amplitude in excess of 1.4m. V1265 Her |Blazhko effect? V1285 Her |The elements tabulated are for the first overtone. P0 = 0.5539d. V1290 Her |SB1, Porb = 45.6228d. V1299 Her |Type SRB is not excluded. V1302 Her |VB B (A 12.2mV; B 12.4mV, 13", 266{deg}, 1998). V1304 Her |VB A (B 12.1m, 16", 329{deg}, 2000). V1314 Her |Blazhko effect? V1323 Her |Intermediate polar; variations with only the spin period were V1323 Her |detected. Porb = 0.11126d. V1344 Her |MinII - MinI = 0.545P. V1366 Her |P strongly varies, current elements after JD 2456000 are given in V1366 Her |the Table. V1373 Her |Period varies. V1377 Her |Period varies. V1390 Her |MinII - MinI = 0.46P. V1396 Her |Blazhko effect. V1440 Her |P2 = 0.291982d. Mode identification is unclear. V1441 Her |Multiperiodic. V1446 Her |VB A (B 3", 133{deg}, 2000). The magnitudes in the Table were V1446 Her |influenced with the companion. V1452 Her |P1 is presented in the Table. P0 = 0.547662d; P1/P0 = 0.7462. V1457 Her |P1 is presented in the Table. P0 = 0.531662d; P1/P0 = 0.7465. V1458 Her |The data for 1SWASP J161858.05+261303.5 data [82030] are combined V1458 Her |measures for a non-variable star (V = 13.2m) near the SuperWASP V1458 Her |position and the real variable. V1460 Her |Outside outburst, type EW with light elements Min = 2456560.640 + V1460 Her |0.2078522d x E, V = 15.08m - 15.55m, MinII 15.45mV. Near outburst V1460 Her |maximum, type EA with the depth of MinI reaching 1.2mV and the V1460 Her |depth of MinII of only about 0.1mV. V1461 Her |P1 is presented in the Table. P0 = 0.559638d; P1/P0 = 0.7461. V1466 Her |P1 is presented in the Table. P0 = 0.545187d; P1/P0 = 0.7460. V1467 Her |Additional non-radial mode, P = 0.2737529d; P(Blazhko) = 112d. V1468 Her |P1 is presented in the Table. P0 = 0.570831d; P1/P0 = 0.7459. V1472 Her |P1 is presented in the Table. P0 = 0.506715d; P1/P0 = 0.7448. V1473 Her |The NSVS data for ROTSE1 J164316.86+264815.8 are combined V1473 Her |measurements for a non-variable star (V = 12.4m) near the ROTSE V1473 Her |position and the real variable. V1474 Her |P1 is presented in the Table. P0 = 0.536720d; P1/P0 = 0.7464. V1477 Her |P1 is presented in the Table. P0 = 0.532323d; P1/P0 = 0.7454. V1478 Her |P1 is presented in the Table. P0 = 0.502498d; P1/P0 = 0.7443. V1480 Her |P1 is presented in the Table. P0 = 0.473596d; P1/P0 = 0.7442. V1481 Her |P1 is presented in the Table. P0 = 0.472265d; P1/P0 = 0.7441. V1482 Her |P1 is presented in the Table. P0 = 0.532921d; P1/P0 = 0.7460. V1483 Her |P1 is presented in the Table. P0 = 0.537739d; P1/P0 = 0.7460. V1484 Her |P1 is presented in the Table. P0 = 0.530745d; P1/P0 = 0.7460. V1486 Her |P1 is presented in the Table. P0 = 0.489858d; P1/P0 = 0.7447. V1487 Her |The data for 1SWASP J165734.53+274827.7 in [82030] are combined V1487 Her |measurements for a non-variable star (V = 14.7m) near SuperWASP V1487 Her |position and this variable (18"S). V1488 Her |P1 is presented in the Table. P0 = 0.502028d; P1/P0 = 0.7459. V1489 Her |P1 is presented in the Table. P0 = 0.550905d; P1/P0 = 0.7462. V1490 Her |VB A (B 12.5mV, 16", 110{deg}, 2000). V1491 Her |P1 is presented in the Table. P0 = 0.555957d; P1/P0 = 0.7456. V1492 Her |P1 is presented in the Table. P0 = 0.478660d; P1/P0 = 0.7446. V1499 Her |P1 is presented in the Table. P0 = 0.503175d; P1/P0 = 0.7457. V1503 Her |Additional non-radial mode, P = 0.340686d; P(Blazhko) = 17.2d. V1507 Her |P1 is presented in the Table. P0 = 0.480341d; P1/P0 = 0.7438. V1519 Her |VB A (B 5", 101, 2000). V1548 Her |P = 168d: is superposed. V1552 Her |P = 320d is superposed. V1561 Her |Multiperiodic. The secondary period is 0.039646d or 0.041285d. V1570 Her |Multiperiodic. P1 is presented in the Table. P2 = 0.30441d, P3 = V1570 Her |0.33497d. The radial mode can be that corresponding to P1 or P2, V1570 Her |the other two modes are probably non-radial. V1571 Her |Between the horizontal branch and subgiant branch in the C-M V1571 Her |diagram. Slow variations and a small-amplitude (0.03m) periodic V1571 Her |variation, maybe related to the star's binary nature. V1574 Her |The light curve shape varies. V1575 Her |Multiperiodic, also P = 0.31936d. P(short)/P(long) = 0.97; one of V1575 Her |the modes is non-radial. V1576 Her |The light curve shape varies. V1581 Her |The light curve shape varies. V1582 Her |P = 170d: is superposed. V1587 Her |P varies, dP/dt = -0.432 x 10^(-6)d per year. V1588 Her |The light curve shape varies strongly. V1589 Her |P varies, dP/dt = +0.044 x 10^(-6)d per year. The light curve shape V1589 Her |varies. V1591 Her |P varies, dP/dt = -0.500 x 10^(-6)d per year. The light curve shape V1591 Her |varies. V1594 Her |Strong Blazhko effect. V1595 Her |VB B (A 17.9mG, B 18.0mG; AB 2", 359{deg}, 2000). V1596 Her |P varies, dP/dt = -0.204 x 10^(-6)d per year. Blazhko effect? V1599 Her |P varies, dP/dt = -0.280 x 10^(-6)d per year. V1601 Her |P varies, dP/dt = -0.232 x 10^(-6)d per year. Blazhko effect. V1602 Her |P varies, dP/dt = +0.120 x 10^(-6)d per year. V1604 Her |Crowded field. Blazhko effect? V1606 Her |Blazhko effect. V1608 Her |Blazhko effect? V1609 Her |Unresolved blend. V1610 Her |P varies, dP/dt = +0.096 x 10^(-6)d per year. V1612 Her |Crowded field. V1616 Her |Blazhko effect? V1617 Her |Very crowded field. V1618 Her |The light curve shape varies? V1619 Her |Cluster non-member? V1621 Her |Blended. V1623 Her |Crowded field. V1625 Her |Crowded. V1626 Her |Crowded. V1627 Her |Crowded field. The light curve shape varies? V1628 Her |Crowded. V1629 Her |Found definitely variable in [g1113], but the period from [g1114] V1629 Her |did not fit the new data; no single period? V1630 Her |P varies, dP/dt = -0.056 x 10^(-6)d per year. V1631 Her |Crowded. V1632 Her |Unresolved blend? V1633 Her |Unresolved blend. V1634 Her |Blazhko effect. V1636 Her |Crowded. V1637 Her |Crowded. V1643 Her |P varies, dP/dt = +0.024 x 10^(-6)d per year. V1644 Her |Blazhko effect. V1645 Her |VB? (17.9mG, 18.1mG, 1", 277{deg}, 2015.5). Blazhko effect? V1646 Her |Blazhko effect? V1648 Her |Blazhko effect. V1650 Her |P varies, dP/dt = +0.780 x 10^(-6)d per year. The light curve shape V1650 Her |varies. V1651 Her |Unresolved VB. Blazhko effect? V1652 Her |VB A (18.2mG; B 18.3mG, 2", 233{deg}, 2000). P varies, dP/dt = V1652 Her |-0.024 x 10^(-6)d per year. V1654 Her |P varies, dP/dt = +0.056 x 10^(-6)d per year. V1658 Her |Very crowded field. The Gaia DR2 proper motion does not seem V1658 Her |reliable. V1660 Her |Very crowded field. V1661 Her |Blazhko effect. V1663 Her |The Gaia DR2 proper motion does not seem reliable. Multiperiodic. V1663 Her |P0 (see the Table) is presumably the fundamental mode. P1 = V1663 Her |0.0615262d (presumably the first overtone). V1666 Her |P varies, quadratic term -1.239d x 10^{-9}N^2. V1667 Her |Multiperiodic? V1670 Her |Blazhko effect [g1115]. alf Her |ADS 10418 A (B 5.39m, 4.9", 107{deg}, 1973; B - SB2, G5III + F2V). alf Her |Slow variations, P ~6yr, {Delta}(m) ~0.5m; quicker changes, P ~ 50d alf Her |- 155d, {Delta}(m) ~ 0.3m - 1.0m. Together with the visual alf Her |companion the star is surrounded by an enormous envelope (R alf Her |~2*10**5R$, expansion velocity 10 km/s, mass loss 3*10**(-8)M$/yr). nu. Her |[Fe/H] = -0.26. SB? omi Her |VB interferometric. phi Her |SB, Porb = 560.5d. ome Her |ADS 10054 A (B 11.5m, 0.8", 232{deg}, 1967; C 11.0m, 28.4", ome Her |96{deg}, 1957; D 27.5", 271{deg}, 1960). Epoch of Min is given. ome Her |Double wave in the light curve. Rapid variations, P = 0.15d ome Her |[09310]. g Her |The mean cycle 1972 - 1981 is given. Slow pulsations (P = 875d +- g Her |70d) and non-periodic variations on the time scale of 5d - 15d with g Her |{Delta}(m) up to 0.2m are superimposed. u Her |ADS 10449 A (B 10.2m, 4.4", 60{deg}). Min II 4.93. R Hor |OH, H2O, SiO maser. P var. Max = 2428868 + 401.5d*E (JD2412800 - R Hor |28900); since JD2428900 - see Table. V Hor |P = 59d (JD2428380 - 910), P = 90d (JD2429170 - 980). X Hor |Epoch of Min brightness is given. Maxima are broad. Usually X Hor |secondary minima are observed. SY Hor |Min II 12.0. SZ Hor |Min II 10.7:. TU Hor |Min II 6.03; Min II - Min I = 0.52P; Max II is fainter than Max I TU Hor |by 0.05m. Peculiar ellipsoidal variable [09245]. TY Hor |Type RCB? UU Hor |P var. Max = 2416826.417 + 0.6436900d*E (JD2416800 - 25000); since UU Hor |JD2425000 - see Table. UX Hor |Min II 14.4. P var. Min I = 2426659.380 + 0.7126943d*E (JD2426650 - UX Hor |30860); since JD2430540 - see Table. UZ Hor |P var. Max = 2426679.425 + 0.338188d*E (JD2426300 - 28430); since UZ Hor |JD2430040 - see Table. VY Hor |{mu} = 0.173", ro = 33{deg}. P = 314s, 617s. AY Hor |Blended. BG Hor |Crowded. BK Hor |Crowded. BL Hor |Crowded. BO Hor |Crowded. BR Hor |VB B (A 16.5mG, B 16.7mG; AB 1.5", 174{deg}, 2000). R Hya |VB A (B 13.0m, 21.6", 324{deg}). SiO maser. P var. According to R Hya |[00458]; Max = 2328201 + 486d*E (JD2328200 - 31120); Max = 2343512 R Hya |+ 507d*E (JD2343300 - 44800); Max = 2372678 + 485d*E (JD2372200 - R Hya |72700); Max = 2380447 + 477d*E (JD2380000 - 81400); Max = 2385160 + R Hya |461d*E (JD2384700 - 88000); Max = 2394350 + 448.6d*E (JD2393900 - R Hya |2402000); Max = 2403742 + 434d*E (JD2403300 - 04200); Max = 2406363 R Hya |+ 429.5d*E (JD2406000 - 11100); Max = 2413642 + 411d*E (JD2413200 - R Hya |14100); Max = 2416563 + 405.5d*E (JD2416100 - 23400); Max = 2424288 R Hya |+ 414.7d*E (JD2423400 - 28500). since JD2428500 - see Table. T Hya |P var. Max = 2399455 + 289.00d*E(JD2398600 - 2421700); Max = T Hya |2422584 + 294.2d*E (JD2421700 - 25800); Max = 2431781 + 284.20d*E T Hya |(JD2425800 - 36200); since JD2437500 - see Table. V Hya |VB A (B 11.58mV, KO III, 46", 186{deg}). Mean brightness variations V Hya |with P = 6670d and A = 3.5m are superimposed by light oscillations V Hya |with A = 1.1m - 2m and elements given in the Table. Deep light V Hya |minima were observed in 1891, 1908, 1925, 1942 - 43, 1959, and V Hya |1962. A graph of the light curve [03614]. W Hya |VB A (B 9.3m, 72", 108{deg}). P var. Max = 2411074 + 379d*E W Hya |(JD2411000 - 14150); Max = 2414644 + 395d*E (JD2414150 - 19400); W Hya |Max = 2419746 + 378d*E (JD2419400 - 25200) [00458]. Max = 2425740 + W Hya |366d*E (JD2425200 - 27000); Max = 2440336 + 397.35d*E (JD2428000 - W Hya |40500); since JD2440500 - see Table. Amplitude and shape of the W Hya |light curve vary strongly. OH, H2O, SiO maser. X Hya |OH, H2O, SiO maser. Y Hya |Mean magnitude varies. RR Hya |H2O maser. RS Hya |P var. Max = 2422973 + 330.2d*E (JD2414000 - 23000); Max = 2429126 RS Hya |+ 342.0d*E (JD2423000 - 29200); Max = 2429455 + 331.2d*E (JD2429200 RS Hya |- 34500); since JD2434500 - see Table. RT Hya |Before 1952 P = 255d; since 1952 - see Table. The character And RT Hya |amplitude of light variations vary strongly. RU Hya |OH, H2O maser. P var. Max = 2429572 + 334.0d*E (JD2414000 - 29600); RU Hya |since JD2428500 - see Table. RW Hya |SB2 (P = 370d). Epoch of Min brightness is given. RX Hya |VB A (B 10.5m). Depth of Min II 0.05m. P var. Min I = 2428261.385 + RX Hya |2.2815942d*E (JD2419500 - 28500); Min I = 2440650.409 + RX Hya |2.2816200d*E (JD2428500 - 41400); since JD2441400 - see Table. SS Hya |VB A (B 12.0m, 13", 195{deg}); SB2. SU Hya |Mean magnitude varies with P = 780d. SV Hya |VB A (B 35", 225{deg}). {Delta}(S) = 7. SX Hya |D = 0.022P. P var. Min I = 2427659.223 + 2.895697d*E (JD2410000 - SX Hya |28000) [00007]; since JD2442500 - see Table. SY Hya |P var. Min = 2425590.589 + 3.403082d*E (JD2425500 - 31150) [07548]. SY Hya |Since JD2432200 - see Table. SZ Hya |P var. Max = 2415714.1429 + 0.53742815d*E (JD2414700 - 26500) SZ Hya |[03626]; Max = 2426410.575 + 0.53736d*E (JD2426400 - 27200) SZ Hya |[00001]; Max = 2431881.5537 + 0.53723051d*E (JD2427880 - 35200) SZ Hya |[03626]; Max = 2435542.267 + 0.5372497d*E (JD2435500 - 38900) SZ Hya |[03627]. Since JD2438770 - see Table. Blazhko effect: Max(A) = SZ Hya |2440705 + 25.8d*n [06557]; 10.44m <= Max <= 11.03m. TT Hya |Min II 7.32; d = 0.035P. TU Hya |P var. Max = 2416980 + 277.5d*E (JD2412500 - 17300); Max = 2417260 TU Hya |+ 272.5d*E (JD2417200 - 19800) [01787]; Max = 2430410 + 281.4d*E TU Hya |(JD2420500 - 30500); Max = 2438332 + 272.3d*E (JD2432000 - 39200); TU Hya |since JD2439200 - see Table. TY Hya |P var. Min = 2434478.464 + 4.660978d*E (JD2419800 - 35000) [01788]; TY Hya |since JD2435000 - see Table. UU Hya |P var. Max = 2427423.84 + 0.5238585d*E (JD2414950 - 27400) [01789]; UU Hya |Max = 2429729.835 + 0.523854d*E (JD2427000 - 31000) [00752]. UU Hya |Spectrum is based on Ca II. UW Hya |Min II 13.8:; Min II - Min I = 0.64P. P = 1.055439d? UY Hya |Min II 13.8. RRC? VV Hya |P var. Max = 2427421 + 155d*E (JD2419500 - 37000) [01792]; since VV Hya |JD2437000 - see Table. VX Hya |(k - b)2 = 0.26. Luminosity class [03149] contradicts the type of VX Hya |light variability. The shape of the light curve strongly varies. VX Hya |The main oscillation with the period P0 given in the Table is VX Hya |superimposed by the secondary one with P1 = 0.172720d [03631]. VX Hya |P1/P0 = 0.773; Pb = 0.761445d. VY Hya |Min II 9.1. VZ Hya |Min II 9.46. WY Hya |Min II 11.2. WZ Hya |(k - b)2 = 0.06. P var. Max = 2416169.681 + 0.53772640d*E WZ Hya |(JD2414000 - 19000); Max = 2419811.736 + + 0.53775858d*E (JD2419000 WZ Hya |- 21000); Max = = 2424618.630 + 0.53774101d*E (JD2421000 - 32000) WZ Hya |[00752]; Max = 2436613.445 + 0.5377229d*E (JD2436600 - 38500) WZ Hya |[03633]; since JD2438000 - see Table. XX Hya |P var. Max = 2439560.355 + 0.50774868d*E (JD2428200 - 39560) XX Hya |[05238]; since JD2439560 - see Table. XZ Hya |Min II 15.0. AE Hya |Min II 14.6. AF Hya |Min II 13.8. AI Hya |Min II 9.84; Min II - Min I = 0.438P; DII = 0.075P; dI = 0.02P; dII AI Hya |= 0.00P; EA/DM. Pulsation period P' = 0.13803d, A = 0.02m - 0.03m AI Hya |[09259]. AV Hya |Min II 10.35; dI = 0.023P:. CH Hya |Min II 15.5; Min II - Min I = 0.57P. CO Hya |Found in Centaurus, in 10{deg} to the south from the position CO Hya |published by the discoverer [00078]. CW Hya |P var? [04027]. Elements given in the Table satisfy observations CW Hya |only in the interval JD2428950 - 30375. DD Hya |P var. Max = 2431139.313 + 0.501818d*E (JD2431100 - 600) [01432]. DD Hya |Since JD2441600 - see Table. DE Hya |d = 0.014P? DF Hya |Min II 11.5. DH Hya |{Delta}(S) = 7. DK Hya |Min II 10.7. DM Hya |d = 0.15P? EU Hya |Min II 10.2. EX Hya |Light variations with Porb and amplitude up to 0.9mV due to EX Hya |eclipses of hot spot are represented by the elements: ET(Min) = EX Hya |2437699.94177 + 0.0682338422d*E, where ET(Min) is the heliocentric EX Hya |Julian Date converted to Ephemeris Time; simultaneously periodic EX Hya |modulation of the shape of the light curve between the outbursts is EX Hya |observed with the amplitude 0.2m - 0.9m and the elements: Max = EX Hya |2437699.8895 + 0.04654656d*E - 1.2d*10**(-12)*E**2 [09265]. Mean EX Hya |interval between bright outbursts is 465d [05695], mean cycle is EX Hya |close to 20 - 30d. EY Hya |P var. Max = 2432707 + 160.5d*E (JD2426100 - 32800); since EY Hya |JD2432800 - see Table. EZ Hya |Min II 10.7. P var. Min I = 2440255.8482 + 0.44976658d*E (JD2431160 EZ Hya |- 40650) [07549]; since JD2440250 - see Table. FG Hya |Min II 10.25; dI = dII = 0.085P. P var. Min I = 2431150.388 + FG Hya |0.3278422d*E (JD2431140 - 34400) [00182]; Min I = 2436968.7067 + FG Hya |0.32783433d*E (JD2434050 - 400) [03639]; Min I = 2436968.7067 + FG Hya |0.32783546d*E (JD2436950 - 43250) [09267]; since JD2444600 - see FG Hya |Table. FI Hya |V27 in the globular cluster NGC 4590 (M68); cluster non-member. FS Hya |According to [01480] P = 91.7d. FW Hya |Min II 12.4. FY Hya |VB A (B 15.45m, 15", 90{deg}); {Delta}(S) = 7:; (k - b)2 = -0.03. GK Hya |Min II 9.57. There is a square term in the elements: GK Hya |-4.01d*10**(-9)*E**2. GM Hya |d <= 0.01P. GN Hya |Min II 13.6. GT Hya |Cep? HS Hya |Min II 8.55. IK Hya |Blazhko effect with Pi ~30d. IW Hya |OH, H2O maser. KM Hya |P var? KU Hya |VB AB (7.3m, 7.4m, A = 0.150", P = 58.93 yr, E = 0.219); A(v) = KU Hya |0.06m. KW Hya |Porb = 7.75043d; E = 0.110 [09273]; Min II 6.35; Min II - Min I = KW Hya |0.54P. V0404 Hya |MinII 15.10. V0412 Hya |MinII 12.9:. V0420 Hya |Porb = 764 d. Symbiotic features in the spectrum. V0421 Hya |Variable brown dwarf. V0427 Hya |VB A (B 13.9mpg, 22", 305{deg}, 1999; C 14.8mpg, 35", 276{deg}, V0427 Hya |1999). V0430 Hya |Blazhko effect? V0434 Hya |MinII - MinI = 0.54P. V0443 Hya |A twice shorter period is not excluded. V0453 Hya |A twice shorter period is not excluded. V0466 Hya |Min II = 11.6. O'Connell effect. V0468 Hya |P varies? [80001]. V0470 Hya |Min II = 13.50. V0472 Hya |Min II = 12.5. V0474 Hya |Min II = 12.2. V0475 Hya |Min II = 13.2. V0476 Hya |Min II = 13.1. V0477 Hya |Min II = 16.2. V0483 Hya |Min II = 12.55. V0484 Hya |A brown dwarf with periodic brightness variations. V0488 Hya |A brown dwarf with periodic brightness variations. V0490 Hya |Min II = 8.71:. VB AB (8.81m, 10.93m, 1".10, 169{deg}, 1991). V0498 Hya |Superhumps: P = 0.06036d. V0500 Hya |P1 is tabulated; P0 = 0.56391d. Amplitude ratio A1/A0 = 2.45. V0502 Hya |Min II = 10.09. VB AB (A 10.3m var; B 12.3m, 2.2", 72{deg}, 1943). V0504 Hya |Type EW with a twice longer period is possible. V0511 Hya |Min II = 9.05. V0514 Hya |Min II = 14.5:. V0515 Hya |P = 0.269198d is also possible. V0518 Hya |The star's position coincides with SN 2001am. V0519 Hya |Min II = 12.50. V0520 Hya |P = 0.331234d is also possible. V0522 Hya |P = 0.255132 is also possible. V0524 Hya |Min II = 17.6. V0541 Hya |Multiperiodic. V0542 Hya |Min II = 10.40. dP/dt = -0.45 x 10^(-5) d/yr. VB AB (10.8m, 11.7m, V0542 Hya |2", 42{deg}, 2003). V0543 Hya |Blazhko effect, P = 59d. V0545 Hya |Min II = 11.98. Besides variations with the tabulated period, a V0545 Hya |second EW periodicity is revealed, P2 = 0.353901d, with amplitudes V0545 Hya |of both minima about 0.25m. V0547 Hya |VB A (B = V0548 Hya, 5", 148{deg}, 1999). V0548 Hya |VB B (A = V0547 Hya; AB 5", 148{deg}, 1999). V0549 Hya |VB B (A = V0550 Hya; AB 13", 185{deg}, 2000). V0550 Hya |VB A (B = V0549 Hya, 13", 185{deg}, 2000). V0551 Hya |Multiperiodic. V0552 Hya |Blazhko effect, P = 48.3d. V0553 Hya |Min II = 12.90. V0554 Hya |Min II = 13.2. V0555 Hya |Min II = 12.20. V0559 Hya |Blazhko effect, P = 26.50d. V0571 Hya |Blazhko effect, P = 11.80d. V0575 Hya |Blazhko effect, P = 8.52d. V0588 Hya |Blazhko effect, P = 87.73d [81056]. V0592 Hya |Possibly Blazhko effect with P = 14.2d. V0598 Hya |VB A (15.4mpg; B 15.6mpg, 18", 43{deg}, 2000). The coordinates in V0598 Hya |[81005] refer to the companion. V0599 Hya |VB B (A 15.1mpg, B 16.6mpg; AB 29", 152{deg}, 2000). The V0599 Hya |coordinates in [81005] refer to the brighter star. V0603 Hya |Double-mode pulsations. The Table contains the period for the first V0603 Hya |overtone. Fundamental mode: P0 = 0.4867803. P1/P0 = 0.7449. V0621 Hya |P1 is presented in the Table. P0 = 0.467934d; P1/P0 = 0.7434. V0623 Hya |P1 is presented in the Table. P0 = 0.545078d; P1/P0 = 0.7461. V0624 Hya |P1 is presented in the Table. P0 = 0.528738d; P1/P0 = 0.7465. V0627 Hya |Period varies. V0635 Hya |P1 is presented in the Table. P0 = 0.558754d; P1/P0 = 0.7462. V0638 Hya |The data for 1SWASP J090758.16-153811.8 in [82030] are combined V0638 Hya |measurements for the a non-variable star (V = 13.6m) near the V0638 Hya |SuperWASP position and the real variable. V0659 Hya |P1 is presented in the Table. P0 = 0.447456d; P1/P0 = 0.7412. V0664 Hya |P1 is presented in the Table. P0 = 0.520738d; P1/P0 = 0.7461. V0677 Hya |[Fe/H] = -1.16. V0678 Hya |[Fe/H] = -1.37. V0679 Hya |P varies, dP/dt = +0.273 x 10^(-6)d per year. V0680 Hya |P varies, dP/dt = -0.125 x 10^(-6)d per year. V0681 Hya |The light elements in the Table are for the first overtone. P0 = V0681 Hya |0.523746d. P1/P0 = 0.7460. V0682 Hya |The light elements in the Table are for the first overtone. P0 = V0682 Hya |0.530818d. P1/P0 = 0.7464. V0683 Hya |The light elements in the Table are for the first overtone. P0 = V0683 Hya |0.535115d. P1/P0 = 0.7469. V0684 Hya |P varies, dP/dt = +0.116 x 10^{-6}d per year. V0685 Hya |P varies, dP/dt = -0.497 x 10^(-6)d per year. V0686 Hya |The light elements in the Table are for the first overtone. P0 = V0686 Hya |0.520186d. P1/P0 = 0.7458. V0688 Hya |The light elements in the Table are for the first overtone. P0 = V0688 Hya |0.557511d. P1/P0 = 0.7450. V0689 Hya |The light elements in the Table are for the first overtone. P0 = V0689 Hya |0.522230d. P1/P0 = 0.7476. V0691 Hya |Blazhko effect. V0692 Hya |Blazhko effect. V0695 Hya |P varies, dP/dt = +0.225 x 10^(-6)d per year. V0697 Hya |P varies, dP/dt = +0.116 x 10^(-6)d per year. V0698 Hya |P varies, dP/dt = +1.553 x 10^(-6)d per year. V0700 Hya |P varies, dP/dt = +0.066 x 10^(-6)d per year. V0702 Hya |Blended. V0705 Hya |P varies, dP/dt = -0.051 x 10^(-6)d per year. V0708 Hya |Blended. Earlier reported as a double-mode variable. V0709 Hya |The light elements in the Table are for the first overtone. P0 = V0709 Hya |0.525259d. P1/P0 = 0.7456. V0710 Hya |P varies, dP/dt = +0.234 x 10^(-6)d per year. V0712 Hya |The light elements in the Table are for the first overtone. P0 = V0712 Hya |0.545757d. P1/P0 = 0.7460. V0713 Hya |Multiperiodic. The period in the Table is that for the fundamental V0713 Hya |mode. P1 = 0.051745d. P1/P0 = 0.786. V0716 Hya |P varies, dP/dt = -1.081 x 10^(-6)d per year. V0717 Hya |The star earlier had signatures of a double-mode RR Lyrae variable. V0718 Hya |P varies? dP/dt = +0.044 x 10^(-6)d per year. V0719 Hya |P varies, dP/dt = -0.488 x 10^(-6)d per year. Blazhko effect. V0720 Hya |Cluster non-member? V0721 Hya |The light elements in the Table are for the first overtone. P0 = V0721 Hya |0.546782d. P1/P0 = 0.7444. V0722 Hya |The light elements in the Table are for the first overtone. P0 = V0722 Hya |0.537097d. P1/P0 = 0.7450. V0723 Hya |The light elements in the Table are for the first overtone. P0 = V0723 Hya |0.530525d. P1/P0 = 0.7450. V0724 Hya |P varies, dP/dt = +0.102 x 10^(-6)d per year. V0726 Hya |Cluster non-member? [g1001]. VB A (15.4mG; B 15.9mG, 2", 278{deg}, V0726 Hya |2000). V0733 Hya |Other possible periods: 0.6342d (RRAB, RR0); 0.2792d; 0.2182d. bet Hya |VB A (B 5.6m, 0.9", 8{deg}, 1959). khi 2 Hya |Min II 5.92. Y Hyi |d = 0.024P. RS Hyi |In the region of the Small Magellanic Cloud. Not a member of the RS Hyi |cloud. RT Hyi |Min II 14.1. RV Hyi |Min II 12.4; Min II - Min I = 0.61P. RY Hyi |In the region of the Small Magellanic Cloud. Not a member of the RY Hyi |Cloud. ST Hyi |The member of the Small Magellanic Cloud. [A/H] = -0.8. SZ Hyi |In the region of the Small Magellanic Cloud. Not a member of the SZ Hyi |Cloud. TW Hyi |{Delta}(S) = 10:. UU Hyi |P = 112.25d? VW Hyi |Mean interval between the supermaxima is 179d. Porb = 0.0742711d. VW Hyi |Between the normal outbursts the brightness periodically increases VW Hyi |by 0.35m - 0.40m because of hot spot appearances: Max = VW Hyi |2440128.0222 + 0.0742711d*E [07550]. During the supermaxima the VW Hyi |period between the superhumps is 0.0769d [09275]. Sometimes the VW Hyi |light oscillations with the amplitude 2% and cycle from 28s to 34s VW Hyi |are observed [07551]. VY Hyi |In the region of the Small Magellanic Cloud. Not a member of the VY Hyi |Cloud. VZ Hyi |RR [00193]. WX Hyi |Mean interval between the supermaxima is 141.5d. Porb = 0.0748134d WX Hyi |[09277]. Period between the superhumps observed during the WX Hyi |supermaxima is 0.07737d [09278]. WZ Hyi |In the region of the Small Magellanic Cloud. Not a member of the WZ Hyi |Cloud. ZZ Hyi |A galaxy PGC 232232 [00001]. AC Hyi |In the region of the Small Magellanic Cloud. Not a member of the AC Hyi |Cloud. BB Hyi |{Delta}(S) = 7:. CY Hyi |MinII 9.8. DM Hyi |Type RR with P = 0.64272d or 0.39125d is also possible. DS Hyi |In the region of the SMC galaxy, probable non-member. V Ind |P var. Max = 2439792.276 + 0.4796030d*E (JD2414000 - 40000) V Ind |[05233]; since JD2440000 - see Table. {Delta}(S) = 7, (k - b)2 = V Ind |0.02. RS Ind |Min II 10.0. P var. RU Ind |VB A (B 12.6m, 2.3", 103{deg}). Min II 12.1. RX Ind |240d < P < 310d. RY Ind |Min II 11.04. ST Ind |Min II 11.79. SU Ind |Min II 9.5:. TV Ind |Min II 11.9. AR Ind |Min II 14.4. RRC? AY Ind |VB? CH Ind |MinII 8.14:. CI Ind |A variable double brown dwarf. VB (0.7"). CK Ind |Besides 6 {Gamma} Dor modes, a {Delta} Sct mode (P = 0.039 d) was CK Ind |detected. CQ Ind |MinII - MinI = 0.33P. CZ Ind |Blazhko effect, P = 133d. DI Ind |Type EW with a twice longer period is not excluded. DQ Ind |Type DSCT: with P = 0.1163d is also possible. DS Ind |Period varies strongly. DW Ind |Blazhko effect, P = 26.7d:. EI Ind |VB (14.7mG, 15.2mG, 2", 50{deg}, 2000). EL Ind |Blazhko effect, P = 950d. M-m varies between 0.13P and 0.18P. R Lac |VB A (B 14.1m, 6", 50{deg}). S Lac |P var. Max = 2412857 + 238.2d*E (JD2410000 - 16400); Max = 2418828 S Lac |+ 241.45d*E (JD2416400 - 20500); Max = 2427307 + 242.7d*E S Lac |(JD2420500 - 27300); Max = 2437290 + 237.4d*E (JD2427300 - 37300); S Lac |since JD2437300 - see Table. U Lac |There are light variations with the periods: 150d, 550 - 690d, U Lac |2900d. V Lac |P var. There is a square term in the elements: V Lac |-6.48d*10**(-8)*E**2. W Lac |P var. Max = 2415255 + 323d*E (JD2414600 - 15300); Max = 2425628 + W Lac |335.5d*E (JD2425600 - 38000) [00458]; Max = 2433844 + 324.5d*E W Lac |(JD2428000 - 33850); since JD2433850 - see Table. X Lac |P var. Max = 2418890.497 + 5.444303d*E (JD2416670 - 29500) [02033]; X Lac |since JD2429500 - see Table. Z Lac |P var. There is a square term in the elements: -3.4d*10**(-8)*E**2. Z Lac |[A/H] = 0.2. RR Lac |P var. Max = 2419434.331 + 6.416146d*E (JD2417900 - 31600); since RR Lac |JD2431600 - see Table. [A/H] = 0.0. RT Lac |Min II 9.62. P var. Min I = 2440382.9005 + 5.0740484d*E + RT Lac |1.02d*10**(-8)*E**2 (JD2411650 - 42500) [08592]; since JD2436470 - RT Lac |see Table. There is a square term in the elements given in the RT Lac |Table: -2.7d*10**(-8)*E**2. Shape of the light curve and depths of RT Lac |the Minima vary. According to [09293] the period of the distortion RT Lac |wave migration is ~9.5 yr, the period of the wave amplitude RT Lac |variations (0 < A <= 0.17m) is ~30 yr. According to [09292] the RT Lac |migration period is nearly half of the value given in [09293]. RV Lac |Mean magnitude varies with the period 550 - 700d. RW Lac |Min II 10.8; DII = 0.024P; Min II - Min I = 0.492P. RX Lac |S7.5/1e. P = 174d (JD2414950 - 29550) [01026]; since JD2436800 - RX Lac |see Table. RY Lac |Oscillations of mean magnitude with P = 300 - 420d and A <= 0.5m RY Lac |are superimposed by oscillations with P = 38 - 91d. SS Lac |Probable member of the open cluster NGC 7209. Min II 10.5; Min II - SS Lac |Min I = 0.57P; d = 0.008P. Apsidal motion with P = 1000 yr is SS Lac |possible. ST Lac |Elements should be checked. SU Lac |P var. Max = 2412748 + 279.10d*E (JD2412700 - 27000) [05707]; Max = SU Lac |2426972 + 286.74d*E (JD2426900 - 31000); Max = 2431008 + 306.0d*E SU Lac |(JD2431000 - 33150) [00001]; Max = 2433150 + 319.14d*E (JD2433150 - SU Lac |42150) [05707]; since JD2442100 - see Table. SW Lac |Min II 9.31. P var. Min I = 2418943.712 + 0.32071236d*E (JD2410000 SW Lac |- 19990); Min I = 2420038.621 + 0.32071510d*E (JD2419990 - 25210); SW Lac |Min I = 2430996.525 + 0.32071665d*E (JD2425210 - 33690); Min I = SW Lac |2436046.5634 + 0.32072132d*E (JD2433690 - 36755) [05222]; Min I = SW Lac |2437572.5723 + 0.32072811d*E (JD2436755 - 40000) [03374]; Min I = SW Lac |2440467.4592 + 0.32072480d*E (JD2440110 - 40500) [06089]; Min I = SW Lac |2441249.3737 + 0.3207197d*E (JD2440500 - 41600); [00001]; Min I = SW Lac |2442697.4039 + 0.3207144d*E (JD2441600 - 43100) [09295]; Min I = SW Lac |2443459.7476 + 0.3207216d*E (JD2443100 - 44400) [09297]; Min I = SW Lac |2444856.8064 + 0.3207184d*E (JD2444400 - 44900) [00001]; since SW Lac |JD2444900 - see Table. Shape of the light curve, depths of minima SW Lac |and heights of maxima vary. TW Lac |d = 0.018P. P var. Min I = 2424387.332 + 3.0374936d*E (JD2424380 - TW Lac |34000) [02389]; Min I = 2434049.593 + 3.037520d*E (JD2434000 - TW Lac |36560) [03115]; since JD2441500 - see Table. TZ Lac |In the region of the open cluster NGC 7243. UW Lac |Depth of Min II 0.05m; d = 0.028P. P var. Min I = 2429158.17 + UW Lac |5.2902d*E (JD2414580 - 29440) [01813]; Min I = 2429158.17 + UW Lac |5.290000d*E (JD2429440 - 35800) [03115]; since JD2436800 - see UW Lac |Table. Apsidal motion is possible [09300]. UY Lac |d = 0.022P. UZ Lac |P var? VX Lac |P var. Min = 2424791.488 + 1.0744891d*E (JD2424700 - 32400); Min = VX Lac |2432479.477 + 1.0744991d*E (JD2432400 - 40510); Min = 2440750.971 + VX Lac |1.0744881d*E (JD2440750 - 43000) [07552]; since JD2443000 - see VX Lac |Table. VY Lac |Min II 10.6. P var? Min I = 2434629.392 + 1.036245d*E (JD2424700 - VY Lac |39830) [01804]; since JD2440080 - see Table. WY Lac |Light variations with P = 850d and A = 1.5m are superimposed by WY Lac |variations with P = 50d and A = 1m. XX Lac |In the region of the open cluster NGC 7243. XZ Lac |P var. AG Lac |Min II 14.0. AR Lac |Min II 6.43; Min II - Min I = 0.5018P; dI = 0.045P; DII = 0.13P; AR Lac |dII = 0.00P. P var. Min I = 2426624.378 + 1.983244d*E (JD2415300 - AR Lac |26800) [09309]; Min I = 2429535.739 + 1.9832125d*E (JD2426800 - AR Lac |36000) [09312]; Min I = 2437018.414 + 1.983252d*E (JD2436000 - AR Lac |37500) [00001]; since JD2437500 - see Table. There is a square term AR Lac |in the elements given in the Table: - 5.24d*10**(-9)*E**2. Shape of AR Lac |the light curve varies; there is a distortion wave with A up to AR Lac |0.13mV migrating in the direction of decreasing phases with P ~2.5 AR Lac |yr. Spectrum investigations [01816,09315, 9316]. AU Lac |Min II 12.2; Min II - Min I = 0.53P. AW Lac |Min II 11.2. BH Lac |Hydrogen lines in the spectrum are sharp and deep [03149]. BL Lac |Z = 0.07; B-V = +1.0. Light curve graph [06784]. BM Lac |The elements are valid in the interval JD2425200 - 26250. BT Lac |There is a square term in the elements: -0.0004d*E**2. Epoch of Max BT Lac |brightness is given in the Table. Mean brightness varies in the BT Lac |range 13.8m - 15.2m with P = 654d. Mean amplitude of the BT Lac |shortperiodical variations is ~1.5m. There occur changes of BT Lac |primaries and secondaries minima into each other. BU Lac |The main variation is superimposed by waves with a possible period BU Lac |-200d. CG Lac |Min II 14.0. CM Lac |Min II 8.53; DII = 0.12P. CN Lac |Min II 12.6. In the region of the open cluster NGC 7209. Not member CN Lac |of the cluster. CO Lac |Min II 10.79. Apsidal motion with P = 42.3 yr is observed. There is CO Lac |a periodic term in The elements given in the Table: -0.0133d CO Lac |cos(157.7{deg} + 0.0359{deg}*E). Min II = 2427534.8439 + CO Lac |1.5422075d*E + 0.0133d cos(157.7{deg} + 0.0359{deg}*E). CS Lac |Min II 9.4. CZ Lac |{Delta}(S) = 1. P var. Max = 2432878.234 + 0.43210346d*E (JD2428700 CZ Lac |- 39400) [01442]; Max = 2443081.309 + 0.4319850d*E (JD2439400 - CZ Lac |43100) [05839]; Max = 2444080.122 + 0.432114d*E (JD2443800 - 44100) CZ Lac |[09009]; since JD2445100 - see Table. DD Lac |VB A (B 9.2m, 69", 16{deg}). P var. Max = 2421914.178 + DD Lac |0.19309018d*E - 0.001798d*10**(-8)*E**2 (JD2421400 - 37600) DD Lac |[05711]; since JD2443000 - see Table. According to [09337] DD Lac |simultaneously the pulsations with the following periods are DD Lac |observed (the corresponding AB values are given in the brackets): DD Lac |P1 = 0.193082d (0.080m), P2 = 0.197382d (0.034m), P3 = 0.182115d DD Lac |(0.020m), P4 = 0.187438d (0.016m), P5 = 0.095109d (0.010m), P6 = DD Lac |0.23583d (0.008m). A var; 0.04m <= A <= 0.12m. DE Lac |{Delta}(S) = 5. P var. Max = 2428807.130 + 0.2536940d*E (JD2427000 DE Lac |- 33000); Max = 2433005.766 + 0.2536929d*E (JD2433000 - 39100) DE Lac |[03378]; since JD2442000 - see Table. DF Lac |[A/H] = 0.2. DG Lac |P var. Min = 2426266.355 + 2.206435d*E (JD2426200 - 40000) [04961]; DG Lac |since JD2440000 - see Table. DH Lac |P var. Max = 2418240 + 284.8d*E (JD2418000 - 27350); since DH Lac |JD2427300 - see Table. DM Lac |Erroneously labeled VV306, instead of VV307, in the chart [05862]. DO Lac |According to [00085], EA. EG Lac |P > 50d? [05386]. EM Lac |Min II 13.09. EN Lac |VB A (B 11.32mV, 27", 345{deg}; C 9.0mV, 62", 48{deg}); SB1 (Porb = EN Lac |12.0968d). Eclipsing system with a pulsating primary component of EN Lac |BCEP type. Depth of Min I 0.05mB. Min I = 2444909.4339 + EN Lac |12.096816d*E; D = 0.015P, d = 0.000P. Simultaneously pulsations are EN Lac |observed with the periods P1 = 0.169170d, P2 = 0.170770d, P3 = EN Lac |0.181692d [09346]. The corresponding amplitudes of pulsations vary. EN Lac |The values of the amplitudes in B system are as follows: A1 = EN Lac |0.046m, A2 = 0.024m, A3 = 0.022m (1952 - 1965); A1 = 0.016m, A2 = EN Lac |0.010m, A3 = 0.014m (1977); A1 = 0.010m, A2 = 0.014m, A3 = 0.023m EN Lac |(1980 - 81). 0.01m <= A <= 0.11m. EO Lac |Min II 12.9; Min II - Min I = 0.485P. EP Lac |Depth of Min II 0.04m. ER Lac |Depth of Min II 0.05m:. ES Lac |Min II 11.6; Min II - Min I = 0.57P. Apsidal motion is possible: ES Lac |Min II = 2433582.95 + 4.459451d*E [09347]. EU Lac |The chart in [05862] is wrong. EV Lac |VB A (B 12.74mB, 10", 260{deg}, 1949). Dark companion (A = 0.0206", EV Lac |P = 45 yr, E = 0.5) [09348]. In 1979 sinusoidal light oscillations EV Lac |were observed in the range 10.20m - 10.27mV: Min = 2444037.576 + EV Lac |4.378d*E [09349]. In 1974 - 76 such periodicity was not observed EV Lac |[09350]. EW Lac |Non-radial pulsations with P = 0.7d - 0.8d are also possible EW Lac |[09351,09352]. EX Lac |d = 0.050P. FQ Lac |A var; P var. Elements given in the Table are valid in the FQ Lac |intervale JD2427950 - 31700. FU Lac |d = 0.013P. GS Lac |Min II 15.2. GX Lac |Min II 10.23. HK Lac |SB1 (Porb = 24.4284d [09355]). HM Lac |Depth of Min II 0.05m. HN Lac |Min II 14.7. HQ Lac |Erroneously labeled VV307, instead of VV306, in the chart [05862]. HR Lac |Min II 14.3. HT Lac |In the region of the open cluster NGC 7209. HW Lac |Min II 14.8. HX Lac |Min II 14.8. HZ Lac |Min II 15.0. IM Lac |Min II 13.2. IN Lac |E? IP Lac |Min II 14.0. IR Lac |Min II 15.4; d = 0.03P. IT Lac |P var. IU Lac |Min II 13.5. IY Lac |Blazhko effect? IZ Lac |Min II 12.7. KO Lac |Min II 14.7. KP Lac |P < 1d. KR Lac |Min II 15.8; dII = 0.05P. KS Lac |Depth of Min II 0.03m. KU Lac |Depth of Min II 0.03m. LU Lac |Min II 15.32. LW Lac |d = 0.03P. Depth of Min II 0.03m? LY Lac |Min II 12.6. LZ Lac |Min II 12.5. MO Lac |d = 0.04P. Depth of Min II 0.05m. MP Lac |Min II 12.5. MV Lac |Min II 15.0. MZ Lac |Min II 12.1; Min II - Min I = 0.713P. Min II = 2433872.702 + MZ Lac |3.158719d*E. Elements for Min I are given in the Table. NN Lac |d = 0.02P. np (usually brighter) component of a close pair. The NN Lac |range of combined brightness is given in the Table. NO Lac |Depth of Min II 0.03m. NR Lac |Min II 13.4. Sp (brighter) component of a close pair. The range of NR Lac |combined brightness is given in the Table. NU Lac |EW? NW Lac |Min II 13.9. Close binary, the components of which are equal in NW Lac |brightness at minimum light. The range of combined brightness is NW Lac |given in the Table. OO Lac |Min II 12.8. OV Lac |150d <= P <= 200d. OX Lac |Depth of Min II 0.04m. PP Lac |Min II 12.0. PT Lac |Min II 15.4. PZ Lac |In the region of the open cluster NGC 7243. QQ Lac |In the region of the open cluster NGC 7243. QU Lac |Depth of Min II 0.04m. V0335 Lac |Min II 15.8. V0338 Lac |In the region of the open cluster IC 1434. V0339 Lac |P = 3.4084964d? V0340 Lac |Min II 12.4; Min II - Min I = 0.762P; Min II = 2432858.521 + V0340 Lac |19.943102d*E. Elements for Min I are given in the Table. V0342 Lac |Min II 12.9. V0343 Lac |Min II - Min I = 0.57P. Depth of Min II 0.03m:. V0344 Lac |Min II 13.0. Min I = 2433873.5784 + 0.39222768d*E (JD2432800 - V0344 Lac |35800); since JD2445200 - see Table. V0345 Lac |Min II 11.6; Min II - Min I = 0.340P; DII = 0.040P; dII = 0.014P. V0345 Lac |Apsidal motion is possible. V0347 Lac |VB. V0350 Lac |VB A (B 9.7m, 66", 94{deg}); SB1 (P = 17.755d [09356]). Min II 6.45 V0350 Lac |[07468]. Mean magnitude varies. See also [08933]. V0355 Lac |Northern component of a pair. V0360 Lac |SB2 (P = 10d [09357]). Min II 5.93. V0362 Lac |VB A (B 13.2m, 1.8", 49{deg}). V0363 Lac |VB A (B 11.3m, F6 III - V:, 6.3", 325{deg}). V0364 Lac |Min II 9.15; Min II - Min I = 0.52P; dI = 0.003P, DII = 0.077P, dII V0364 Lac |= 0.009P. V0412 Lac |SB, Porb = 41.95yr. V0413 Lac |SB, Porb = 2.9833d. V0442 Lac |Quasi-periodic brightness variations of a planetary nebula, V0442 Lac |possibly due to variable mass loss or pulsations. V0450 Lac |MinII 13.65. V0457 Lac |A twice shorter period is not excluded. V0468 Lac |Multiperiodic. V0485 Lac |O'Connell effect. V0493 Lac |EW type with a twice longer period is also possible. V0514 Lac |A twice longer period is also possible. V0524 Lac |VB A (B 4", 112{deg}, 1998). Double-mode pulsation. The other V0524 Lac |period is 0.101399d. V0529 Lac |VB A (B 5", 297{deg}, 1998). V0556 Lac |A twice longer period is also possible. V0568 Lac |P = 0.12351d is also possible. V0600 Lac |VB A (B 4.5", 207{deg}, 1998). V0607 Lac |Near the galaxy 2MASX J22525476+5235101. V0639 Lac |A twice longer period is also possible. V0651 Lac |RRC type with P = 0.4109221d is also possible. V0665 Lac |During each observing run, one or two of the three periods (that in V0665 Lac |the Table and also 48.10d and 46.09d) was observed. V0667 Lac |VB A (15.4mG; B 15.8mG, 10", 21{deg}, 2000). V0680 Lac |Triple-mode pulsations. The Table presents the first-overtone V0680 Lac |period (P1). P2 = 0.14968d, P3 = 0.12458. V0681 Lac |VB A (13.6mG; B 14.3mG, 5.5", 309{deg}, 2000). The variability V0681 Lac |range in the Table is for combined light. V0685 Lac |The Table contains light elements for eclipses. DSCT pulsations: P V0685 Lac |= 0.060193d, amplitude = 0.1mag. V0693 Lac |A twice longer period is also possible. V0696 Lac |VB B (A 13.5mG, B 15.1mG; AB 7", 266{deg}, 2000). The variability V0696 Lac |range in the Table is for combined light. V0700 Lac |VB A (16.1mG; B 16.2mG, 3", 222{deg}, 2000). The variability range V0700 Lac |in the Table is for combined light. V0712 Lac |VB (16.9mG, 17.1mG, 2", 169{deg}, 2000). The variability range in V0712 Lac |the Table is for combined light. V0716 Lac |VB B (A 15.3mG, B 15.7mG; AB 20", 322{deg}, 2000); other companions V0716 Lac |around. A twice longer period is not excluded. V0717 Lac |O'Connell effect. V0720 Lac |Not red. V0724 Lac |VB A (15.1mG; B 15.2mG, 11", 211{deg}, 2000). V0734 Lac |VB B (A 13.2mG, B 14.4mG; AB 7", 344{deg}, 2000). The variability V0734 Lac |range in the Table is for combined light. V0737 Lac |VB (14.3mG, 14.5mG, 4", 328{deg}, 2000). The variable is NW- comp. V0737 Lac |The variability range in the Table is for combined light. V0741 Lac |Type EW with a twice longer period is not excluded. V0743 Lac |VB B (A 14.1mG, B 15.9mG; AB 4", 190{deg}, 2000). The variability V0743 Lac |range in the Table is for combined light. V0745 Lac |VB B (A 13.7mG, B 16.6mG; AB 6.5", 26{deg}, 2000). The variability V0745 Lac |range in the Table is for combined light. V0773 Lac |Blended with several fainter stars. The variability range in the V0773 Lac |Table is for combined light. V0782 Lac |VB A (15.6mG; B 16.4mG, 6.5", 344{deg}, 2000). V0787 Lac |O'Connell effect. V0788 Lac |VB (14.8mG, 16.0mG, 1", 88{deg}, 2000). The variability range in V0788 Lac |the Table is for combined light. V0795 Lac |Period varies. V0805 Lac |Multiperiodic. P2 = 0.68501d, possible P3 = 0.5672d. V0807 Lac |O'Connell effect. V0813 Lac |Multiperiodic, P2 = 0.6878d. V0815 Lac |Double maxima, at phases 0.00P and -0.12P. V0820 Lac |Type ELL with a twice longer period is also possible. V0832 Lac |VB A (11.8mG; B 14.1mG, 7.5", 125{deg}, 2000). V0843 Lac |O'Connell effect. V0845 Lac |VB A (15.9mG; B 17.5mG, 5", 257{deg}, 2000). V0863 Lac |VB? V0880 Lac |VB A (15.5mG; B 16.7mG, 9", 245{deg}, 2000). V0881 Lac |P = 52d is superposed. V0886 Lac |VB A (13.2mG; B 14.4mG, 9", 115{deg}, 2000). V0896 Lac |VB A (12.2mG; B 13.5mG, 5", 75{deg}, 2000). V0898 Lac |VB A (16.1mG; B 17.1mG, 4", 304{deg}, 2000). Type EW with a twice V0898 Lac |longer period is also possible. R Leo |P var. Max = 2385112 + 312.43d*E (JD2385100 - 2402500); Max = R Leo |2402929 + 314.33d*E (JD2402500 - 11500); Max = 2411416 + 308.93d*E R Leo |(JD2411500 - 16500); Max = 2416984 + 317.84d*E (JD2416500 - 22500); R Leo |Max = 2423328 + 312.75d*E (JD2422500 - 27000); Max = 2427081 + R Leo |307.40d*E (JD2427000 - 30000); Max = 2437337 + 312.13d*E (JD2430000 R Leo |- 37500); since JD2437500 - see Table. SiO, H2O, OH maser. S Leo |P var. Max = 2420654 + 189.24d*E (JD2420200 - 26100); Max = 2426142 S Leo |+ 185.92d*E (JD2426100 - 28100); since JD2428100 - see Table. V Leo |H2O maser. W Leo |P var. Max = 2434651 + 385.41d*E (JD2409500 - 35000); since W Leo |JD2437500 - see Table. OH maser. Y Leo |P var. Min = 2422372.520 + 1.6860978d*E (JD2418000 - 23500) Y Leo |[02389]; Min = 2422372.5368 + 1.68607314d*E (JD2423500 - 38600) Y Leo |[09307]; since JD2438600 - see Table. There is periodic term in the Y Leo |elements given in the Table: +0.00375d*sin(0.21487{deg}*E + Y Leo |141.7{deg}). Depth of Min II 0.1m IR. RR Leo |{Delta}(S) = 7.1. P var. Max = 2430440.3385 + 0.45238172d*E + RR Leo |1.963d*10**(-10)*E**2 (1898 - 1977) [08299]; since JD2441400 - see RR Leo |Table. RT Leo |Min II 10.5. RW Leo |P var. Before JD2440800 Min = 2424993.458 + 1.6825365d*E [03115]; RW Leo |since JD2440800 - see Table. RX Leo |{Delta}(S) = 6.8. SS Leo |P var. Max = 2415485.723 + 0.62633242d*E (JD2414000 - 22000) SS Leo |[00752]; since JD2422000 - see Table. [Fe/H] = -1.59. ST Leo |(k - b)2 = 0.08. SZ Leo |P var. Before JD2442500 Max = 2425331.400 + 0.5340833d*E [04157]; SZ Leo |since JD2442500 - see Table. Light curve shape var? TU Leo |Minor planet (8) Flora. TV Leo |P var. Max = 2419852.318 + 0.6728362d*E (JD2419000 - 28000) TV Leo |[00001]; since JD2437000 - see Table. (k - b)2 = -0.01. TX Leo |VB A (B 7.8m, 2", 157{deg}, 1971); A binary according to lunar TX Leo |occultation data: ro = 0.0005". The range of combined brightness is TX Leo |given. Min II 5.69; DII = 0.19P; Min II - Min I = 0.550P. TY Leo |Elements need confirmation. UU Leo |Min II 11.5. P var. Since JD2430000 - see Table. UV Leo |Min II 9.49; d = 0.014P. P var. Before JD2434000 Min I = UV Leo |2425574.302 + 0.60008516d*E [07554]; since JD2434000 - see Table. UX Leo |Min II 10.4. Moments of Min by BBSAG contradict the tabulated UX Leo |elements. UZ Leo |Min II 10.12. P var, nonlinear term: +2.8d*10**(-12)*E**2. XX Leo |Min II 11.4. Period should be checked. XY Leo |Min II 9.80. P var. Min = 2435195.66306 + 0.2841091d*E (JD2434000 - XY Leo |36500) [03392]; Min = 2437376.465 + 0.28409592d*E (JD2436500 - XY Leo |40000) [00001]; Min = 2441005.5364 + 0.28410727d*E (JD2441000 - XY Leo |44000) [09084]; since JD2444000 - see Table. The light curve shape XY Leo |var. XZ Leo |Min II 11.1. AB Leo |Epoch of Min is given. According to [01853], Max = 2428880 + AB Leo |103.2d*E (JD2414600 - 19000, 2428000 - 31600); During other time AB Leo |intervals cycles 75d - 125d. AD Leo |{mu} = 0.49", P = 265{deg}; {pi} = 0.20". X-ray and radio source. AD Leo |Astrometric binary? AF Leo |H2O maser. AM Leo |VB A (B 10.64m, 11", 270{deg}). Min II 9.83. AP Leo |Min II 9.88. P var. Min = 2414986.868 + 0.430350d*E (JD2414700 - AP Leo |18600); since JD2418600 - see Table. Light curve shape var. AQ Leo |Elements for fundamental mode pulsations (P0) see Table. For the AQ Leo |first overtone: P1 var?; P1 = 0.4101369d (1929 - 1969); P1 = AQ Leo |0.410130d (1957 - 1969); during 1973 - 1975 Max1 = 2441766.486 + AQ Leo |0.4101487d*E. {delta}(M0) = 0.23m, {delta}(M1) = 0.46M. AU Leo |Vr = +7545 km/s. Variability is doubtful. BB Leo |[Fe/H] = -1.32. BL Leo |Min II14.4. P var. Since JD2442000 - see Table. BV Leo |Min II 16.1. BW Leo |Min II 15.4. BX Leo |[Fe/H] = -1.23. BZ Leo |Min II 15.8. CD Leo |Light curve shape var. CE Leo |Min II 12.5. P var? Min by BBSAG contradict the tabulated elements. CN Leo |Mu = 4.7", P = 235{deg}; {pi} = 0.41". Soft X-ray source, radio CN Leo |source. CW Leo |Dust envelope, 6"*4". Molecular radioemission: SiO, SiS, HCN, HC3N, CW Leo |CO, H2O, NH3, etc. Polarization in I band up to 24%. CX Leo |VB A (B 12.3m, 132{deg}); SB (Porb = 12685.4d). CY Leo |{mu} = 0.307", P = 141.3{deg}; {pi} = 0.022". Outside flares CY Leo |{Delta}(m) < = 0.036m; P = 600s, 822s, 1638s [06209]. A single CY Leo |strong flare with {delta}(M) = 0.61m in blue light of 10 Min CY Leo |duration was observed [06141], which is attributed by several CY Leo |authors to the presence of a red flaring companion. DE Leo |P = 1.2d - 2.0d? DG Leo |VB B (A 6.6m, A 8IV, SB2, Porb = 4.15d; B 6.9m, 0.271", 211.2{deg}, DG Leo |1980, Porb ~200yr). The range of the bombined brightness is given. DH Leo |SB1, Porb = 1.070354d. FL Leo |Variability range according to E.M. Halbedel, IBVS No. 3502, 1990. FX Leo |Not a nearby star (despite having a Gl number). GU Leo |MinII 12.19. GV Leo |MinII 11.87. HI Leo |The depth of MinII is 0.5. HK Leo |Epoch of Min is given. HM Leo |Porb = 0.1868d. HQ Leo |The tabulated amplitude was probably influenced by a companion in HQ Leo |35" np. HY Leo |Porb = 0.1736d; Pspin = 0.04804d. IK Leo |Superhumps P = 0.056281d. IQ Leo |Min II = 15.2. IU Leo |Porb = 0.3763d. KO Leo |P = 0.293919d is also possible. KT Leo |P = 0.256494 is also possible. KV Leo |Multiperiodic. SB? LR Leo |Pulsates in the first overtone (see Table) and fundamental (Max = LR Leo |2454701.577 + 0.557447d x E) modes. P1/P0 = 0.7469. A nonradial LR Leo |mode with P = 0.559369d may also be present. LU Leo |O'Connell effect. LY Leo |O'Connell effect. LZ Leo |VB A (13.6mV; B 15.7mV, 9", 258{deg}, 2000). MV Leo |Porb = 0.14608d. NV Leo |Double-mode pulsations. The Table gives the first-overtone light NV Leo |elements. For the fundamental mode, Max = 2454800.541 + 0.483098d x NV Leo |E. P1/P0 = 0.7441. OX Leo |Multiperiodic. P2 = 0.89405d. PS Leo |P1 is presented in the Table. P0 = 0.509437d; P1/P0 = 0.7443. PW Leo |P1 is presented in the Table. P0 = 0.503529d; P1/P0 = 0.7454. PX Leo |P1 is presented in the Table. P0 = 0.521624d; P1/P0 = 0.7456. PY Leo |P1 is presented in the Table. P0 = 0.530969d; P1/P0 = 0.7455. PZ Leo |P1 is presented in the Table. P0 = 0.536083d; P1/P0 = 0.7462. QQ Leo |P1 is presented in the Table. P0 = 0.502380d; P1/P0 = 0.7456. QR Leo |P1 is presented in the Table. P0 = 0.561943d; P1/P0 = 0.7460. QS Leo |P1 is presented in the Table. P0 = 0.471002d; P1/P0 = 0.7440. QU Leo |P1 is presented in the Table. Additional non-radial mode, P = QU Leo |0.359842d. P0 = 0.490181d; P1/P0 = 0.7441. QV Leo |P1 is presented in the Table. P0 = 0.560076d; P1/P0 = 0.7455. QY Leo |P1 is presented in the Table. P0 = 0.469265d; P1/P0 = 0.7432. V0335 Leo |P1 is presented in the Table. P0 = 0.481418d; P1/P0 = 0.7445. V0338 Leo |P1 is presented in the Table. P0 = 0.553220d; P1/P0 = 0.7466. V0340 Leo |P1 is presented in the Table. P0 = 0.489670d; P1/P0 = 0.7450. V0342 Leo |VB A (B 11.9m, 35", 300{deg}, 2011). V0343 Leo |P1 is presented in the Table. P0 = 0.465896d; P1/P0 = 0.7435. V0344 Leo |P1 is presented in the Table. P0 = 0.533747d; P1/P0 = 0.7461. V0345 Leo |P0 is presented in the Table. P1 = 0.358597d; P1/P0 = 0.7442. V0350 Leo |P1 is presented in the Table. P0 = 0.547015d; P1/P0 = 0.7460. V0351 Leo |P1 is presented in the Table. P0 = 0.472132d; P1/P0 = 0.7438. R LMi |SiO, H2O, OH mazer. T LMi |Min II 10.97. P var. Min I = 2420573.698 + 3.019889d*E (JD2420200 - T LMi |25000); Min I = 2423856.323 + 3.0199336d*E (JD2423800 - 35500); T LMi |since JD2438400 - see Table. U LMi |1m <= A <= 3.3m. Periodicity sometimes breaks down. V LMi |{Delta}(S) = 5.7. Y LMi |P var. Max = 2428636.322 + 0.52443938d*E + 0.0597d* Y LMi |*sin(0.0657{deg}*E + 27.2{deg}) (JD2425250 - 28500); Max = Y LMi |2428636.348 + 0.5244564d*E (JD2428500 - 30000) [01856]; mean Y LMi |elements for interval JD2432200 - 38900 are given in the Table; in Y LMi |this interval the period changed with the cycle of ~2100d. Blazhko Y LMi |effect with the period 33.4d [01856]; 07m <= A <= 1.9m, 0.19P <= m Y LMi |- M <= 0.44P. RT LMi |Min II 11.7. RU LMi |Spectrum description [09326]. RW LMi |VB A (B 15.5m B, 9", 10{deg}). 0.3m - 2.6m K, 7.64m - 10.71m, 9.7m RW LMi |- 14.6m R, 14.1m - 18.1m B, 14.8m - 18.6m U. Mean brightness RW LMi |varies. Gaseous-dust circumstellar envelope. CO emission. Spectrum RW LMi |description [09327]. RY LMi |VB A (B 16.1m, dM2, 15", 126{deg}); {mu} = 0.14", P = 264{deg}. P0 RY LMi |= 215.197388s, dP0/dt = 5.6s*10**(-14)/s, A0 = 0.0440m; P1 = RY LMi |304.4s, A1 = 0.0150m; P2 = 271.0s, A2 = 0.0134m; P3 = 107.6s, A3 = RY LMi |0.0032m; P4 = 126.2s, A4 = 0.0028m; P5 = 119.8s, A5 = 0.0026m. Mean RY LMi |brightness varies by 0.05m. WZ LMi |MinII 12.68. XX LMi |MinII 12.56. XY LMi |MinII 11.13. XZ LMi |SB1? YY LMi |SB1? YZ LMi |Min II = 19.3. AC LMi |Porb = 0.07938d. AD LMi |SB1, Porb = 15.465d. AE LMi |Min II = 13.1. AF LMi |Min II = 14.5. AG LMi |Min II = 10.75:. A twice longer period, with equally deep minima, AG LMi |is also possible. AR LMi |P1 is presented in the Table. P0 = 0.493881d; P1/P0 = 0.7448. AV LMi |P1 is presented in the Table. P0 = 0.547379d; P1/P0 = 0.7460. AW LMi |Additional non-radial mode, P = 0.3056288d; P(Blazhko) = 25d. AX LMi |P1 is presented in the Table. P0 = 0.487467d; P1/P0 = 0.7445. AY LMi |Additional non-radial mode, P = 0.313789d; P(Blazhko) = 13.4d. AZ LMi |P1 is presented in the Table. P0 = 0.571772d; P1/P0 = 0.7459. BB LMi |P1 is presented in the Table. P0 = 0.535953d; P1/P0 = 0.7463. R Lep |P var. Max = 2398883 + 436.44d*E (JD2398000 - 2412000); Max = R Lep |2412849 + 418.04d*E (JD2412000 - 23000); Max = 2423300 + 441.38d*E R Lep |(JD2423000 - 36000); since JD2436000 - see Table. A var; 5.5m <= R Lep |Max <= 9.5m (Possible period is more than 40 years [03402]). S Lep |Mean magnitude varies with the cycle of 890d. H2O maser. T Lep |SiO maser. U Lep |P var. Max = 2425084.431 + 0.58147098d*E (JD2411000 - 25090); Max = U Lep |2425084.431 + 0.58147377d*E (JD2425080 - 37700) [03403]; since U Lep |JD2436600 - see Table. {Delta}(S) = 8.5; (k - b)2 = 0.00. V Lep |Min II 9.9. Z Lep |Min II 12.0:. RR Lep |Min II 10.4. RS Lep |Min II 9.96. RU Lep |P var? RZ Lep |S 4/4. SS Lep |SB2 (Porb = 258.2d [09363]). SY Lep |VB A (B 15.2m: V, 18", 270{deg}). AM Lep |VB B (A = HR 1696, 4.45m, B8V; B 12", 337{deg}, 1998). BC Lep |Min II = 10.70. BH Lep |A brown dwarf with periodic brightness variations. BL Lep |VB (6", 19{deg}, 1999); the variable is probably the southern BL Lep |component. Combined magnitudes are presented in the Table. BN Lep |P varies strongly. BO Lep |VB A (11.4mV; B 11.6mV, 19", 163{deg}, 1998). BW Lep |Type EW (EC) with a twice longer period is also possible. Cluster BW Lep |non-member. BX Lep |P varies [g1127]. CF Lep |Crowded. CH Lep |Multiperiodic. P0 is presented in the Table, P1 = 0.0391700d. P1/P0 CH Lep |= 0.7791. CI Lep |Cluster non-member. CK Lep |Crowded. CM Lep |Crowded. CN Lep |Crowded. CO Lep |Multiperiodic. P2 = 0.36099d and P3 = 0.37037d are probably CO Lep |non-radial modes. CT Lep |Blazhko effect [g1126]. CW Lep |Cluster non-member. CX Lep |Cluster non-member. CZ Lep |Cluster non-member. S Lib |P var. Max = 2405692 + 192.14d*E (JD2402700 - 24000); Max = 2424141 S Lib |+ 194.74d*E (JD2424000 - 30500); Max = 2431900 + 190.34d*E S Lib |(JD2430500 - 37200); Max = 2439203 + 197.61d*E (JD2437200 - 39300); S Lib |since JD2441000 - see Table. Mean value of the period is given in S Lib |the Table. A var (1.8m <= A <= 5m). W Lib |P var. Max = 2412272 + 203.76d*E (JD2412000 - 28500); Max = 2428573 W Lib |+ 201.48d*E (JD2428500 - 34000); since JD2434000 - see Table. X Lib |P var. Max = 2423500 + 165.75d*E (JD2413000 - 25000); since X Lib |JD2425000 - see Table. Y Lib |P var. Max = 2413452 + 275.7d*E (JD2413400 - 22000); Max = 2422273 Y Lib |+ 272.5d*E (JD2422000 - 28000) [00458]; Max = 2434921 + 277.04d*E Y Lib |(JD2428000 - 35000); since JD2435000 - see Table. Z Lib |P var. Max = 2417736 + 294.5d*E (JD2407100 - 17800); since Z Lib |JD2424400 - see Table. RR Lib |P var. Max = 2409699 + 277.4d*E (JD2409600 - 15600); Max = 2416345 RR Lib |+ 273.2d*E (JD2416300 - 19700); Max = 2421027 + 278.6d*E (JD2421000 RR Lib |- 27150) [00458]; since JD2427150 - see Table. RS Lib |P var. Max = 2413396 + 217.2d*E (JD2413300 - 20000); Max = 2420110 RS Lib |+ 219.6d*E (JD2420000 - 27500) [00458]; Max = 2429078 + 215.6d*E RS Lib |(JD2427500 - 35000); Max = 2438196 + 219.9d*E (JD2435000 - 42600); RS Lib |since JD2441700 - see Table. RT Lib |P var. Max = 2413776 + 254.21d*E (JD2413000 - 19000); since RT Lib |JD2419000 - see Table. RU Lib |P var. Max = 2413363 + 312.0d*E (JD2413300 - 16200); Max = 2416807 RU Lib |+ 322.5d*E (JD2416800 - 21000); Max = 2421309 + 317.0d*E (JD2421300 RU Lib |- 24200); Max = 2424804 + 311.5d*E (JD2424800 - 29800) [00458]; Max RU Lib |= 2434909 + 319.9d*E (JD2429800 - 35000); since JD2437700 - see RU Lib |Table. RV Lib |Min II 9.44. RX Lib |[A/H] = -0.5. P var. Max = 2430913.6 + 24.950d*E (JD2425000 - RX Lib |36300) [00266]; since JD2436300 - see Table. SS Lib |Min II 10.8; d = 0.030P. ST Lib |VB A (B 14m, 14", 0{deg}). TV Lib |{Delta}(S) = 2.5. TY Lib |d = 0.019P. UW Lib |[Fe/H] = - 0.25. VV Lib |P var. Max = 2424268.474 + 0.4781418d*E (JD2419800 - 2425000); VV Lib |since JD2425000 - see Table. VW Lib |Observations given in [00293] contradict the elements given in the VW Lib |Table. VY Lib |P var? [03506].{Delta}(S) = 6. VZ Lib |Min II 10.55; dI = 0.000P; dII = 0.005P. P var. Min I = 2429022.227 VZ Lib |+ 0.358053d*E (JD2428600 - 30400) [09368]; Min I = 2430899.223 + VZ Lib |0.358448d*E (JD2430400 - 32400) [02532]; since JD2444330 - see VZ Lib |Table. YZ Lib |Min II 12.9. AA Lib |P var? The elements are valid in the interval JD2427800 - 29600. AF Lib |The chart in [06286] has south on top. AP Lib |Z = 0.0486. AQ Lib |[Fe/H] = -0.60. BE Lib |The chart in [06286] is wrong. BH Lib |Recommended chart in [06286]: part III, page 50. BT Lib |Min II 12.3. BW Lib |The chart in [06286] is wrong. CG Lib |[Fe/H] = -1.82. P var. Max = 2438592.287 + 0.3068674d*E (JD2427800 CG Lib |- 39600) [07557]; since JD2439600 - see Table. CQ Lib |The coordinates in [01870] are wrong. CZ Lib |The chart in [06286], part I, page 40 is wrong. Recomended chart in CZ Lib |[06286]: part III, page 52. EH Lib |{Delta}(S) = 0. 9.35m <= Max < = 9.49m V; Max (A) = 2442162.556 + EH Lib |0.273778d*E [09336]. ES Lib |Min II 7.33. EU Lib |70d <= P <= 90d. FI Lib |90d <= P <= 110d. FS Lib |OH emission. FX Lib |Spectrum description [06167,09371]. KZ Lib |MinII 11.22. LZ Lib |Deviations from the light curve with the tabulated period reveal P2 LZ Lib |= 0.334339d, also with an EW light curve. A quadruple system? MR Lib |Blazhko effect, P = 41.7d. NY Lib |P = 0.361945d is also possible. OO Lib |P = 0.462571d is also possible. OR Lib |The mean brightness varies slowly. OZ Lib |Superposed variations with an amplitude up to 0.5m and a period OZ Lib |about 53d. PT Lib |Min II = 14.6. A twice shorter period and type RRC are possible. PW Lib |P varies? [80001]. QZ Lib |Superhumps, P= 0.064602d. V0339 Lib |Min II = 14.2. V0351 Lib |Min II = 14.0. V0364 Lib |Two outbursts were observed. Porb = 0.70242d. V0366 Lib |P varies. The light elements in the Table are for JD 2453639 - V0366 Lib |2455100. V0368 Lib |Double-mode pulsations. The Table contains light elements for the V0368 Lib |first overtone. Fundamental mode: Max = 2455000.800 + 0.57857d x E. V0368 Lib |P1/P0 = 0.7443. V0377 Lib |P1 is presented in the Table. P0 = 0.544401d; P1/P0 = 0.7455. V0379 Lib |P1 is presented in the Table. P0 = 0.483137d; P1/P0 = 0.7447. V0381 Lib |[Fe/H] = -2.01. V0382 Lib |Type BLBOO (BLBoo) is also possible. V0392 Lib |Blended. del Lib |VB A (B 11.3m, 9", 351{deg}; C 12.80m, 67", 90{deg}); Min II 4.98. del Lib |P var? S Lup |VB A (B = X Lup, 13", 176{deg}). P var. Max = 2411950 + 347.81d*E S Lup |(JD2411950 - 14000); Max = 2414040 + 339.31d*E (JD2414000 - 19000); S Lup |Max = 2419135 + 345.12d*E (JD2419000 - 26000); Max = 2426038 + S Lup |336.60d*E (JD2426000 - 29500); Max = 2429743 + 345.15d*E (JD2429500 S Lup |- 35000); since JD2437600 - see Table. X Lup |VB B (A = S Lup). Y Lup |P var. Max = 2424691 + 408.15d*E (JD2423000 - 25500); Max = 2425503 Y Lup |+ 394.81d*E (JD2425500 - 30250); Max = 2430641 + 407.75d*E Y Lup |(JD2430250 - 35000); since JD2437900 - see Table. RU Lup |Sometimes varies quasiperiodically: P1 = 3.5457d, P2 = 3.8375 RU Lup |[02412]. H2O maser. RY Lup |Quasiperiodicity: P = 3.7609d [09366]. SX Lup |Min II 11.8. TY Lup |The chart in [06286] is wrong. UX Lup |[A/H] = -0.9. P var. P = 16.2403d (JD2411526 - 14040); P = 16.2065d UX Lup |(JD2414040 - 24016); P = 16.2492d (JD2424016 - 25638); P = 16.1794d UX Lup |(JD2425638 - 26449); P = 16.2241d (JD2426449 - 29693) [05387]. VV Lup |Close northern companion. VZ Lup |P var? Light curve shape var? CC Lup |The chart in [06286] is wrong. CW Lup |The charts in [06286] are wrong. CX Lup |Min II 12.8. CY Lup |High Max every 360d, especially faint Min 80d before these high CY Lup |Max. DG Lup |Min II 15.1. DQ Lup |The chart in [06286] is wrong. DY Lup |In [00087] the information on variability of DY Lup is accompanied DY Lup |by the coordinates of DZ Lup and vice versa. The chart for DY Lup DY Lup |in [06286] is labeled DZ Lup, the chart for DZ Lup in [06286] is DY Lup |wrong. DZ Lup |In [00087] the information on variability of DY Lup is accompanied DZ Lup |by the coordinates of DZ Lup and vice versa. The chart for DY Lup DZ Lup |in [06286] is labeled DZ Lup, the chart for DZ Lup in [06286] is DZ Lup |wrong. EL Lup |VB. ER Lup |P2 = 140d. EU Lup |The chart in [06286] is wrong. FK Lup |Min II 10.7:. FM Lup |The chart in [02385] is wrong. FR Lup |Deep Min II. FT Lup |Min II 9.98. dI = 0.025P?, dII >= 0.066P. P var. Before JD2439300 FT Lup |Min I = 2427987.310 + 0.470089d*E [03948]; since JD2445000 - see FT Lup |Table. All the observations are well represented also by the FT Lup |elements: Min I = 2445061.834 + 0.470083d*E - 0.114d*10**(-9)*E**2 FT Lup |[09360]. Light curve shape var? FV Lup |Min II 11.2. GG Lup |Min II 5.8. GN Lup |VB A (B 10.2m vis, 10", 98{deg}). GO Lup |Relatively short P. GW Lup |In the dark nebula Barnard 228. HL Lup |The initial identification with 2U 1543 - 47 is wrong. 2U 1543 - 47 HL Lup |= IL Lup. HM Lup |B - V: +1.12. HN Lup |B - V: +1.55, +1.68. HO Lup |B - V: +0.70, +0.81. OO Lup |A twice shorter period is not excluded. OR Lup |SB3, G1IV/V + G8:V/IV: + K0:V. OT Lup |A twice shorter period is not excluded. OU Lup |MinII - MinI = 0.28P. PP Lup |MinII - MinI = 0.28P. PQ Lup |Blazhko effect, P=48.8d. PS Lup |P varies, current elements are given. PZ Lup |Min II = 10.67. QQ Lup |Min II = 13.2. QT Lup |Min II = 12.80. QU Lup |Min II = 10.53. dP/dt = -0.61 x 10^{-5} d/yr. VB AB (11.3, 11.3, QU Lup |0.8", 326{deg}, 1991). QV Lup |Min II = 11.68. QZ Lup |Min II = 8.43:. V0339 Lup |Blazhko effect, P = 49.5d. V0353 Lup |Min II = 12.7. V0363 Lup |Min II = 11.85. V0372 Lup |OH, SiO maser. V0378 Lup |Min II = 11.0. V0379 Lup |Min II = 9.89. V0386 Lup |Min II = 11.3. V0412 Lup |VB A (18.3mG; B 19.5mG, 2.5", 269{deg}, 2000). V0414 Lup |Blended. V0417 Lup |Blended. V0421 Lup |Blended. V0423 Lup |Blended. V0425 Lup |VB A (18.4mG; B 18.6mG, 3.5", 23{deg}, 2000). V0426 Lup |Crowded field. V0436 Lup |VB B (A 18.0mG, B 18.4mG; AB 3.4", 164{deg}, 2000). V0448 Lup |VB? V0451 Lup |Crowded. V0452 Lup |Crowded. V0455 Lup |Crowded. V0458 Lup |VB B (A 14.4mG, B 14.5mG; AB 4", 198{deg}, 2000). alf Lup |VB A (B 14.0m, 27.6", 232{deg}, 1901). Soft X-ray source. P2 = alf Lup |3.145d is possible [08417]. gam Lup |SB, Porb = 2.8081d. del Lup |Less probable variant of elements: Max = 2441045.160 + 0.14273*E. R Lyn |S 4/5E - S 6/6 - . S Lyn |VB A (B 14m, 12.6", 155{deg}). P var. Max = 2414564 + 300.26d*E S Lyn |(JD2414500 - 27400); Max = 2434241 + 294.42d*E (JD2427400 - 35100); S Lyn |Max = 2440225 + 300.44d*E (JD2435100 - 40220); since JD2440220 - S Lyn |see Table. T Lyn |P var. Max = 2425012 + 419.0d*E (JD2412800 - 34700); since T Lyn |JD2434700 - see Table. U Lyn |H2O, OH emission. P var. Max = 2417168 + 440.3d*E (JD2417100 - U Lyn |26000) [00458]; Max = 2435908 + 432.05d*E (JD2426000 - 36000); Max U Lyn |= 2439898 + 447.1d*E (JD2436000 - 40000); since JD2440000 - see U Lyn |Table. V Lyn |Cycles 55d and 87d replace one another. Mean brightness varies. Y Lyn |SB. RR Lyn |VB A (B 10m, 50"). Min II 5.90; Min II = 2438051.3115 + RR Lyn |9.945074d*E; E = 0.081; Min II - Min I = 0.45P (JD2437700). RW Lyn |[Fe/H] = -1.37. RZ Lyn |Min II 10.8. SW Lyn |Min II 9.65; dI = 0.038P. P var. Min I = 2425643.323 + 0.6440661d*E SW Lyn |(JD2425640 - 35850) [02742]; Min I = 2438795.8016 + 0.6440520d*E SW Lyn |(JD2438380 - 840) [09387]; Min I = 2440614.0107 + 0.6440729d*E SW Lyn |(JD2439500 - 40620) [00001]; Min I = 2442786.4493 + 0.6440677d*E SW Lyn |(JD2440650 - 42790) [07292]; since JD2442780 - see Table. SX Lyn |Min II 10.1. P var. Min I = 2428636.375 + 2.0225615d*E (JD2427400 - SX Lyn |34700) [00519]; Min I = 2442561.424 + 2.0225172d*E (JD2442400 - SX Lyn |44000); since JD2444000 - see Table. SZ Lyn |SB (Porb = 1146d, E = 0.26 [09388]). {Delta}(S) = 0. There is a SZ Lyn |periodical term in the elements: -0.00573d cos 2{pi} (EP0/P1 + SZ Lyn |0.007); P0 = 0.120534920d, P1 = 1150d. Amplitude and shape of the SZ Lyn |light curve vary. TT Lyn |{Delta}(S) = 7. TV Lyn |[Fe/H] = -0.99. TW Lyn |{Delta}(S) = 10. P var. Max = 2418676.804 + 0.4817201d*E (JD2418670 TW Lyn |- 20155); Max = 2420155.685 + 0.4816929d*E (JD2420155 - 27480); Max TW Lyn |= 2427479.359 + 0.4817481d*E (JD2427480 - 28630); Max = 2428627.310 TW Lyn |+ 0.4818529d*E (JD2428620 - 37800) [02819]. Since JD2445000 - see TW Lyn |Table. TZ Lyn |Epoch of Min brightness is given. UU Lyn |Min II 11.82. UV Lyn |Min II 9.78. UZ Lyn |VR var (P = 0.065d [09392]). VV Lyn |VB A (B 11.76m, 38.6",354{deg}); SB. VW Lyn |P1 = 590s, P2 = 260s [09393]. CW Lyn |Type RRC: is also possible. DY Lyn |MinII 10.16. EO Lyn |Min II = 14.1. EQ Lyn |Porb = 0.0599d. EZ Lyn |Brightenings and mini-outbursts between superoutburts, 16.5m - EZ Lyn |17.1mV, with oscillations ({Delta} V about 0.2m, P = 0.0295d). EZ Lyn |Superhumps in superoutbursts: P = 0.0597d. FG Lyn |Min II = 11.00. FH Lyn |Porb = 0.2890d. FI Lyn |Min II = 10.18. FL Lyn |Possible Porb = 0.0687d. Superhumps P = 0.06921d. FN Lyn |Min II = 10.36. FT Lyn |Min II = 13.08. HS Lyn |A twice shorter period is not excluded. IW Lyn |VB A (B 7", 349{deg}, 1999). IZ Lyn |Probably a VB unresolved in the photometry. KX Lyn |[Fe/H] = -1.9. LO Lyn |Blazhko effect, P=9.763d. LR Lyn |Blazhko effect? [81001]. LV Lyn |P0 is presented in the Table. P1 = 0.360108d; P1/P0 = 0.7460. LW Lyn |P1 is presented in the Table. P0 = 0.477799d; P1/P0 = 0.7442. MM Lyn |P1 is presented in the Table. P0 = 0.480261d; P1/P0 = 0.7442. MQ Lyn |Additional non-radial mode, P = 0.2534778d; P(Blazhko) = 22.7d. MR Lyn |P1 is presented in the Table. P0 = 0.485654d; P1/P0 = 0.7451. MS Lyn |Porb = 0.080d. MT Lyn |P1 is presented in the Table. P0 = 0.501434d; P1/P0 = 0.7447. MV Lyn |P1 is presented in the Table. P0 = 0.478181d; P1/P0 = 0.7442. MW Lyn |Period varies. NQ Lyn |Cluster non-member? [g0001]. NR Lyn |The coordinates in [g0136] are offset by 3.5". A twice longer NR Lyn |period is also possible [g0001]. NZ Lyn |VB B, with a close bright companion. OW Lyn |Crowded. OX Lyn |Crowded. OZ Lyn |Crowded. PP Lyn |Crowded. PQ Lyn |Close to the cluster center, crowded. PR Lyn |Crowded. PS Lyn |The proper motion in the Gaia DR2 catalog does not seem realistic. PU Lyn |Crowded. PW Lyn |Crowded. PX Lyn |Crowded. PY Lyn |Crowded. PZ Lyn |Blend. QQ Lyn |Crowded. QR Lyn |Crowded. QS Lyn |Crowded. QT Lyn |Crowded. QU Lyn |VB B, with a close bright companion. QX Lyn |Crowded. QY Lyn |Crowded. QZ Lyn |Crowded. V0335 Lyn |Crowded. V0336 Lyn |P varies. V0339 Lyn |Crowded. V0343 Lyn |Crowded. V0344 Lyn |Crowded. The magnitude range in the Table is likely contaminated by V0344 Lyn |companions. V0346 Lyn |Crowded. V0348 Lyn |The light elements in the Table are for the first overtone. P0 = V0348 Lyn |0.54621d; P1/P0 = 0.7452. V0351 Lyn |Crowded. V0352 Lyn |VB? V0354 Lyn |Crowded. V0357 Lyn |Crowded. V0366 Lyn |Crowded. V0368 Lyn |Crowded. S Lyr |P var. Max = 2416186 + 432.01d*E (JD2415700 - 20100); Max = 2420961 S Lyr |+ 445.83d*E (JD2420900 - 26500); Max = 2426748 + 429.01d*E S Lyr |(JD2426500 - 30700); Max = 2432357 + 441.88d*E (JD2432000 - 34600); S Lyr |since JD2442500 - see Table. U Lyr |VB A (B 13.0m, 9.4", 182{deg}). P var. Max = 2418345 + 459.22d*E U Lyr |(JD2418000 - 27000); since JD2432000 - see Table. V Lyr |OH maser. W Lyr |P var. Max = 2415578 + 198.39d*E (JD2413000 - 19000); Max = 2420322 W Lyr |+ 194.99d*E (JD2419000 - 25500); Max = 2431326 + 198.97d*E W Lyr |(JD2427000 - 31500); Max = 2432494 + 195.11d*E (JD2431500 - 36500); W Lyr |since JD2437500 - see Table. Y Lyr |{Delta}(S) = 0.8. Z Lyr |P var. Max = 2418150 + 285.07d*E (JD2417500 - 22200); Max = 2423600 Z Lyr |+ 291.37d*E (JD2422200 - 29500); Max = 2430000 + 284.00d*E Z Lyr |(JD2429500 - 36800); since JD2436800 - see Table. RR Lyr |[Fe/H] = -1.14. {Delta}(S) = 6. Blazhko effect of variable RR Lyr |amplitude (practically to complete disappearance of Blazhko RR Lyr |effect); Pi = 40.8d. Variations of Max light phase up to 0.14P; RR Lyr |magnitude in Max var in the range up to 0.6m, that in Min var in RR Lyr |the range up to 0.1m [03418].According to [07270], a cycle ~4 yr is RR Lyr |present in Blazhko effect amplitude changes; at the end of the RR Lyr |cycle the Blazhko effect phase changes abruptly by 0.25Pi. Magnetic RR Lyr |field strength varies with the pulsational period [09339]. P var. RR Lyr |Max = 2414856.480 + 0.56682069d*E (JD2414800 - 18800); Max = RR Lyr |2421854.052 + 0.56685169d*E (JD2418800 - 26500) [09379]; Max = RR Lyr |2426571.3828 + 0.56684333d*E (JD2426500 - 32500) [09338]; Max = RR Lyr |2438215.9492 + 0.566830d*E (JD2438000 - 41000) [05238]; Max = RR Lyr |2438215.9492 + 0.56683313d*E (JD2441000 - 42900) [09338]; since RR Lyr |JD2442900 - see Table. RS Lyr |P var. Max = 2415566 + 299.38d*E (JD2415000 - 24000); Max = 2425176 RS Lyr |+ 308.08d*E (JD2424000 - 37200); since JD2437200 - see Table. RT Lyr |P var. Max = 2437022 + 250.85d*E (JD2415000 - 39000); since RT Lyr |JD2439000 - see Table. RU Lyr |P var. Max = 2415983 + 370.70d*E (JD2415900 - 33000); Max = 2433035 RU Lyr |+ 363.0d*E (JD2433000 - 41000); since JD2441000 - see Table. RV Lyr |D = 0.015P. P var. Min = 2415949.7096 + 3.599007d*E (JD2412185 - RV Lyr |16000); Min = 2415949.7096 + 3.599046d*E (JD2416000 - 21400) RV Lyr |[00001]; Min = 2432015.671 + 3.5989845d*E (JD2421400 - 32000); Min RV Lyr |= 2432015.671 + 3.5990235d*E (JD2432000 - 39300) [09085]; since RV Lyr |JD2442000 - see Table. RW Lyr |OH, H2O maser. RX Lyr |P var. Max = 2416226 + 249.94d*E (JD2415000 - 28800); since RX Lyr |JD2428800 - see Table. RZ Lyr |P var. Max = 2416415.360 + 0.51127069d*E (JD2413000 - 19000) RZ Lyr |[00001]; Max = 2426161.4375 + 0.51124948D*E (JD2426000 - 38000) RZ Lyr |[00323]; since JD2438000 - see Table. Blazhko effect, height of Max RZ Lyr |varies: 10.6m - 10.9m, Max ({Delta}(m)) = 2430904.3 + 116.654d*N + RZ Lyr |0.01034d*N**2; Min ({Delta}(m)) - Max ({Delta}(m)) = 59.3d [03419]. RZ Lyr |[Fe/H] = -1.69; {Delta}(S) = 10.0. SS Lyr |P var. Max = 2421695 + 350.48d*E (JD2416000 - 22500); Max = 2429991 SS Lyr |+ 355.22d*E (JD2429000 - 38000); since JD2438000 - see Table. SZ Lyr |According to [05750], during JD2434665 - 35044 the amplitude was SZ Lyr |twice smaller than usual (due to the depth of Min), and a temporary SZ Lyr |phase shift by 0.5P occured. TT Lyr |d = 0.010P; Min II 9.44. TW Lyr |VB A (B 15.2m pg, 14".70{deg}, 1912). TY Lyr |P var. Max = 2419285 + 336.49d:*E (JD2419000 - 23700); Max = TY Lyr |2423985 + 329.79d*E (JD2423700 - 31250); since JD2438600 - see TY Lyr |Table. TZ Lyr |VB A (B 12.29m, 2.54", 2.5{deg}). Min II 11.05. P var. Min I = TZ Lyr |2420669.480 + 0.5288234d*E (JD2420000 - 38000); since JD2438000 - TZ Lyr |see Table. UX Lyr |B - V: +0.11, +0.47. UZ Lyr |d = 0.012P:. P var. Min = 2424268.474 + 1.891253d*E (JD2422500 - UZ Lyr |25500) [02087]; since JD2425500 - see Table. AA Lyr |Min II 13.5. AH Lyr |d = 0.03P. Min II 12.1. AK Lyr |Min II 12.9. AL Lyr |P var. Max = 2427865.82 + 12.9837d*E (JD2414800 - 28000) [00001]; AL Lyr |Max = 2432889.03 + 12.98047d*E (JD2428000 - 35500) [04427]; since AL Lyr |JD2435500 - see Table. AQ Lyr |P var. Max = 2425301.592 + 0.3571721d*E (JD2425300 - 29000); Max = AQ Lyr |2428944.739 + 0.3571285d*E (JD2429000 - 30200); Max = 2430158.976 + AQ Lyr |0.3571611d*E (JD2430200 - 33900); Max = 2433909.178 + 0.3571861d*E AQ Lyr |(JD2433900 - 35700); during JD2435700 - 37800 - see Table. Blazhko AQ Lyr |effect? According to visual observations, 0.4m <= {Delta}(m) <= AQ Lyr |1.2m. AY Lyr |Cycles of supermaxima 188.9d - 212.8d. Superhumps period: Ps = AY Lyr |0.07552d [06249]. BF Lyr |P var. Max = 2425296 + 130d*E (JD2425300 - 800); During JD2429045 - BF Lyr |570 - see Table. BH Lyr |P var. Max = 2413712.358 + 0.6129028d*E (JD2413712 - 27927); Max = BH Lyr |2434472.547 + 0.6128941d*E (JD2434472 - 36102); since JD2436423 - BH Lyr |see Table. BQ Lyr |{Delta}(S) = 0:. BV Lyr |d = 0.025P. CC Lyr |P var. Max = 2433182.7 + 24.028d*E (JD2426100 - 33400); Max = CC Lyr |2437078.8 + 24.200d*E (JD2433400 - 37100) [00001]; Max = 2439418.5 CC Lyr |+ 24.185d*E (JD2437100 - 39420) [05644]; since JD2440400 - see CC Lyr |Table. Light curve shape var? [A/H] = -2.2. CV Lyr |Possible superposition of P2 = 135d. CX Lyr |P var. Max = 2418596.111 + 0.616689d*E (JD2414880 - 20000); Max = CX Lyr |2427696.396 + 0.616669d*E (JD2427530 - 30610); since JD2433000 - CX Lyr |see Table. {Delta}(S) = 7:. DD Lyr |P var. Max = 2425494.334 + 0.372610d*E (JD2418900 - 27600) [00001]; DD Lyr |since JD2427600 - see Table. DF Lyr |Min II 13.4. DI Lyr |P var. Max = 2437160.310 + 0.4174486d*E (JD2437160 - 39293); Max = DI Lyr |2439293.468 + 0.4178451d*E (JD2439293 - 40768); since JD2440768 - DI Lyr |see Table. DN Lyr |P2 = 600d. DR Lyr |[Fe/H] = -1.41; {Delta}(S) =7.4. DU Lyr |Min II 13.3. EN Lyr |B - V: + 0.40. + 0.43. P var. {Delta}(m) var. EP Lyr |Max I Phase = 0.20P; Min II 10.36m - 10.58m, Phase = 0.50P; Max II EP Lyr |10.01m - 10.10m, Phase = 0.70P. Secondary oscillations: P2 = 45.1d, EP Lyr |P3 = 7067d [09354]. EW Lyr |P var; nonlinear term: +0.00210d*10**(-6)*E**2 (JD2426500 - 45500); EW Lyr |since JD2442000 the observations are represented also by the EW Lyr |elements: Min = 2445597.391 + 1.948763d*E [07037,00001]. EX Lyr |[Fe/H] = -0.63; {Delta}(S) = 2.5. EZ Lyr |VB A (B 12.3m, 14", 302{deg}, 1934). P var. Since JD2426577 - see EZ Lyr |Table. {Delta}(S) = 7.1. FG Lyr |VB A (B 14m, <10"). d = 0.035P. P var? FH Lyr |P var? FK Lyr |The identification with HDE 337663(G5) [00021] is wrong. FL Lyr |Min II 9.52, DII = 0.05P. FN Lyr |B - V: +0.15, +0.48. FO Lyr |Min II 13.7. GY Lyr |The elements describe the brightest maxima. Between them there are GY Lyr |2 - 3 waves of smaller amplitude. Red. HP Lyr |Min II 11.0. HQ Lyr |P var, periodic term: +30d*sin(8{deg}*E). HT Lyr |Min II 13.3. HY Lyr |Min II 14.1. IK Lyr |Blazhko effect? IL Lyr |According to [00569], Max = 2429375.519 + 0.377620d*E, M - m = IL Lyr |0.14P:. IO Lyr |{Delta}(S) = 3. IP Lyr |Min II 13.3. IW Lyr |Min II 13.3. IY Lyr |Min II 14.1. KM Lyr |Blazhko effect: Pi = 30d, 0.14P <= M - m <= 0.20P. KP Lyr |ADS 11423 C (A 8.5m, B 9.7m; AB - C 77", 208{deg}; D 13.1m, C - D KP Lyr |14", 61{deg}, 1904). P2 = 1300d is possible. KR Lyr |P var. The light curve shape var. KT Lyr |Min II 14.9. KX Lyr |{Delta}(S) = 0. LQ Lyr |[Fe/H] = -1.39; {Delta}(S) = 7.2. LR Lyr |P var? [Fe/H] = -1.41; {Delta}(S) = 7.4. LT Lyr |Rapid variation (0.5m in an hour) were observed. LX Lyr |{Delta}(S) = 8:. LZ Lyr |P var. Min = 2425347.565 + 1.611143d*E (JD2425347 - 32119) [00569]; LZ Lyr |since JD2442870 - see Table. MN Lyr |Min II 14.1. MR Lyr |Alternative P = 0.66d:. MS Lyr |P < 0.5d? MT Lyr |Min II 16.2. MV Lyr |SB (Porb = 0.1336d [09373]). Quasiperiodic fadings of different MV Lyr |amplitude: Min = 2425558 + 455.5d*E (JD2425500 - 30100); Min = MV Lyr |2430113 + 325.3d*E (JD2430100 - 36900); Min = 2436944 + 357.8d*E MV Lyr |(JD2436900 - 44100) [09372]. After JD2444100 the mean brightness MV Lyr |level became fainter by 5m; outbursts with an amplitude up to 3m of MV Lyr |1 - 2 months duration are observed [09404]. During the bright level MV Lyr |of light, flickering up to 0.4m in 5 Min in U bAnd is observed MV Lyr |[00365]. Soft X-ray source. B - V: 0.00 +- 0.40; U - B: -0.86 + MV Lyr |-1.30. MW Lyr |P var. Max = 2429521.386 + 0.3978817d*E (JD2427700 - 36000); since MW Lyr |JD2436000 - see Table. Blazhko effect: Pi = 33.3d; the amplitude MW Lyr |varies by 0.6m. MZ Lyr |Min II 14.0. NV Lyr |d = 0.02P:. NW Lyr |P var. Max = 2436483.323 + 1.6012330d*E (JD2414500 - 36400) NW Lyr |[03506]; since JD2436400 - see Table. B - V: +0.38, +0.86. NY Lyr |Min II 13.1. NZ Lyr |O - C vary harmonically with an amplitude +- 0.01d, Pi ~2500P. OQ Lyr |VB (B 12.1m vis, 5.3", 175{deg}, 1930). OS Lyr |40d <= P <= 60d. P2 = 400d - 500d is superimposed. PQ Lyr |d = 0.014P; Min II 14.9. PS Lyr |d = 0.02P:; Min II 11.4. PU Lyr |Close companions sf, s. PV Lyr |d = 0.03P:. PY Lyr |Min II 13.4. P var. Min I = 2434980.4372 + 0.38576671d*E (JD2432700 PY Lyr |- 36900) [04248]; since JD2442500 - see Table. QQ Lyr |Min II 14.6. QT Lyr |Min II 14.6. QU Lyr |Min II 13.1. V0335 Lyr |Large scatter in the light curve. V0336 Lyr |P var. Min = 2429965.283 + 1.9049105d*E (JD2429370 - 31590); during V0336 Lyr |JD2438930 - 40010 - see Table. V0337 Lyr |Large scatter in the light curve. V0348 Lyr |Min II 16.8. The elements are valid during JD2444023 - 45232. V0350 Lyr |P var. The elements are valid during JD2438280 - 45232. V0355 Lyr |The elements are valid during JD2429322 - 45232. V0356 Lyr |VB A (B 17.5m, 10", 120{deg}, [00001]). V0361 Lyr |Min II 15.3, Max II 14.7, Max II - Min I = 0.70P. The elements are V0361 Lyr |valid during JD2433776 - 45232). V0372 Lyr |The chart in [03910] is wrong. Called GR256 in [06358] V454 Lyr. V0380 Lyr |Faint close companion nf. V0385 Lyr |Faint close companion sf. V0388 Lyr |No brightenings were observed during JD2438322 - 39289. V0389 Lyr |The elements are valid during JD2438322 - 40007. V0390 Lyr |The elements are valid during JD2439913 - 40007. V0401 Lyr |Min II 14.4:. The period may be spurious. V0403 Lyr |P var?, Pi = 500 P? V0404 Lyr |Min II 12.4. V0406 Lyr |Min II 13.0. V0409 Lyr |P var? The elements are valid during JD2434500 - 40000. Blazhko V0409 Lyr |effect? V0411 Lyr |Min II 14.4. Alternatively RRC (P = 0.291315d). V0412 Lyr |Min II 14.1; Min II - Min I = 0.48P. V0413 Lyr |Min II 14.8? V0415 Lyr |Cycle <= 150d. V0417 Lyr |Min II 16.2. P var? V0418 Lyr |P var. The elements are valid during JD2437100 - 40400. V0423 Lyr |Min II 15.5. P var? V0424 Lyr |Blazhko effect? V0428 Lyr |Min II 14.3. Apsidal motion? V0429 Lyr |Min II 14.8? V0431 Lyr |Min II 15.1. V0435 Lyr |Possibly ew with twice longer P. P may be spurious. V0462 Lyr |P var? The elements are valid during JD2439913 - 40007. V0467 Lyr |Min II 12.9. JD2415288 - 43287; the elements are valid during V0467 Lyr |JD2415288 - 43287; large scatter on the light curve. According to V0467 Lyr |[09412], during JD2443424 - 44165 the light variation range is V0467 Lyr |12.4m - 12.6m pg, the elements are not valid. V0470 Lyr |U = 0.40", p = 7{deg}. P1 = 738.6s, P2 = 557.4s, P3 = 318.0s, P4 = V0470 Lyr |291.9s, P5 = 259.1s. V0473 Lyr |P var, {Delta}(m) var. According to [09413], P = 1.490795d + V0473 Lyr |1.22d*10**(-6)*(JD - 2443600)/365.25d. Cyclic P variations: P V0473 Lyr |{alpha} = 1178.5d; Pt = 2655d. {Delta}(m) varies with the period P V0473 Lyr |{alpha}; P4 = 1063.5d may be traced in the variations of Vr. 0.06m V0473 Lyr |<= {Delta}(m) <= 0.36m. V0474 Lyr |P2 = 76d. V0477 Lyr |The central star of planetary nebula Abell 46. Strong reflection V0477 Lyr |effect. Depths of minima: Min I 1.42m B, Min II ~0.1m B. V0531 Lyr |Minima observed only between JD 2448600 and 2448800. V0550 Lyr |SB, Porb = 1.0309d. V0591 Lyr |MinII 13.85. V0592 Lyr |MinII 12.82. V0604 Lyr |According to [78265], P = 11.5791 d. V0608 Lyr |Called SBG 3268 in [78267], in contradiction with the star's V0608 Lyr |coordinates and brightness. V0609 Lyr |The period in the table is twice that in [78267], to justify the V0609 Lyr |suggested classification. V0627 Lyr |According to [78267], P = 3.34154 d. V0634 Lyr |The coordinates in [78266] are wrong. V0641 Lyr |P = 0.4599d is not excluded. V0664 Lyr |VB A (A 13.0mV; B 14.5mV, 11", 302{deg}, 1998). V0668 Lyr |Multiperiodic. V0691 Lyr |O'Connell effect. V0722 Lyr |A post-asymptotic-branch star with non-periodic, sometimes rapid, V0722 Lyr |brightness variations. V0723 Lyr |Multiperiodic, P2 = 0.0745095d. V0725 Lyr |VB A (B 16.7mpg, 6", 102{deg}, 2000). V0730 Lyr |SRB type with P = 85d is also possible. V0742 Lyr |Pulsations: P = 40d - 50d, amplitude 0.4m. V0753 Lyr |VB A (B 4", 178{deg}, 1998). V0754 Lyr |O'Connell effect. V0755 Lyr |O'Connell effect. V0757 Lyr |Periods 2.2148d or 2.8458d are also possible. V0758 Lyr |O'Connell effect. V0766 Lyr |O'Connell effect. V0775 Lyr |O'Connell effect. V0778 Lyr |RRC type with P = 0.29403d or P = 0.2270d is also possible. V0780 Lyr |VB A (B 17.1m, 5", 307{deg}, 1998). V0781 Lyr |VB A (B 17.3m, 6", 191{deg}, 1998). The one-day alias, P = V0781 Lyr |0.055562d, is also possible. V0784 Lyr |O'Connell effect. V0785 Lyr |Strong O'Connell effect. V0798 Lyr |Not red. V0817 Lyr |EW type with a twice longer period is not excluded. V0827 Lyr |VB A (B 5", 125{deg}, 2000); the range in the Table can be V0827 Lyr |influenced by the companion. Type EW with a twice longer period is V0827 Lyr |also possible. V0836 Lyr |Multiperiodic. P0 is presented in the Table; P1 = 0.090297d, P1/P0 V0836 Lyr |= 0.7746; other periods. V0846 Lyr |VB B (A 14.9mG; B 15.3mG, 19", 146{deg}, 2000); the range in the V0846 Lyr |Table can be influenced by the companion. V0868 Lyr |P varies? V0870 Lyr |Variations on the Palomar red plates: 16.3mR (1950 June 17) and V0870 Lyr |19.4mR (1987 June 21). The Table presents light elements for EA V0870 Lyr |variations during the high state. V0874 Lyr |The elements in the Table are for eclipses. ELL variations: P = V0874 Lyr |0.857724d, amplitude 0.02m. V0875 Lyr |VB A (B 9.1mV, 1".3, 126{deg}, 2015). The amplitude is for combined V0875 Lyr |brightness. V0897 Lyr |P = 0.734873d (that would correspond to the RRAB/RR0 type) is also V0897 Lyr |possible. V0903 Lyr |P varies [g0139]. alf Lyr |IR excess. bet Lyr |ADS 11745 A (B 8.6m, B7V, 46", 149{deg}; C 13.0m, 47", 248{deg}). bet Lyr |Min II 3.85. P var. Nonlinear terms: +3.883d*10**(-6)*E**2 - bet Lyr |0.10d*10**(-10)*E**3. Light curve shape var. Radio and X-ray bet Lyr |source. IR excess. del 2 Lyr |Open cluster {delta}**2 Lyr member [02505]. R Men |Sometimes P = 120d; Sometimes P = 240d. T Men |In the Large Magellanic Cloud region; not a member of the Cloud. T Men |There is a sguare term in the elements: +8.1d*10**(-6)*E**2. U Men |VB A (B 10.4m, 0.6", 71{deg}, 1935.3). A var (0.8m <= A <= 2.9M). P U Men |var. Max = 2416927 + 426.9d*E (JD2415200 - 17400) [00207]; since U Men |JD2417400 - see Table. V Men |Epoch corresponds to the middle of the light curve ascending V Men |branch. W Men |The member of the Large Magellanic Cloud. RR Men |Min II 12.1. RS Men |In the Large Magellanic Cloud region; not a member of the Cloud. RT Men |In the Large Magellanic Cloud region; not a member of the Cloud. RU Men |In the Large Magellanic Cloud region; not a member of the Cloud. RV Men |In the Large Magellanic Cloud region; not a member of the Cloud. RW Men |In the Large Magellanic Cloud region; not a member of the Cloud. TU Men |Porb = 0.1176d [09376]. Superhump Period Ps = 0.12625d [04772]. TY Men |Min II 8.47; d I = 0.00P, d II = 0.07P. Shape of the light curve TY Men |varies. TZ Men |Min II 6.36. UX Men |Min II 9.47; Min II - Min I = 0.50045P. One of the components may UX Men |be a physical variable. WY Men |In the region of the NGC 1841 globular cluster; not a member of the WY Men |cluster. In the halo of the magellanic clouds system. WZ Men |In the region of the NGC 1841 globular cluster, not a member of the WZ Men |cluster. In the halo of the Magellanic Clouds system. XX Men |In the region of the NGC 1841 globular cluster, not a member of the XX Men |cluster. In the halo of the Magellanic Clouds system. XY Men |In the Large Magellanic Cloud region; not a member of the Cloud. XY Men |Min II 10.88; dI = 0.05P; dII = 0.00P. XZ Men |There are there oscillations simultaneously: P1 = 0.1083d (A1 = XZ Men |0.0094m B), P2 = 0.0855d (A2 = 0.0082m B), P3 = 0.0955d (A3 = XZ Men |0.0058m B); P2/P1 = 0.789. AN Men |Type RRC: is also possible. AT Men |LMC non-member. AU Men |LMC non-member. BB Men |Min II = 11.80. P varies. dP/dt = +0.21 x 10^(-5) d/yr. BC Men |VB B (A 7.54m; AB 16", 260{deg}, 2000). iot Men |Min II 6.05. R Mic |P var. Max = 2413373 + 138.60d*E (JD2413300 - 29600) [00458]; Max = R Mic |2432745 + 137.43d*E (JD2429600 - 34700); Max = 2435091 + 140.84d*E R Mic |(JD2434700 - 37800); since JD2437800 - see Table. S Mic |P var. Max = 2413499 + 214.5d*E (JD2413500 - 15900) [00458]; Max = S Mic |2432102 + 208.23d*E (JD2422700 - 32200); since JD2432200 - see S Mic |Table. U Mic |OH, H2O emission. V Mic |OH, H20 emission. Y Mic |Mean brightness varies. Z Mic |(k - b)2 = 0.12; {Delta}(S) = 4. RR Mic |[A/H] = -1.4. P var. Max = 2433032.96 + 31.78175d*E (JD2415000 - RR Mic |35300) [02747]; since JD2443600 - see Table. RY Mic |P var? Elements given in the Table represent observations in the RY Mic |interval JD2436100 - 40210. According to [00085] Max = 2428670 + RY Mic |190d*E. RZ Mic |Min II 11.2. TV Mic |Min II 12.4. UZ Mic |Min II 12.4. VW Mic |In the interval JD2436600 - 840) Max = 2436807.248 + 0.35620d*E. VW Mic |Since JD2442600 - see Table. WY Mic |P = 0.511427d? [00001]. XZ Mic |In the interval JD2436670 - 840 Max = 2436731.480 + 0.449208d*E. XZ Mic |Since JD2442630 - see Table. ZZ Mic |(k - b)2 = 021; {Delta}(S) = 0. P var? Max = 2437192.3131 + ZZ Mic |0.0671786d*E (JD2437180 - 460) [04308]; Max = 2439320.2162 + ZZ Mic |0.0671575d*E (JD2439320 - 340) [05683]; since JD2440440 - see ZZ Mic |Table. Further period increase is possible [09380]. According to ZZ Mic |[07985] there are two simultaneous oscillations with the periods P1 ZZ Mic |and P2: P1 = 0.0654d, P2 = 0.0513d. P2/P1 = 0.784; A2(U) = 0.25 ZZ Mic |A1(U). AE Mic |In the interval JD2436670 - 840 Max = 2436728.470 + 0.324142d*E. AE Mic |Since JD2442630 - see Table. AH Mic |Min II 13.6. AT Mic |VB (A 10.83m V, M 4.5Ve; B 10.9m V, M 4.5Ve; a = 6.40", P = 675 yr, AT Mic |e = 0.60 [09381]. {mu}, Vr, {pi} - common with AU Mic. Unusually AT Mic |high freguency of flares allows to suppose that both components are AT Mic |variable. The range of combined brightness variation of the system AT Mic |is given in the Table. AU Mic |{mu}, {pi}, Vr - common with AT Mic. SB? 0.20P <= M - m <= 0.55P. AU Mic |There are periodical light variations and also flares with A <= AU Mic |0.5m U [08601]. AW Mic |Shape of the light curve strongly varies. Multiperiodicity is AW Mic |possible. AX Mic |In minimum brightness B - V = +1.42, U - B = +1.20. CZ Mic |MinII 12.9:. DE Mic |MinII 8.00. DS Mic |Period varies [81001]. DY Mic |Period varies strongly, the Table presents the mean period. EH Mic |Period varies? R Mon |Peculiar non-stellar object at the apex of the reflection variable R Mon |[09396] cometary nebula NGC 2261. Probably young star surrounded by R Mon |dust cloud. Light curve in [09394]. S Mon |In the open star cluster NGC 2264. VB A (B 8.2m, 2.9", 213{deg}; S Mon |9.9m, 16.6", 14{deg}.) T Mon |SB (Porb> = 70 yr [09397]). [A/H] = 0.3. There is a sguare term in T Mon |the elements given in the Table: +5.34d*10**(-6)*E**2. Deviations T Mon |from the parabola in the O - C, E diagram have a wave-like trend. T Mon |If this wave is attributed to the light-time effect, Porb = 100 T Mon |years. The observations are also satisfied by the following system T Mon |of linear elements: Max = 2412874.56 + 27.0093d*E (JD2405200 - T Mon |15250) [09398]; Max = 2426004.62 + 27.0180d*E (JD2415250 - 27150); T Mon |since JD2427150 - Max = 2436137.090 + 27.0205d*E [02392]. U Mon |P var. Min = 2408897 + 92.26d*E (JD2408800 - 36210) [00368]; since U Mon |JD2437300 - see Table. Mean magnitude varies with the period 2320d U Mon |[00657]. Spectrum investigation [02226]. V Mon |P var. Max = 2412172 + 334.5d*E (JD2412000 - 23500) [00458]; Max = V Mon |2427870 + 332.5d*E (JD2423500 - 28200); Max = 2429904 + 342.0d*E V Mon |(JD2428200 - 30800); Max = 2439570 + 331.6d*E (JD2430800 - 41225); V Mon |since JD2441225 - see Table. X Mon |P var. Max = 2415078 + 154.0d*E (JD2415000 - 18800); Max = 2419758 X Mon |+ 149.6d*E (JD2419700 - 21000); Max = 2421136 + 155.0d*E (JD2421000 X Mon |- 24600); Max = 2424673 + 169d*E (JD2424600 - 25600); Max = 2425644 X Mon |+ 155.6d*E (JD2425600 - 26800); Max = 2427028 + 150.7d*E (JD2427000 X Mon |- 28000) [00458]; Max = 2429521 + 155.8d*E (JD2428000 - 36300); Max X Mon |= 2438846 + 145.3d*E (JD2437800 - 38900); since JD2440800 - see X Mon |Table. The amplitude strongly varies; sometimes irregular light X Mon |variations are observed. Y Mon |P var. Max = 2415792 + 228.6d*E (JD2415300 - 19700); Max = 2419928 Y Mon |+ 227.4d*E (JD2419700 - 24300) [00458]; Max = 2432647 + 233.3d*E Y Mon |(JD2424300 - 32900); since JD2432900 - see Table. RR Mon |P var. Max = 2417476 + 384.5d*E (JD2417400 - 19600) [00458]; since RR Mon |JD2419600 - see Table. RU Mon |Min II 11.06; D II var: 0.06P <= DII <= 0.12P; Min II - Min I var: RU Mon |0.25P < = Min II - Min I <= 0.75P. P var. In the interval JD2429100 RU Mon |- 38409 Min I = 2418357.0140; 3.5846794d(E - 406) - 0.429d cos RU Mon |{alpha} + 0.06d*sin(2{alpha}) + 0.010d*cos(3{alpha}) + RU Mon |0.003d*sin(4{alpha}), MinII = 2418355.2220 + 3.5846794d(E - 406) + RU Mon |0.429d cos {alpha} + 0.060D*sin(2{alpha}) - 0.010d cos*3{alpha} + RU Mon |0.003d*sin(4{alpha}) (JD2416900 - 29100); Min I = 2429641.567 + RU Mon |3.5846391d*(E - 3554) - 0.429d*cos({alpha}) + 0.060d*sin(2{alpha}) RU Mon |+ 0.010d*cos(3{alpha}) + 0.003d*sin(4{alpha}), Min II = 2429639.775 RU Mon |+ 3.5846391d(E - 3554) + 0.429d*cos({alpha}) + 0.060d*sin(2{alpha}) RU Mon |- 0.010d*cos(3{alpha}) + 0.003d*sin(4{alpha}), where {alpha} = RU Mon |0.01245{deg}(E - 406) [03445]. The epochs E are being calculated RU Mon |for Min I from JD hel. 2416901.205, and for Min II - from JD hel. RU Mon |2416900.248. In the interval JD2438409 - 41743 Min I = 2438409.6045 RU Mon |+ 3.584586d(E - 6000) - 0.4290d*cos({alpha}) + RU Mon |0.0620d*sin(2{alpha}) + 0.0107d*cos(3{alpha}) + RU Mon |0.0026d*sin(4{alpha}) - 0.00036d cos 5{alpha}, Min II = RU Mon |2438407.8122 + 3.584586d(E - 6000) + 0.4290d cos {alpha} + RU Mon |0.0620d*sin(2{alpha}) - 0.0107d*cos(3{alpha}) + RU Mon |0.0026d*sin(4{alpha}) + 0.00036d*cos(5{alpha}), where {alpha} = RU Mon |0.012385{deg}(E - 406) [07987]. since JD2441743 - Min I = RU Mon |2441743.2633 + 3.584670d(E - 6930) - 0.4336d cos {alpha} + RU Mon |0.0634d*sin(2{alpha}) + 0.0111d*cos(3{alpha}) + RU Mon |0.0021d*sin(4{alpha}), Min II = 2441741.4710 + 3.584689d(E - 6930) RU Mon |+ 0.4336d cos {alpha} + 0.0634d*sin(2{alpha}) - RU Mon |0.0111d*cos(3{alpha}) + 0.0021d*sin(4{alpha}), where {alpha} = RU Mon |70.6{deg} + 0.0114{deg}(E - 6094) [09546]. Linear elements for Min RU Mon |I epochs in 1973 - 1990 are given in the Table. Corresponding RU Mon |elements for Min II epochs are: Min II = 2441741.575 + 3.584567d*E. RU Mon |E = 0.38. Apsidal motion period is 285 years. RV Mon |Mean brightness varies with P = 1047d. RW Mon |Min II 9.45; d I = 0.027P, d II = 0.023P. P var. Min I = RW Mon |2417943.687 + 1.9061012d*E (JD2417940 - 32900) [03450]; since RW Mon |JD2432900 - see Table. RX Mon |P var. Max = 2418980 + 343.2d*E (JD2416200 - 19000); Max = 2423097 RX Mon |+ 338.9d*E (JD2422000 - 28500); since JD2428500 - see Table. RY Mon |VB A (B 12.29M, 28"). SS Mon |In the region of the open cluster NGC 2264. SU Mon |S 5/7 - S 6/7. P var: 69d (JD2416700 - 19100); 203.5d (JD2420100 - SU Mon |22920); 69d (JD2423000 - 30100). In the intervals JD2423000 - 520 - SU Mon |const (11.5m), JD2424820 - 980 - const (11.8m). SV Mon |[A/H] = 0.2. P var. Max = 2419041.805 + 15.230721d*E (JD2412000 - SV Mon |22000) [00025]; Max = 2422651.931 + 15.23256d*E (JD2422600 - 23850) SV Mon |[09400]; Max = 2424571.60 + 15.2513d*E (JD2423850 - 24600); Max = SV Mon |2434045.326 + 15.2304d*E (JD2424600 - 34100); since JD2433000 - see SV Mon |Table. SX Mon |Mean brightness varies with P = 1100d. SZ Mon |VB A (B 11m - 12m, 10" [09401]). Min II 10.55. P var. Min I = SZ Mon |2426357.1 + 32.760d*E (JD2422000 - 26400); Min I = 2427861.2 + SZ Mon |32.708d*E (JD2426750 - 32000); since JD2432800 - see Table. Shape SZ Mon |of the light curve varies. Heights of maxima and depths of minima SZ Mon |are constant. TU Mon |Min II 9.1. TV Mon |In the region of the open star cluster NGC 2237. TW Mon |Wachmann [03453] assigns the variable to the RRab type with the TW Mon |elements Max = 2433001.371 + 0.8743887*E, but notes a considerable TW Mon |dispersion of the points around the mean light curve obtained with TW Mon |this period. As the periods by Hessner (PH) and Wachmann (PW) are TW Mon |mutually related (1/PW ~1/PH + 1) it is more probable on account of TW Mon |the above mentioned circumstance that the variable belongs to TW Mon |cepheids. TX Mon |[A/H] = -0.3. UV Mon |The form of the light curve being unusual for RR Lyr type variables UV Mon |(Max II 13.5 at the phase 0.39P, Min II 13.8 at the phase 0.22P), UV Mon |the period may be doubtful, though it was found independently by UV Mon |two investigators [00380,03453]. UX Mon |Min II 8.52; dI = 0.044P. P var? Brightness in maximum varies with UX Mon |the amplitude up to 0.2m. VV Mon |Min II 9.55; dI = dII = 0.07P. There is a square term in the VV Mon |elements given in the Table: -0.12d*10**(-7)*E**2. VW Mon |P var. Max = 2425243.40 + 0.6041350d*E (JD2414700 - 30700); since VW Mon |JD2430700 - see Table. In [00386,05448] And other previous works VW Mon |the spurious period value 1.532d is being accepted suggesting the VW Mon |curious nature of the variable. Serious observations are necessary VW Mon |to select the true value of the period. VX Mon |Depth of Min II 0.07m. VY Mon |In the region of the nebula IC 446. XX Mon |[A/H] = -0.2. XZ Mon |Min II 13.6; d = 0.02P:. AA Mon |[A/H] = -0.9. P var. Max = 2430788.266 + 3.938052d*E (JD2425300 - AA Mon |34800) [03453]; since JD2434800 - see Table. AC Mon |In the region of the open cluster NGC 2323. AK Mon |P var. Max = 2425279 + 319.2d*E (JD2425200 - 28000); since AK Mon |JD2428000 - see Table. AN Mon |Min II 11.7:; d = 0.027P. AO Mon |Min II 10.16; DII = 0.14P; Min II - Min I = 0.4933P. P var. Min I = AO Mon |2426735.333 + 1.884758d*E (JD2426700 - 40000); since JD2440000 - AO Mon |see Table. AQ Mon |Min II 10.9; DII = 0.05P; dI = 0.014P. AR Mon |Min II 9.03; d = 0.011P. There is a square term in the elements AR Mon |given in the Table: -1.22d*10**(-6)*E**2. AU Mon |Min II 8.2:. Shape of the light curve varies. Brightness in maximum AU Mon |varies periodically with the amplitude 0.2m: Max = 2443105 + AU Mon |411d*E; M - m = 0.5P. AV Mon |Depth of Min II 0.04m. AW Mon |P var. Min = 2425649.053 + 20.797d*E (JD2425500 - 26400) [09408]; AW Mon |Min = 2426439.340 + 20.81905d*E (JD2426400 - 35900) [00511]; since AW Mon |JD2435900 - see Table. AX Mon |Binary system with an envelope and gaseous streams. Porb = 232.60d AX Mon |[06103]. Spectrum investigation [09411]. Epoch of Min brightness AX Mon |preceeding the moment of conjunction for 0.25p is given in the AX Mon |Table; A = 0.4m U. Besides periodical variations, there are rapid AX Mon |light fluctuations up to 0.1m. BB Mon |Depth of Min II 0.04m. BC Mon |P var. Max = 2421240 + 275.8d*E (JD2421200 - 25960); Max = 2428880 BC Mon |+ 267.2d*E (JD2425960 - 30000); since JD2430000 - see Table. BE Mon |{Delta}(S) = 0. BH Mon |d = 0.01p:. BM Mon |Min II 12.3. According to [09415], apsidal motion is possible. BO Mon |Min II 10.1. P var. Min I = 2428211.596 + 2.2251753d*E (JD2415000 - BO Mon |36000) [00007]; since JD2436000 - see Table. BP Mon |P var? Elements given in the Table are valid in the interval BP Mon |JD2425600 - 29700. BT Mon |VB A (B 16.0m, 10", 0{deg}). After the outburst in 1939 the BT Mon |brightness varies in the range 16.0m - 18.7m with the elements: Min BT Mon |= 2443491.7155 + 0.3338141d*E; D = 0.20p, 0 <= d < = 0.03p. Before BT Mon |the outburst in 1939, according to [09417], the following elements BT Mon |were valid: Min = 2429500.207 + 0.3338010d*E. Emission nebula with BT Mon |the radius of 3.8" was discovered in 1981 around the nova [09148]. BX Mon |Usually was considered as mira type variable [09421]. In the Table BX Mon |the epoch of light maximum and the period are given according to BX Mon |[09419]. According to [09420] the Balmer emission lines originate BX Mon |in the nebulosity surrounding the symbiotic system and are excited BX Mon |by the hot component, and light variations are due to the orbital BX Mon |motion in the system. BZ Mon |d = 0.030P. In the region of the open cluster CR 106. CC Mon |In the region of the open cluster CR 106. CD Mon |P var. Max = 2427704 + 273.8d*E (JD2427400 - 30400); since CD Mon |JD2430400 - see Table. CE Mon |Min II 14.2. CF Mon |Min II 13.7; d = 0.02P:. CH Mon |d = 0.030P. CS Mon |VB A (B 13m, 9", 0{deg}). CT Mon |In the region of the open cluster NGC 2244. CU Mon |[A/H] = -0.2. CV Mon |In the centre of an anonymous open cluster. VB A (B 13.76m, 10", CV Mon |270{deg}; C 13.72m, 14", 270{deg}). P var. Max = 2429805.142 + CV Mon |5.378782d*E (JD2429360 - 36000); since JD2436000 - see Table. DD Mon |Min II 11.3. DF Mon |The chart in [05285] is wrong, the star observed was not DF Mon. DN Mon |Min II 13.9. DR Mon |In the region of the open cluster Cr 106. DT Mon |P var. Max = 2425324 + 345d*E (JD2425300 - 28200) In the interval DT Mon |JD2429250 - 37700 there were cycles 119d, 230d, 350d. DW Mon |In the region of the open cluster NGC 2286. EE Mon |P var. Max = 2425300.42 + 4.80776d*E (JD2425300 - 27720); since EE Mon |JD2427720 - see Table. EH Mon |d = 0.023P. EK Mon |P var. Max = 2425302.59 + 3.95773d*E (JD2425200 - 33000) [00387]; EK Mon |since JD2433000 - see Table. EP Mon |d = 0.026P. ES Mon |d = 0.02P. EW Mon |Min II 14.2. FH Mon |Depth of Min II 0.04m. FP Mon |In the region of the open cluster NGC 2353. FS Mon |Min II 11.2. FU Mon |S 6.5/7.5. FW Mon |d = 0.016P. Depth of Min II 0.04m. FX Mon |OH emission. FZ Mon |The elements should be checked. GH Mon |Min II 13.1. GP Mon |In the region of the open cluster NGC 2264. GQ Mon |In the region of the open cluster NGC 2264. GR Mon |In the region of the open cluster NGC 2264. GU Mon |Min II 12.5. GV Mon |Depth of Min II 0.04m. GX Mon |OH, H2O, SIO maser. HI Mon |Min II 9.9. HM Mon |Min II 13.6. P var. Min I = 2430110.1948 + 0.40765737d*E (JD2429600 HM Mon |- 35400) [05285]; since JD2435400 - see Table. HO Mon |d = 0.03P. HP Mon |d = 0.04P:. HR Mon |Depth of Min II 0.03m. HY Mon |Min II 12.4. IL Mon |d = 0.03P. IM Mon |Min II 6.47. IO Mon |In the region of the open cluster NGC 2264. IP Mon |In the region of the open cluster NGC 2264. IQ Mon |In the region of the open cluster NGC 2264. IR Mon |P var? IS Mon |Depth of Min II 0.05m. IX Mon |Min II 12.8. IZ Mon |Min II 12.0. KU Mon |In the region of the open cluster NGC 2264. KV Mon |In the region of the open cluster NGC 2264. KW Mon |In the region of the open cluster NGC 2264. KX Mon |In the region of the open cluster NGC 2264. KY Mon |In the region of the open cluster NGC 2264. KZ Mon |In the region of the open cluster NGC 2264. LL Mon |In the region of the open cluster NGC 2264. LM Mon |In the region of the open cluster NGC 2264. LN Mon |In the region of the open cluster NGC 2264. LO Mon |In the region of the open cluster NGC 2264. LP Mon |In the region of the open cluster NGC 2264. LQ Mon |In the region of the open cluster NGC 2264. LR Mon |In the region of the open cluster NGC 2264. LS Mon |In the region of the open cluster NGC 2264. LT Mon |In the region of the open cluster NGC 2264. LU Mon |In the region of the open cluster NGC 2264. LV Mon |In the region of the open cluster NGC 2264. LW Mon |In the region of the open cluster NGC 2264. LX Mon |In the region of the open cluster NGC 2264. LY Mon |In the region of the open cluster NGC 2264. LZ Mon |In the region of the open cluster NGC 2264. MM Mon |In the region of the open cluster NGC 2264. MN Mon |In the region of the open cluster NGC 2264. MO Mon |VB A (B 20m, 10", 356{deg}); in the region of the open cluster NGC MO Mon |2264. MP Mon |In the region of the open cluster NGC 2264. MQ Mon |In the region of the open cluster NGC 2264. MX Mon |Min II 11.7. NN Mon |Min II 12.9. NS Mon |Min II 11.1. NT Mon |In the region of the open cluster NGC 2264. NU Mon |In the region of the open cluster NGC 2264. NV Mon |In the region of the open cluster NGC 2264. NW Mon |In the region of the open cluster NGC 2264. NX Mon |In the region of the open cluster NGC 2264. NY Mon |In the region of the open cluster NGC 2264. NZ Mon |In the region of the open cluster NGC 2264. OO Mon |In the region of the open cluster NGC 2264. OP Mon |In the region of the open cluster NGC 2264. OQ Mon |In the region of the open cluster NGC 2264. OR Mon |In the region of the open cluster NGC 2264. OS Mon |In the region of the open cluster NGC 2264. OT Mon |In the region of the open cluster NGC 2264. OU Mon |In the region of the open cluster NGC 2264. OV Mon |In the region of the open cluster NGC 2264. OW Mon |In the region of the open cluster NGC 2264. OX Mon |VB A (B 15m, 7", 35{deg}); in the region of the open cluster NGC OX Mon |2264. OY Mon |In the region of the open cluster NGC 2264. OZ Mon |In the region of the open cluster NGC 2264. PP Mon |In the region of the open cluster NGC 2264. PQ Mon |In the region of the open cluster NGC 2264. PR Mon |The elements should be checked. PT Mon |In the region of the open cluster NGC 2264. PU Mon |In the region of the open cluster NGC 2264. PV Mon |In the region of the open cluster NGC 2264. PW Mon |In the region of the open cluster NGC 2264. PX Mon |In the region of the open cluster NGC 2264. PY Mon |In the region of the open cluster NGC 2264. QR Mon |290d <= P <= 400d. Depth of Min varies by 0.9m with the period QR Mon |about 2000d. QT Mon |In the region of the open cluster NGC 2264. QU Mon |In the region of the open cluster NGC 2264. QV Mon |In the region of the open cluster NGC 2264. QW Mon |In the region of the open cluster NGC 2264. QX Mon |In the region of the open cluster NGC 2264. QY Mon |In the region of the open cluster NGC 2264. QZ Mon |In the region of the open cluster NGC 2264. V0335 Mon |In the region of the open cluster NGC 2264. V0336 Mon |In the region of the open cluster NGC 2264. V0337 Mon |In the region of the open cluster NGC 2264. V0338 Mon |In the region of the open cluster NGC 2264. V0339 Mon |In the region of the open cluster NGC 2264. V0340 Mon |In the region of the open cluster NGC 2264. V0341 Mon |In the region of the open cluster NGC 2264. V0342 Mon |In the region of the open cluster NGC 2264. V0343 Mon |In the region of the open cluster NGC 2264. V0344 Mon |In the region of the open cluster NGC 2264. V0345 Mon |In the region of the open cluster NGC 2264. V0346 Mon |In the region of the open cluster NGC 2264. V0347 Mon |VB A (B 20m, 12", 120{deg}); in the region of the open cluster NGC V0347 Mon |2264. V0348 Mon |In the region of the open cluster NGC 2264. V0349 Mon |In the region of the open cluster NGC 2264. V0350 Mon |In the region of the open cluster NGC 2264. V0351 Mon |In the region of the open cluster NGC 2264. V0352 Mon |In the region of the open cluster NGC 2264. V0353 Mon |In the region of the open cluster NGC 2264. V0354 Mon |In the region of the open cluster NGC 2264. V0355 Mon |In the region of the open cluster NGC 2264. V0356 Mon |VB (3", 78{deg}); in the region of the open cluster NGC 2264. V0357 Mon |In the region of the open cluster NGC 2264. V0358 Mon |In the region of the open cluster NGC 2264. V0359 Mon |In the region of the open cluster NGC 2264. V0360 Mon |In the region of the open cluster NGC 2264. V0361 Mon |In the region of the open cluster NGC 2264. V0362 Mon |In the region of the open cluster NGC 2264. V0363 Mon |In the region of the open cluster NGC 2264. V0364 Mon |In the region of the open cluster NGC 2264. V0365 Mon |VB B (A = V591 Mon, B 7", 135{deg}); in the region of the open V0365 Mon |cluster NGC 2264. V0366 Mon |In the region of the open cluster NGC 2264. V0367 Mon |In the region of the open cluster NGC 2264. V0368 Mon |VB (9", 252{deg}); in the region of the open cluster NGC 2264. V0369 Mon |VB (11", 264{deg}); in the region of the open cluster NGC 2264. V0370 Mon |VB (8", 97{deg}); in the region of the open cluster NGC 2264. V0371 Mon |In the region of the open cluster NGC 2264. V0372 Mon |SC 7/7.5. V0373 Mon |In the region of the open cluster NGC 2264. V0379 Mon |d = 0.015P:. V0380 Mon |Min II 12.9; P = 1.98904166d? V0383 Mon |Min II 15.2. V0384 Mon |Min II 13.0. V0389 Mon |Min II 14.9. V0393 Mon |Min II 14.3. V0394 Mon |d = 0.02P; depth of Min II 0.04m. V0395 Mon |d = 0.03P. V0396 Mon |Min II 13.5. V0397 Mon |Min II 11.9. V0398 Mon |In the region of the open cluster NGC 2264. V0399 Mon |In the region of the open cluster NGC 2264. V0400 Mon |In the region of the open cluster NGC 2264. V0401 Mon |In the region of the open cluster NGC 2264. V0402 Mon |In the region of the open cluster NGC 2264. V0403 Mon |In the region of the open cluster NGC 2264. V0404 Mon |d = 0.02P:. V0405 Mon |In the region of the open cluster NGC 2264. V0406 Mon |In the region of the open cluster NGC 2264. V0407 Mon |In the region of the open cluster NGC 2264. V0408 Mon |In the region of the open cluster NGC 2264. V0409 Mon |In the region of the open cluster NGC 2264. V0410 Mon |In the region of the open cluster NGC 2264. V0411 Mon |In the region of the open cluster NGC 2264. V0412 Mon |In the region of the open cluster NGC 2264. V0413 Mon |In the region of the open cluster NGC 2264. V0414 Mon |In the region of the open cluster NGC 2264. V0415 Mon |In the region of the open cluster NGC 2264. V0416 Mon |In the region of the open cluster NGC 2264. V0417 Mon |In the region of the open cluster NGC 2264. V0418 Mon |In the region of the open cluster NGC 2264. V0419 Mon |In the region of the open cluster NGC 2264. V0420 Mon |In the region of the open cluster NGC 2264. V0421 Mon |In the region of the open cluster NGC 2264. V0422 Mon |In the region of the open cluster NGC 2264. V0423 Mon |In the region of the open cluster NGC 2264. V0424 Mon |In the region of the open cluster NGC 2264. V0425 Mon |In the region of the open cluster NGC 2264. V0426 Mon |VB A (B = NSV 3125 17.0m, 6", 117{deg}); in the region of the open V0426 Mon |cluster NGC 2264. V0427 Mon |In the region of the open cluster NGC 2264. V0428 Mon |In the region of the open cluster NGC 2264. V0429 Mon |In the region of the open cluster NGC 2264. V0430 Mon |In the region of the open cluster NGC 2264. V0431 Mon |In the region of the open cluster NGC 2264. V0432 Mon |In the region of the open cluster NGC 2264. V0433 Mon |In the region of the open cluster NGC 2264. V0434 Mon |In the region of the open cluster NGC 2264. V0435 Mon |In the region of the open cluster NGC 2264. V0436 Mon |In the region of the open cluster NGC 2264. V0437 Mon |In the region of the open cluster NGC 2264. V0438 Mon |In the region of the open cluster NGC 2264. V0439 Mon |In the region of the open cluster NGC 2264. V0440 Mon |In the region of the open cluster NGC 2264. V0441 Mon |In the region of the open cluster NGC 2264. V0442 Mon |Min II 11.6. V0443 Mon |In the region of the open cluster NGC 2264. V0444 Mon |In the region of the open cluster NGC 2264. V0445 Mon |Min II 11.3. V0446 Mon |[A/H] = -0.7. V0447 Mon |[A/H] = -1.4. V0448 Mon |Min II 9.8. V0449 Mon |d = 0.02P. V0450 Mon |Min II 12.6. V0451 Mon |Min II 14.7. V0452 Mon |Min II 12.7; d = 0.02P. V0453 Mon |Min II 11.8. V0454 Mon |Min II 12.2. V0455 Mon |Min II 15.3. V0456 Mon |Min II 13.7. V0457 Mon |Min II 14.3; d = 0.03P:. V0458 Mon |Min II 13.8. V0459 Mon |Min II 14.7. V0460 Mon |Min II 10.7. V0463 Mon |d = 0.03P; P = 2.2476768d? V0464 Mon |Min II 12.3. V0465 Mon |P var. Max = 2429642.44 + 2.71341d*E (JD2425600 - 30800) [03551]; V0465 Mon |Max = 2431845.65 + 2.713212d*E (JD2430000 - 35200) [03453]; Max = V0465 Mon |2435541.315 + 2.713668d*E (JD2435200 - 41600); since JD2441600 - V0465 Mon |see Table. V0466 Mon |VB A (B 15m, 135{deg}). V0474 Mon |(k - b)2 = 0.32. Blazhko effect: Max(O - C) = 2441664.962 + V0474 Mon |7.74639d*N; Min(O - C) = 2441669.569 + 7.74639d*N; 0.03m <= A <= V0474 Mon |0.37m; -0.02d <= O - C <= +0.03d. Freguency analysis gives three V0474 Mon |principal oscillations [08669]: P1 = 0.1361258d (A1 = 0.18m), P2 = V0474 Mon |0.1337745d (A2 = 0.12m), P3 = 0.1385591d (A3 = 0.04m). V0478 Mon |In the region of the nebula IC 2169. V0479 Mon |In the region of the nebula IC 2169. V0481 Mon |In the region of the nebula IC 2169. V0482 Mon |In the region of the nebula IC 2169. V0483 Mon |In the region of the nebula IC 2169. V0486 Mon |VB A (B 18.4M, 6"). In the region of the nebula NGC 2245. V0487 Mon |In the region of the nebula NGC 2245. V0488 Mon |In the region of the nebula NGC 2245. V0489 Mon |In the region of the nebula NGC 2245. V0490 Mon |In the region of the nebula NGC 2247. V0493 Mon |In the region of the open cluster Tr 5. V0494 Mon |Depth of Min II 0.05m. V0496 Mon |Min II 12.8. V0497 Mon |8.9 - 11.8 IR. V0498 Mon |P = 2.4727818d? V0500 Mon |In the region of the open cluster NGC 2264. V0501 Mon |Min II 13.1; Min II - Min I = 0.445P; DII = 0.036P. V0503 Mon |9.2 - 10.9 IR. V0505 Mon |Min II 7.55. V0507 Mon |SB2 (P = 53.781d [09483]); d = 0.015P:. V0510 Mon |[A/H] = -0.1. V0513 Mon |Depth of Min II 0.04m. V0514 Mon |Min II 13.3. V0515 Mon |Min II 12.7. V0521 Mon |Min II 10.4. V0524 Mon |Min II 15.2. V0526 Mon |P var. Max = 2433304.284 + 2.675208d*E (JD2429300 - 35170); since V0526 Mon |JD2439170 - see Table. V0527 Mon |Depth of Min II 0.05m. V0530 Mon |Min II 12.8. V0532 Mon |Min II 12.8. RRC? V0535 Mon |P var. Max = 2431846.445 + 0.3328791d*E (JD2429600 - 34060); since V0535 Mon |JD2434060 - see Table. [Fe/H] = -1.44. V0539 Mon |In the region of the open cluster NGC 2244. V0540 Mon |In the region of the nebula IC 446. V0541 Mon |In the region of the nebula IC 446. V0542 Mon |In the region of the nebula IC 446. V0543 Mon |In the region of the open cluster NGC 2244. V0544 Mon |In the region of the open cluster NGC 2244. V0545 Mon |In the region of the open cluster NGC 2244. V0546 Mon |In the region of the open cluster NGC 2244. V0547 Mon |In the region of the open cluster NGC 2244. V0548 Mon |In the region of the open cluster NGC 2244. V0549 Mon |In the region of the open cluster NGC 2244. V0550 Mon |VB A (B 17.3m, 6", 0{deg} ); in the region of the open cluster NGC V0550 Mon |2244. V0551 Mon |In the region of the open cluster NGC 2244. V0552 Mon |In the region of the open cluster NGC 2244. V0553 Mon |In the region of the open cluster NGC 2244. V0554 Mon |In the region of the open cluster NGC 2244. V0555 Mon |In the region of the open cluster NGC 2244. V0556 Mon |In the region of the open cluster NGC 2244. V0557 Mon |In the region of the open cluster NGC 2244. V0560 Mon |Depth of Min II 0.05m. V0565 Mon |Connected with the diffuse nebula NGC 2313 having diameter of 10" V0565 Mon |and a faint cometary nebula. V0569 Mon |VB A (B 10.8m, 6.2", 281{deg}; C 10.5m, 38.3", 295{deg}). The range V0569 Mon |of combined light variation of A and B components is given. V0569 Mon |According to [08215], P = 0.18d. V0571 Mon |(k - b)2 = 0.32. Non-radial pulsation with variable periods: P1 = V0571 Mon |0.0999081d (A1 = 0.052m), P2 = 0.0749998d (A2 = 0.015m) (JD2440914 V0571 Mon |- 41692) [07127]; P1 = 0.0894534d (A1 = 0.038m), P2 = 0.15988d (A2 V0571 Mon |= 0.025m), P3 = 0.106516d (A3 = 0.014m). P4 = 0.26998d (A4 = V0571 Mon |0.012m), P5 = 0.15069d (A5 = 0.011m) (JD2441662 - 719) [09450]. V0577 Mon |VB (A 11.3m V, B 14.8m V; a = 0.312", P = 16.60 yr, e =0.38). Both V0577 Mon |components are probably variables. The range of combined light V0577 Mon |variation of the system is given in the Table [06146]. V0578 Mon |In the region of the open cluster NGC 2244. V0579 Mon |In the region of the open cluster NGC 2264. V0580 Mon |In the region of the open cluster NGC 2264. V0581 Mon |In the region of the open cluster NGC 2264. V0582 Mon |In the region of the open cluster NGC 2264. V0583 Mon |In the region of the open cluster NGC 2264. V0584 Mon |In the region of the open cluster NGC 2264. V0585 Mon |In the region of the open cluster NGC 2264. V0586 Mon |In the region of the open cluster NGC 2264. V0588 Mon |In the region of the open cluster NGC 2264. V0589 Mon |In the region of the open cluster NGC 2264. V0590 Mon |VB (10", 358{deg}); in the region of the open cluster NGC 2264. V0591 Mon |VB A (B = V365 Mon, 7", 135{deg}); in the region of the open V0591 Mon |cluster NGC 2264. V0593 Mon |In the region of the open cluster NGC 2264. V0594 Mon |In the region of the open cluster NGC 2264. V0595 Mon |In the region of the open cluster NGC 2264. V0596 Mon |In the region of the open cluster NGC 2264. V0597 Mon |In the region of the open cluster NGC 2264. V0598 Mon |In the region of the open cluster NGC 2264. V0599 Mon |In the region of the open cluster NGC 2264. V0600 Mon |In the region of the open cluster NGC 2264. V0601 Mon |In the region of the open cluster NGC 2264. V0602 Mon |In the region of the open cluster NGC 2264. V0603 Mon |In the region of the open cluster NGC 2264. V0604 Mon |In the region of the open cluster NGC 2264. V0605 Mon |In the region of the open cluster NGC 2264. V0606 Mon |In the region of the open cluster NGC 2264. V0607 Mon |In the region of the open cluster NGC 2264. V0608 Mon |In the region of the open cluster NGC 2264. V0609 Mon |In the region of the open cluster NGC 2264. V0610 Mon |In the region of the open cluster NGC 2264. V0611 Mon |In the region of the open cluster NGC 2264. V0612 Mon |In the region of the open cluster NGC 2264. V0613 Mon |S 3/2. V0616 Mon |Novalike outbursts were observed in 1917 (Max JD2421540) and in V0616 Mon |1975 (Max JD2442646). In quiescent state probably ellipsoidal light V0616 Mon |variation is observed with P = 0.325d and A = 0.2m [09458], and V0616 Mon |also slower light variations with P = 7.39d [09459] or 7.8d V0616 Mon |[09460]. Spectrum description [09461,09462]. V0624 Mon |In the region of the open cluster Cr 106. V0628 Mon |In the region of the open cluster NGC 2264. V0629 Mon |In the region of the open cluster NGC 2264. V0630 Mon |VB A (B 21m, 3", 300{deg}); in the region of the open cluster NGC V0630 Mon |2264. V0632 Mon |In the region of the open cluster NGC 2368. V0637 Mon |Basic oscillation with A1 = 0.05m and elements given in the Table V0637 Mon |is superimposed by the second one with A2 = 0.02m and the elements: V0637 Mon |Max = 2443496.1624 + 0.19740d*E. Beat period Pb = 6.09d. V0638 Mon |VB (6.5m, 8.5m; 0.8", 178{deg}). V0640 Mon |In the region of the open cluster NGC 2244. Porb = 14.39604d V0640 Mon |[06103]. Irregular light variations. Probably transitional stage V0640 Mon |from a binary system of O stars to a system of WR type [04107]. V0641 Mon |VB A (B 10.91m, 21.4", 310{deg}; C 12.46m, 25.8", 285{deg}). In the V0641 Mon |region of the open cluster NGC 2264. V0642 Mon |In the region of the open cluster NGC 2264. Cluster non-member. V0642 Mon |Epoch of light minimum is given in the Table. V0645 Mon |Epoch of light minimum is given in the Table. V0741 Mon |Type ACV: is also possible. V0750 Mon |In the region of the nebula IC 2177. V0753 Mon |Type ACV: is also possible. V0851 Mon |Cluster non-member. V0852 Mon |The depth of MinII is at least 0.07. V0853 Mon |MinII 16.05. V0857 Mon |MinII 15.98. V0858 Mon |MinII 15.87. V0859 Mon |MinII 14.50. Cluster non-member? V0860 Mon |MinII 9.38. V0861 Mon |MinII 12.7. V0863 Mon |MinII 9.13. V0875 Mon |Multiple (A 12.6mV; B 13.4mV, 18", 218{deg}; C = var, 14.51mV, 10", V0875 Mon |101{deg}; D 15.8mV, 12", 168{deg}, 1990). The tabulated variability V0875 Mon |range could be influenced by the companions. V0878 Mon |O'Connell effect. V0879 Mon |VB (A 8.4m, B 10.4m, 7", 265{deg}, 1999). V0880 Mon |VB A (A 8.7m; B 9.9m, 14", 300{deg}, 1991). Combined magnitudes are V0880 Mon |tabulated. V0898 Mon |VB A (B 15.0mpg, 19", 173{deg}, 1999). V0900 Mon |Min II = 12.65. V0901 Mon |The tabulated light elements are for the fundamental mode. First V0901 Mon |overtone: Max = 2453724.711 + 1.61404d x E. V0902 Mon |Several longer period aliases are also possible. V0903 Mon |Min II = 12.80. V0904 Mon |Min II = 12.68. V0906 Mon |Min II = 10.82. V0907 Mon |Min II = 10.57. V0908 Mon |Min II = 11.54. V0909 Mon |Min II = 10.63. V0910 Mon |Min II = 11.39. V0912 Mon |VB A (B 14.4m, 3"s). V0915 Mon |Min II = 11.15. V0917 Mon |Min II = 9.93. V0919 Mon |Min II = 11.7. V0920 Mon |Min II = 7.48. VB AB (A 7.74m, A2:V:m, SB, Porb = 6.7663d; B 9.18m, V0920 Mon |G8IIIe, SB, Porb = 4.4813d; AB 0.9", 37{deg}, 1995). Component A V0920 Mon |varies. V0922 Mon |Min II = 11.38. V0925 Mon |Min II = 8.52. V0927 Mon |Min II = 11.16. V0929 Mon |Min II = 13.7. V0930 Mon |Min II = 8.40. V0931 Mon |VB AB (A 10.49m; B 11.10m, 3.3", 282{deg}, 1999). V0934 Mon |Min II = 13.4. V0935 Mon |Min II = 9.9. Min II - MinI = 0.78P. V0936 Mon |Min II = 14.2. V0937 Mon |Min II = 8.84. Light elements for eclipses are tabulated. V0937 Mon |Pulsations with P = 0.110480d and amplitude about 0.08m. V0938 Mon |Min II = 15.0 :. V0948 Mon |Min II = 13.7. V0953 Mon |Min II = 14.4. Type RRC with a twice shorter period is not V0953 Mon |excluded. V0960 Mon |In a nebula. V0962 Mon |SB2, Porb = 5.32d; the F2V component varies. Multiperiodic; other V0962 Mon |periods are P2 = 0.77214d and P3 = 0.68432d. V0964 Mon |VB AB (12.5m, 13.0m, 2".7, 213{deg}, 2000). V0965 Mon |Blazhko effect, P=37.24d. V0966 Mon |Pulsates in the first (see Table) and second (Max = 2453761.54 + V0966 Mon |0.85905d x E) overtone modes. P2/P1 = 0.8043. V0972 Mon |A period of 0.948d was also detected. V0973 Mon |The amplitude of periodic variations (see Table) is 0.08m; a single V0973 Mon |flare was observed. V0975 Mon |Light elements for eclipses are tabulated. Outside eclipses, P = V0975 Mon |3.25d, amplitude 0.03m. VB A (B = NSV 03138, 16.1 - 16.7mV, 7", V0975 Mon |357{deg}, 1999). V0979 Mon |The light elements for the first overtone are given in the Table. V0979 Mon |Second overtone: Max = 2453800.32 + 1.03153 x E. P2/P1 = 0.8005. V0982 Mon |VB A (B 14.35mF, 10", 256{deg}, 1998). V0985 Mon |Pulsates in the first (see Table) and second (Max = 2453674.01 + V0985 Mon |0.70772d x E) overtone modes. P2/P1 = 0.8046. V0988 Mon |P = 0.36319d is also possible. V0989 Mon |VB A (B 6", 264{deg}, 1998). V1014 Mon |VB (A 9.52m, B 10.56m; AB 3", 194{deg}, 2001). The magnitude range V1014 Mon |in the Table is for combined brightness. S Mus |Marked on the chart for BO Mus. Max II = Max I, Phase (Max II) = S Mus |0.15P. P var? SB 1 (Porb = 506.4d). T Mus |P2 = 1021d. V Mus |In the Coal Sack region. RV Mus |P = 128d: is possible. RW Mus |P = 130d: is possible. RY Mus |V1 (NGC 4833). RZ Mus |V2 (NGC 4833). Cluster non-member. SY Mus |Min II 11.2; Min I - Min II = 170d. Elements for Min I of SY Mus |quasiperiodic variations observed during JD2434910 - 41510 are SY Mus |given. Radio source. TU Mus |Min II 8.65. P var. Min I = 2424260.396 + 1.38728d*E (JD2423900 - TU Mus |29300) [00039]; during JD2437380 - 41900 - see Table. The light TU Mus |curve shape var. TV Mus |Min II 11.3. TW Mus |Min II 12.4. TZ Mus |B - V: +1.22, +1.43. UW Mus |Min II 11.9. UY Mus |Min II 12.0. VW Mus |Min II 13.9. WY Mus |P var. Periodic term: +0.35d*sin(0.12{deg}*E). XZ Mus |Before JD2419200 Max = 2412590 + 113d*E. AB Mus |Min II 13.0. AS Mus |[A/H] = 0.5. AX Mus |P var. During JD2412550 - 19200 - see Table; during JD2423900 - AX Mus |26100 P = 97.3d. AY Mus |Min II 10.8. Min II - Min I = 0.481P. The elements are valid during AY Mus |1897 - 1943. In the time interval JD2441683 - 721 eclipses did not AY Mus |occur [08094]. BB Mus |P, possibly P should be doubled. BD Mus |Depth of Min II 0.05m. BE Mus |Min II 14.1. BF Mus |Min II 14.4. BK Mus |P very long P: 56d < d < 310d. BR Mus |Min II 11.25. B - V: +0.10m. BS Mus |Min II 11.5. BX Mus |Depth of Min II 0.04m. CD Mus |Min II 14.7. CS Mus |P > 120d. DW Mus |According to [08135], the spectral type is M5e, typical of Mira DW Mus |stars. Elements in [03934] were deduced from the observed DW Mus |brightness variations with P ~355d which was considered to be a DW Mus |spurious period; rapid variations were confirmed by 7h of DW Mus |photographic observations. DZ Mus |Possibly Pshould be doubled. EE Mus |In the coal sack. The flare was observed spectroscopically. EN Mus |d = 0.035P:. EP Mus |[A/H] = 0.2. According to [08136], EA, P = 4.15d, D = 0.05P, 11.63m EP Mus |- 12.60m V, Min II 11.7:. ET Mus |Alternatively possible type EW [08727,04001]. EV Mus |d = 0.09P:. EY Mus |In the Coal Sack region. EZ Mus |Alternative possible values of P 4.3032d, 4.3224d. FH Mus |Depth of Min II 0.03m. FO Mus |P var? GK Mus |Min II 15.0. GN Mus |Min II 14.2. GO Mus |Min II 15.2. GP Mus |B - V: +1.03, +1.61. KU Mus |Type RV: is also possible. MR Mus |MinII 8.53. NT Mus |VB A (B 12.8m, 14", 233{deg}, 2000). OT Mus |VB, several companions within 15". OW Mus |A twice longer period is not excluded. PX Mus |The mean brightness varies with a possible period about 750d. QR Mus |VB A (B 14.3mpg, 18", 228{deg}, 2000). QU Mus |VB A (B 14.7mpg, 13", 183{deg}, 2000). V0338 Mus |Min II = 10.1. VB AB (10.14m, 11.00m, 2.4", 129{deg}, 1985). V0340 Mus |Min II = 8.06. V0355 Mus |SB2. V0356 Mus |Double-mode pulsations. The Table gives the first-overtone light V0356 Mus |elements. For the second overtone, Max = 2453693.12 + 0.734376d x V0356 Mus |E. P2/P1 = 0.8043. V0360 Mus |Erroneously named in the finding chart legend in [g0143]; the V0360 Mus |correct chart is Fig. 2(c), upper right. The declination in the V0360 Mus |Table differs by 7" from that in [g0143]. V0364 Mus |Erroneously named in the finding chart legend in [g0143]; the V0364 Mus |correct chart is Fig. 2(c), upper middle. V0365 Mus |Cluster non-member? V0368 Mus |Cluster non-member? V0369 Mus |Type ELL (Ell) with a twice longer period is also possible. V0377 Mus |Cluster non-member? V0378 Mus |Erroneously named in the finding chart legend in [g0143]; the V0378 Mus |correct chart is Fig. 2(c), lower right. V0379 Mus |Erroneously named in the finding chart legent in [g0143]; the V0379 Mus |correct chart is Fig. 2(c), upper left. Cluster non-member? V0381 Mus |MinII - MinI = 0.58P. V0383 Mus |VB A (15.4mG; B 16.2mG, 3.5", 1{deg}, 2000). V0384 Mus |Period varies. V0385 Mus |Crowded. V0387 Mus |VB B (A 14.6mG, B 15.4mG; AB 2", 57{deg}, 2000). V0391 Mus |VB B (A 15.1mG, B 15.3mG; AB 4", 124{deg}, 2000). V0392 Mus |VB A (15.2mG; B 15.4mG, 4", 255{deg}, 2000). V0393 Mus |VB A (15.3mG; B 15.4mG, 5", 8{deg}, 2000). V0394 Mus |Crowded. V0395 Mus |Crowded. Strong Blazhko effect. V0396 Mus |Crowded. V0397 Mus |Several close companions. V0398 Mus |Crowded. V0399 Mus |Cluster non-member? V0400 Mus |VB A (15.3mG; B 16.1mG, 5", 142{deg}, 2000). V0402 Mus |Blazhko effect? V0403 Mus |Crowded. V0408 Mus |Crowded. The Gaia EDR3 identification is not absolutely certain. V0409 Mus |VB B (A 14.8mG, B 15.4mG; AB 5", 139{deg}, 2000). V0410 Mus |Cluster non-member? alf Mus |VB A (B 13.0m, 29.3", 316{deg}). eta Mus |VB A (B 7.30m, 60"). tet Mus |VB (A 5.64m, B 7.5m, 5.3", 187{deg}); SB (Porb = 18.341B). Variable tet Mus |intensity of emission lines with respect to the continuum (double tet Mus |wave; elements in the Table are for the epochs of Min I variability tet Mus |in the UV range ({lambda} lambda 1550 - 3300 A) with an amplitude tet Mus |about 2%, P = 1.5d and rapid changes (lamda lamda 1550 - 1800 A) tet Mus |with an amplitude about 3 - 5% on the time scale of 50s - 70s tet Mus |[08532]. Connected with a nebula, 80'*45'. R Nor |VB A (B 14.0m, 5.7", 268{deg}, 1929). P var. Max II = 2406371 + R Nor |486.94d*E (JD2406300 - 25000); Max II = 2426359 + 500.56d*E R Nor |(JD2426000 - 30500); Max II = 2431377 + 489.0d*E (JD2430500 - R Nor |34500); since JD2437600 - see Table. Like R Cen, has a doudle Max, R Nor |JD2437600 - see Table. Like R Cen, has a doudle Max, divided by a R Nor |comparatively shallow Min II. Max II is usually brighter than Max R Nor |I. Phase (Min I) = 0.43P, Phase (Max I) = 0.70P, Phase(Min II) = R Nor |0.85P. S Nor |In the centre of the open cluster NGC 6087, cluster member. [A/H] = S Nor |-0.1. T Nor |P var.Max = 2414783 + 241.87d*E (JD2414700 - 28000); Max = 2428084 T Nor |+ 244.93d*E (JD2428000 - 35000); since JD2437000 - see Table. U Nor |P var. Max = 2415028.94 + 12.64084d*E (JD2415000 - 26000) [00060]; U Nor |since JD2434000 - see Table, [A/H] = -0.6. W Nor |P2 ~1300d. Y Nor |VB A (B 12.2m vis, 4.0", 156{deg}, 1903). Z Nor |Min II 9.6. RR Nor |Min II 9.9. RS Nor |B - V: +1.13, +1.48. RT Nor |Quasiperiodic variations: P1 ~59d, P2 ~175d [08140]. RV Nor |[A/H] = 0.8. There are irregularities in the light curve. SV Nor |Min II 12.6. SW Nor |D = 0.013P, d = 0.003P. SX Nor |d = 0.1P. SY Nor |VB A (B 12.8m, 2.1", 315{deg}, 1934). B - V: +1.16, +1.49. [A/H] = SY Nor |0.5. SZ Nor |Min II 12.6. TT Nor |Twice longer P is possible. TU Nor |Min II 12.5. Associated with a small faint nebula. TV Nor |Min II 9.3. TW Nor |In the region of the poor open cluster Lynga 6. B - V: +1.79, TW Nor |+2.22. [A/H] = 0.2. TX Nor |Min II 12.5. TZ Nor |Min II 12.1. UV Nor |d ~0.07P. UX Nor |In Max light B - V = +0.30. UY Nor |d = 0.025P. UZ Nor |d = 0.02P. VV Nor |In the region of the cluster NGC 6152. VX Nor |Depth of Min II ~0.03m. VZ Nor |In the region of the cluster NGC 6152. Min II 14.3. WX Nor |The chart is erroneously labelled as that for WZ Nor. Min II 12.8. WZ Nor |The chart is erroneously labelled as that for WX Nor. Min II 13.4. XY Nor |Min II 13.2. AA Nor |[A/H] = -0.1. AF Nor |In the region of the open cluster NGC 5999. AQ Nor |The chart in [06286] is wrong. AR Nor |The chart in [06286] is wrong. AT Nor |d = 0.026P:. BE Nor |Min II 14.2. BF Nor |The chart in [06286] is wrong. BH Nor |Min II 13.2. BP Nor |Close companion. CE Nor |d = 0.05P. Min II 11.8? CG Nor |The chart in [06286] is wrong. CI Nor |The chart in [06286] is wrong. CT Nor |The chart in [06286] is wrong. CX Nor |Min II 15.0. DE Nor |The chart in [06286] is wrong. DF Nor |The chart in [06286] is wrong. DO Nor |Min II 14.2. In the region of the open cluster NGC 6087. DP Nor |The chart in [06286] is wrong. DR Nor |In the region of the open cluster NGC 6087. EE Nor |The chart in [06286] is wrong. EM Nor |Min II 13.8. ET Nor |d = 0.032P. FG Nor |The chart in [06286] is wrong. FI Nor |The chart in [06286] is wrong. FK Nor |Min II 15.0. FQ Nor |According to [00060], P = 1.994d? FW Nor |Min II 14.5. GM Nor |d = 0.02P; Min II 11.01; Min II - Min I = 0.499P (JD2441683 - 721), GM Nor |Min II - Min I = 0.531P (JD2425381 - 28402). B - V = 0.44m. GN Nor |Min II 13.3, DII = 0.16P, Min II - Min I = 0.405P (JD2425900). GN Nor |Apsidal motion: P = 500yr. GO Nor |Min II 13.7. GQ Nor |Min II 13.8. GR Nor |[A/H] = 0.9. GT Nor |d = 0.048P. GU Nor |In the region of the open cluster NGC 6067. B - V: +1.17, +1.40. GU Nor |[A/H] = 0.1. GV Nor |d = 0.03P:. GX Nor |Min II 15.0. HH Nor |VB B (A 9.9m vis, FO; B 12.6", 148{deg}). d = 0.05P. HI Nor |D is very small. HK Nor |Min II 12.9. HO Nor |Min II 13.2:. HW Nor |d = 0.024P. HZ Nor |P = 2.921584d is possible. IQ Nor |B - V: +1.55, +1.93. IS Nor |In the region of the open cluster NGC 6067. IT Nor |Min II 9.8. KL Nor |P >= 140d. KM Nor |P >= 170d. KQ Nor |Mira Ceti type is not excluded [04001]. KT Nor |P >= 180d. KX Nor |Min II 14.8. LO Nor |P >= 220d. LV Nor |Deep Min II. LX Nor |Possible P values: 0.60492d, 0.7851d, etc. NR Nor |Min II 15.9. NS Nor |Min II 10.50 V; Min II - Min I = 0.67P NW Nor |P > 140d. NX Nor |Min II 14.4. OS Nor |Epoch of Min is given. EW/KW type is possible. OT Nor |Min II 13.7. OU Nor |Min II 15.1. OV Nor |P >= 200d. OW Nor |P >= 120d. OX Nor |P >= 110d. PQ Nor |Possibly a cepheid which is a fainter component of an unresolved PQ Nor |binary. Epoch of Max is given. PT Nor |In the region of the open cluster NGC 6067. QT Nor |HV 5388 = HV 8903. The coordinates in [00424] are wrong. QV Nor |3U 1538 - 52. No.12 [04124]. Epoch of Min corresponding to the QV Nor |X-ray eclipse is given. Depth of Min I 0.05m V, that of Min II QV Nor |0.08m V. The period of X-ray pulses Px = 528.928s [04114]. A flare QV Nor |was observed with {Delta}(m) > 0.3m [09456]. QX Nor |4U 1608 - 52. QZ Nor |In the open cluster NGC 6067. V0367 Nor |May be not a supergiant. V0374 Nor |Type LBV: is also possible. V0384 Nor |MinII 10.30. V0389 Nor |Min II 15.7. V0392 Nor |VB (A 8.59m; B 9.29m, 13", 205{deg}, 2000). The combined brightness V0392 Nor |is tabulated. V0396 Nor |Cluster non-member. MinII - MinI = 0.44P. V0405 Nor |Min II = 9.08:. MinII - MinI = 0.56P. V0410 Nor |Min II = 16.60. V0412 Nor |Min II = 16.90:. O'Connell effect. V0413 Nor |Min II = 15.80. V0414 Nor |Min II = 14.95:. V0415 Nor |Min II = 17.90. V0417 Nor |Min II = 16.65. V0418 Nor |Min II = 16.45. V0419 Nor |Min II = 16.35. V0420 Nor |Min II = 17.95. V0422 Nor |Min II = 17.50. V0424 Nor |Min II = 14.73. V0426 Nor |Min II = 18.0. V0427 Nor |Min II = 16.78. V0428 Nor |Min II = 13.22. V0429 Nor |The coordinates in [80419] are wrong. V0430 Nor |Min II = 17.18. The coordinates in [80419] are wrong. V0432 Nor |Min II = 17.30. V0434 Nor |Min II = 16.45. V0436 Nor |Min II = 17.65. V0437 Nor |Min II = 14.10. V0438 Nor |Min II = 17.0. V0440 Nor |Min II = 16.13. V0441 Nor |Min II = 16.6. V0442 Nor |Min II = 14.95. V0443 Nor |Min II = 16.8. V0445 Nor |Min II = 17.2. V0447 Nor |Min II = 16.62. V0448 Nor |Min II = 16.50. V0449 Nor |Min II = 15.75. V0451 Nor |Min II = 9.58. V0479 Nor |Multiperiodic; P2 = 0.204945d. V0495 Nor |SB2. V0498 Nor |VB B (A 9.25mV; B 9.72mV, A6V, 7", 160{deg}, 1998). Combined V0498 Nor |magnitudes are presented in the Table. V0501 Nor |VB A (B 5", 99{deg}, 20000). Combined magnitudes are presented in V0501 Nor |the Table. V0558 Nor |VB A (B 11.4m, 3", 183{deg}, 1933; C 11.4m, 6", 159{deg}, 1972). mu. Nor |In the region of the open cluster NGC 6169. U Oct |P var. Max = 2420685 + 302.00d*E (JD2414900 - 20700); Max = 2424320 U Oct |+ 300.74d*E (JD2422800 - 29800); Max = 2431901 + 309.60d*E U Oct |(JD2429800 - 32250); Max = 2434018 + 300.70d*E (JD2432250 - 38800); U Oct |since JD2438800 - see Table. X Oct |P var.Max = 2415170 + 208.40d*E (JD2415100 - 17100); Max = 2417425 X Oct |+ 201.24d*E (JD2417100 - 20700); Max = 2423780 + 207.95d*E X Oct |(JD2422000 - 24000); Max = 2424370 + 200.18d*E (JD2424000 - 25600); X Oct |since JD2425600 - see Table. Depths of minima are stongly variable; X Oct |1.1m <= A <= 4.0m. RV Oct |{Delta}(S) = 10. TX Oct |Min II 12.7. UV Oct |{Delta}(S) = 9; (k - b)2 = 0.06. Blazhko effect: P = 80d; 0.14P <= UV Oct |M - m <= 0.24P, 0.4m <= A <= 1.3m. UZ Oct |Min II 9.48; dI = 0.00P, dII = 0.05P. P var. Min I = 2440223.1560 + UZ Oct |1.1493709d*E (JD2438300 - 42000); since JD2442000 - see Table. AM Oct |Min II 14.9. BC Oct |Min II 10.8:V. Also possible is P=26.45924 with MinII - MinI = BC Oct |0.338P. BE Oct |P < 20d:. BG Oct |P = 0.7490d? BK Oct |Min II 14.6. BP Oct |(k - b)2 = 0.25. CC Oct |Basic radial pulsation with P1 = 0.12490d (A1 = 0.042m) is CC Oct |superimposed by others with periods: P2 = 0.0795317d (A2 = 0.008m), CC Oct |P3 = 0.12336d (A3 = 0.014m); P4 = 0.11068d (A4 = 0.008m), P5 = CC Oct |0.12713d (A5 = 0.006m); P6 = 0.11815d (A6 = 0.006m). CD Oct |{mu} = 0.51", p = 279{deg}. One of the periods P = 686s (A = CD Oct |0.01m). CE Oct |Light oscillation with P2 = 0.054511d (A2 = 0.0056m) is CE Oct |superimposed by an oscillation with P1 = 0.2100d or 0.2660d (A1 = CE Oct |0.0052m), which is due to pulsation or ellipsoidal variability in a CE Oct |close binary system. CP Oct |Variability type and spectral type (F2/F3Ib/II) do not agree. DU Oct |MinII 9.34. DV Oct |In the constellation Octans. DZ Oct |Blazhko effect, P=36.8d. EV Oct |Min II = 14.5. EX Oct |Min II = 11.20. EZ Oct |Min II = 12.04. GH Oct |Blazhko effect, P = 222d. GM Oct |Blazhko effect, P = 70.8d:. alf Oct |SB, Porb = 9.073d. R Oph |P var. Max = 2399214 + 302.1d*E (JD2399200 - 2427900) [00458]; Max R Oph |= 2427915 + 304.0d*E (JD2427900 - 34900); Max = 2434906 + 301.5d*E R Oph |(JD2434900 - 40600) [00001]; since JD2440600 - see Table. U Oph |ADS 10428 A (B 12.26m, GOV, 20.4", 358{deg}). Min II 6.46. P var. U Oph |Periodic term: +0.0120d*sin(0.0483{deg}*E + 4.7833{deg}). V Oph |P var. Max = 2411155 + 296.73d*E (JD2411000 - 24000); Max = 2424198 V Oph |+ 302.46d*E (JD2424000 - 28000); since JD2428000 - see Table. W Oph |P var. Before JD2420500 Max = 2415186 + 335.07d*E; Max = 2420870 + W Oph |325.33d*E (JD2420500 - 24700); since JD2424700 - see Table. X Oph |VBA (A = 0.34", Porb = 485.3 yr; B - 9m, K1III, 0.4", 142{deg}, X Oph |1980). The range of the combined brightness is given. P var. Max = X Oph |2416416 + 336.61d*E (JD2416400 - 26000); Max = 2426161 + 331.28d*E X Oph |(JD2426000 - 32500); Max = 2432788 + 335.50d*E (JD2432500 - 38000); X Oph |since JD2438000 - see Table. Y Oph |SB1? Porb = 2612d? P var. Before JD2427000 Max = 2408694.77 + Y Oph |17.11884d*E; since JD2432000 - see Table. [A/H] = -0.2. Z Oph |P var. Max = 2411896 + 349.0d*E (JD2411800 - 21000) [00458]; Max = Z Oph |2420962 + 352.1d*E (JD2421000 - 25000); Max = 2425183 + 347.4d*E Z Oph |(JD2425000 - 31000); Mean elements after JD2431000 - see Table. RR Oph |P var. Nonlinear term: -0.009282d*E2. RS Oph |Previous outbursts: 1898, 1933, 1958. According to [07575], in 1972 RS Oph |- 1973 there were semiregular variations ({Delta}(m) ~0.5M, P = 50D RS Oph |- 70D). RT Oph |P var. Before JD2426500 Max = 2417452 + 429.00d*E; Max = 2426461 + RT Oph |422.67d*E (JD2426500 - 34000); since JD2434500 - see Table. OH, H2O RT Oph |maser. RU Oph |P var. Before JD2422000 Max = 2417388 + 200.95d*E; Max = 2422011 + RU Oph |203.62d*E (JD2422000 - 27300); Max = 2427298 + 200.5d*E (JD2427300 RU Oph |- 29000); Max = 2429305 + 203.88d*E (JD2429000 - 33000); during RU Oph |JD2433000 - 40500 - see Table. RV Oph |d = 0.015P; Min II 9.56, DII = 0.09P. The light curve share var. RW Oph |P var. Max = 242494 + 247.86d*E (JD2425000 - 34000). The Table RW Oph |gives mean elements. RX Oph |OH, H2O maser. RY Oph |P var. Max = 2415235 + 151.05d*E (JD2414700 - 24000); Max = 2424152 RY Oph |+ 149.69d*E (JD2424000 - 31000); Max = 2431339 + 150.94d*E RY Oph |(JD2431000 - 40000); since JD2440000 - see Table. RZ Oph |d = 0.030P. SS Oph |P var. Before JD2432500 Max = 2417330 + 179.88d*E. ST Oph |(k - b)2 = 0.03. SV Oph |The elements are valid since JD2422000. SW Oph |VB A (B 12.0m vis, 2.4", 91{deg}, 1943). d = 0.02P. P var. Min = SW Oph |2418880.528 + 2.445948d*E (JD2418880 - 26200) [00001]; Min = SW Oph |2431235.216 + 2.446086d*E (JD2427900 - 33500) [02389]; since SW Oph |JD2434000 - see Table. SX Oph |d = 0.03P. SZ Oph |P var. Before JD2428400 Min = 2421057.556 + 3.708454d*E; since SZ Oph |JD2442000 - see Table. TT Oph |[Fe/H] = -0.5. TW Oph |P2 = 2000d:. Associated with a nebula of variable brightness TW Oph |[03479]. UU Oph |d = 0.024P. P var? UX Oph |P var. Max = 2426041 + 117.34d (JD2406430 - 28040); since JD2433100 UX Oph |- see Table. VW Oph |P var. Mean elements are given. During JD2422500 - 30600 Max = VW Oph |2430554 + 282.69d*E. WW Oph |Epoch of Min is given. The chart in [06286] is wrong. WZ Oph |Min II 9.82. XX Oph |A symbiotic object featuring deep fadings of long duration [09489]. AH Oph |H2O maser. AQ Oph |The chart in [06286] is wrong. BE Oph |The data in [00278] refer to another star. BF Oph |SB? P var? since JD2430000 - see Table. BN Oph |80d <= P <= 250d. DM Oph |P var. P = 220d (1893 - 1910), P = 216d (1914 - 1928). DQ Oph |P = 35d is possible. FK Oph |V2 (NGC 6273). GM Oph |V12 (NGC 6284). GR Oph |P var. Max = 2415425 + 136d*E (1893 - 1908); during 1910 - 1928 - GR Oph |see Table. IL Oph |P2 = 140d:. IW Oph |In the field of the globular cluster NGC 6293, possible cluster IW Oph |member. KM Oph |In the field of the globular cluster NGC 6304, field star. KO Oph |In a dark nebula. KQ Oph |P2 = 1500d. KR Oph |P2 > 5000d. OU Oph |V70 (NGC 6266). PU Oph |VB (A = V29 (NGC 6266), the data are in the Table; B = V28 (NGC PU Oph |6266), 16.6m - 17m, 4B, 4.8", 7{deg}), B: RRAB, Max = 2433423.52 + PU Oph |0.49749d*E, M - m = 0.15P. V0378 Oph |Min II 14.2. In the region of the open cluster CR 359. Epoch of Max V0378 Oph |is given. V0380 Oph |Porb = 0.16d. Blue. V0391 Oph |In the region of the open cluster CR 359. P var? Before JD2427000 V0391 Oph |Min = 2425501.425 + 2.89558d*E [00432]; since JD2441500 - see V0391 Oph |Table. V0392 Oph |Red. V0402 Oph |P var. Max = 2425364 + 154d*E (JD2425350 - 670); since JD2425670 - V0402 Oph |see Table. V0413 Oph |{Delta}(S) = 3. Blazhko effect? V0414 Oph |B - V: +0.41, +0.77. V0423 Oph |In the region of the open cluster CR 359. V0426 Oph |Outbursts separated by 17d - 55d [08079]; in 1976 - 77 the cycle V0426 Oph |was 32.3d. Outside outbursts 12.7m - 13.3m, waves with a cycle of V0426 Oph |20 - 30 Min and slower variations. V0438 Oph |H20 Maser. V0439 Oph |B - V: +0.63, +0.97. V0442 Oph |Porb = 0.14056d. V0445 Oph |VB A (B 13.04m y, 21"nf). (k - b)2 = 0.35; {Delta}(S) = 2. V0445 Oph |According to [05692], Blazhko effect (Pi > 2000d). V0449 Oph |P var. Before JD243900 Min = 2428696.465 + 1.243078d*E; Min = V0449 Oph |2442959.607 + 1.243095d*E (JD2439000 - 43000); since JD2443000 - V0449 Oph |see Table. V0451 Oph |Min II 8.31; Min II - Min I = 0.494P; DII = 0.12P. V0452 Oph |{Delta}(S) = 5:. V0455 Oph |P var? The Table gives mean elements which need confirmation. V0456 Oph |Min II 10.5. P var. Before JD2436100 Min = 2428422.341 + V0456 Oph |1.015986d*E [00476]; since JD2441800 - see Table. V0465 Oph |B - V: +0.68, +1.10. P var? V0471 Oph |Very red. V0478 Oph |B - V: +0.86, +1.33. [A/H] = -0.7. The elements need confirmation. V0487 Oph |D <= 0.14P. In the region of the open cluster Cr 359. V0496 Oph |In the region of the open cluster Cr 359. V0501 Oph |Min II 11.1. V0502 Oph |Min II 8.81. P var. Since JD2434500 - see Table. V0506 Oph |Min II 12.0. In the region of the open cluster Cr 359. V0508 Oph |Min II 10.59. V0509 Oph |In the region of the open cluster Cr 359. V0511 Oph |Min II 13.7. In the region of the open cluster Cr 359. V0515 Oph |Max = 2425600 + 300d*E (JD2425600 - 26700); P = 140d (JD2426700 - V0515 Oph |27300); during JD2427300 - 30200 - see Table. V0516 Oph |In the region of the globular cluster NGC 6304. V0517 Oph |In the region of the globular cluster NGC 6304. V0521 Oph |P = 164d (JD2415000 - 24600); P2 - 4000d. V0526 Oph |Min II 13.6. V0527 Oph |Min II 14.8. V0532 Oph |P >= 6000d. V0533 Oph |P >= 80d. V0534 Oph |d = 0.03P. V0535 Oph |d = 0.025P. V0536 Oph |d = 0.04P:. V0537 Oph |Min II 12.8. V0540 Oph |d = 0.05P; Min II 13.4. V0541 Oph |[A/H] = -1.0. In the region of the globular cluster NGC 6401; V0541 Oph |cluster non-member? V0543 Oph |Min II 13.6. V0549 Oph |Min II 14.0. V0550 Oph |Min II 13.0. V0554 Oph |[A/H] = -1.1. V0555 Oph |Sharp and flat maxima. Blazhko effect? V0557 Oph |Min II 15.7. In the region of the open cluster Cr 359. V0558 Oph |B - V: +0.57, +0.68. [Fe/H] = -1.48. According to [09037], P = V0558 Oph |0.299d. V0564 Oph |[Fe/H] = -1.37. Epoch of Min is given. P var. Nonlinear term: V0564 Oph |+0.0073d*(E + 10)**2. V0565 Oph |P = 0.3957d is possible. Photoelectric observations of 1968 V0565 Oph |contradict the elements [05746]. V0566 Oph |dI = 0.048P; Min II 7.89, dII = 0.06P. P var. Before JD2440500 Min V0566 Oph |= 2436744.4200 + 0.40964091d*E [08287]; since JD2440500 - see V0566 Oph |Table. V0567 Oph |(k - b)2 = 0.22; {Delta}(S) = 0. According to [07984], Max = V0567 Oph |2441134.467 + 0.1300729d*E. V0568 Oph |Red. V0570 Oph |VB A (B 16.3m, 5", 90{deg}). V0572 Oph |In the region of the open cluster Cr 359. V0573 Oph |d = 0.034P. In the region of the open cluster Cr 359. V0574 Oph |P2 ~500d. V0577 Oph |Min II 11.9. Min II - Min I = 0.583P. DII = 0.050P. e = 0.22. V0580 Oph |VB A (B 15.5m, 0.2'). V0585 Oph |A long-period variation is superimposed? V0586 Oph |In the region of the open cluster Cr 359. V0590 Oph |Min II 13.6. V0592 Oph |Max = 2427227 + 78d*E (JD2426100 - 29400); during JD2429400 - 30150 V0592 Oph |- see Table. After intervals of irregular variability the V0592 Oph |periodicity resumes without phase shift. V0605 Oph |Epoch of Min is given. V0618 Oph |Min II 14.7:. V0636 Oph |d = 0.030P. V0683 Oph |P var. The light curve shape varies. V0687 Oph |P may be twice longer. V0693 Oph |Blazhko effect? [05692]. V0695 Oph |P var? The light curve shape varies. V0698 Oph |P var? since JD2442950 - see Table. V0700 Oph |B - V: +0.49, +0.50. [Fe/H] = -2.10. V0716 Oph |{Delta}(S) = 7. V0720 Oph |VI (NGC 6171). Cluster non-member. V0722 Oph |P var. Max = 2437089.456 + 0.6190385d (JD2419900 - 37100) [07806]; V0722 Oph |since JD2436700 - see Table. V0729 Oph |P var. Max = 2437492.766 + 0.4685794d*E (JD2423500 - 37800) V0729 Oph |[03560]; since JD2437400 - see Table. V0732 Oph |Unusual light curve (sharp Max; primary Min; broad Max; secondary V0732 Oph |Min 15.2). V0734 Oph |P var. Max = 2420636.497 + 0.562489d*E (JD2420600 - 29100); during V0734 Oph |JD2429100 - 37150 - see Table. V0735 Oph |Min II 10.6. V0737 Oph |P = 374d is possible. V0767 Oph |According to [00104], waves with {Delta}(m) = 0.3m - 1.4m vis of V0767 Oph |50d - 110d duration; mean brightness var, {Delta}(m) ~0.4m in 800d V0767 Oph |- 1000d. V0782 Oph |Very red. V0784 Oph |B - V: +0.26, +0.56. The period should be checked. V0786 Oph |Red. V0788 Oph |Blazhko effect? Pi = 115d. V0799 Oph |P = 215d is possible. V0802 Oph |Red. V0816 Oph |B - V: +0.25, +0.63. V0822 Oph |Blazhko effect? V0823 Oph |In the region of the open cluster IC 4665. V0825 Oph |In the region of the open cluster IC 4665. V0829 Oph |Blazhko effect? Pi = 165d. V0832 Oph |Red. V0838 Oph |P2 ~500d is possible. V0839 Oph |{mu} = 0.041", ro = 292{deg}. Min II 9.38. V0840 Oph |VB A (B 12m, 16", 116{deg}). V0841 Oph |Max = 2396146. V0843 Oph |SN Kepler. Max 2307193. Gaseous remnant. V0844 Oph |Min II 14.9. V0845 Oph |VB A (B 15.7m). V0847 Oph |Min II 13.1. V0848 Oph |Min II 13.4. V0851 Oph |Max = 2425828 + 95d*E (JD2425600 - 29700); during JD2429700 - 34250 V0851 Oph |- see Table. V0854 Oph |According to [08116], the spectrum resembles that of a T Tau - type V0854 Oph |star. V0868 Oph |Min II 13.6. In the region of the open cluster Cr 359. V0870 Oph |In the region of the open cluster Cr 359. V0872 Oph |P = 0.825d is possible. V0878 Oph |Min II 16.5. In the region of the open cluster Cr 359. V0911 Oph |P2 = 81d, P3 = 114d. P4 > P3? Standstills up to 100d. V0919 Oph |VB A (B sp). V0920 Oph |Min II 15.9. V0924 Oph |Min II 16.4. V0929 Oph |d = 0.050P. V0934 Oph |E type is possible. V0936 Oph |In the region of the open cluster Cr 359. V0938 Oph |Min II 15.3. In the region of the open cluster Cr 359. V0940 Oph |Min II 15.6. V0941 Oph |Min II 16.5. V0943 Oph |Min II 16.4. In the region of the open cluster Cr 359. V0945 Oph |Min II 15.1. In the region of the open cluster Cr 359. V0947 Oph |Min II 14.5. In the region of the open cluster Cr 359. V0952 Oph |P = 0.954d is possible. V0954 Oph |In the region of the open cluster Cr 359. Min II 14.9. According to V0954 Oph |[03500], const, V = 12.86m, B - V = +1.36m, V0959 Oph |P var? Max = 2429785.419 + 0.084857d*E (JD2429785 - 845) [02757]; V0959 Oph |during JD2443719 - 732 - see Table; other possible elemente: Max = V0959 Oph |2443726.469 + 0.07786d*E. V0960 Oph |In the region of the open cluster Cr 359. V0963 Oph |Min II 15.1. In the region of the open cluster Cr 359. V0968 Oph |[Fe/H] = -1.48. In the region of the open cluster Cr 359. V0969 Oph |Min II 13.8:. In the region of the open cluster Cr 359. V0977 Oph |In the region of the globular cluster NGC 6426. V0978 Oph |In the region of the globular cluster NGC 6426. V0979 Oph |V11 (NGC 6426). Cluster non-member. V0980 Oph |In the the region of globular cluster NGC 6426. P = 0.25740d is V0980 Oph |possible. V0983 Oph |In the region of the open cluster Cr 359. V0986 Oph |In July 1980 Vr varied with P = 0.179d, 0.147d, 0.225d, and V0986 Oph |possibly 0.097d, but there were no spectrum variations, and the V0986 Oph |photometric P = 0.323d was not noticeable in Vr. SB? Porb = 15d - V0986 Oph |20d; there is also excess power at low frequences in the V0986 Oph |photometric data. Earlier studies revealed photometric periods V0986 Oph |0.284d - 0.4d and violation of periodicity. V0987 Oph |d = 0.02P. Min II 14.6. In the region of the open cluster Cr 359. V0998 Oph |In the region of the globular cluster NGC 6171. V0999 Oph |In the region of the globular cluster NGC 6171. V1000 Oph |Blazhko effect? V1002 Oph |Min II 15.2. RRC type with twice shorter P is possible. V1004 Oph |Blazhko effect? V1010 Oph |Min II 6.46. P var. P = 0.661464d (JD2415000 - 25000) [05738]; V1010 Oph |since JD2425000 - see Table, nonlinear term: -3.87d*10**(-10)*E**2. V1010 Oph |Min I var.The light curve shape and the depth of Min I var. V1011 Oph |Blazhko effect? V1015 Oph |D <= 0.23P, d < 0.02P; Min II 14.5. V1017 Oph |[Fe/H] = -1.25. P var? Max = 2437433.935 + 0.2343d*E (JD2437433 - V1017 Oph |514) [03625]. During JD2442954 - 45140 - see Table. According to V1017 Oph |[09037], P = 0.361d. V1018 Oph |Possibly eclipsing. V1021 Oph |{Delta}(m) var. B - V: +0.42, +0.62. V1022 Oph |d = 0.06P:; Min II 15.95. V1024 Oph |Max = 2437433.559 + 0.5914d*E (JD2437433 - 514) [03625]. During V1024 Oph |JD2442954 - 45140 - see Table. RR(B) type is possible; P = 0.371d V1024 Oph |satisfies the observations during JD2442954 - 44407. V1026 Oph |Max = 2437433.562 + 0.6563d*E (JD2437433 - 514) [03625]. During V1026 Oph |JD2442954 - 45140 - see Table. V1028 Oph |Blazhko effect? V1032 Oph |P > 1.0d is not excluded. V1033 Oph |Max = 2437433.714 + 0.4845d*E (JD2437433 - 514) [03625]. During V1033 Oph |JD2442954 - 45140 - see Table. V1035 Oph |Max = 2437433.388 + 0.6100d*E (JD2437433 - 514) [03625]; during V1035 Oph |JD2442954 - 45140 - see Table. V1039 Oph |P = 0.3166d is possible. V1040 Oph |The light curve shape var. V1041 Oph |[Fe/H] = -1.06. V1042 Oph |The light curve shape var. Max = 2437433.633 + 0.5528d (JD2437433 - V1042 Oph |514) [03625]. During JD2442954 - 45140 - see Table. V1052 Oph |Max = 2437433.537 + 0.7546d*E (JD2437433 - 514) [03625]; during V1052 Oph |JD2442954 - 45140 - see Table. V1054 Oph |VB Wolf 630AB (A 9.76m V, 12.47{mu}; B 9.78m V; A = 0.22", Porb = V1054 Oph |1.71665 yr; C = Wolf 629, 11.70m V,14.75{mu}, dM4, 72", D = vB8, V1054 Oph |16.7m V, 221", common {mu}). {mu} = 1.19", ro = 222{deg}. V1054 Oph |Lx/Lopt(V) = 0.05. V1072 Oph |P var. Max = 2439025.31 + 0.444715d*E (JD2438500 - 39025); since V1072 Oph |JD2442800 - see Table. V1075 Oph |Red. V1077 Oph |P var. Max = 2438614.40 + 0.373926d*E (JD2438200 - 700); Max = V1077 Oph |2442871.516 + 0.37384d*E (JD2442810 - 910): Max = 2442983.345 + V1077 Oph |0.373911d*E (JD2442920 - 3330); since JD2443330 - see Table. V1089 Oph |VB AB (B 16.4m, 2", 45{deg}). V1099 Oph |Red. V1100 Oph |Red. V1111 Oph |OH, H2O, SiO maser. V1120 Oph |Min II 14.3. V1121 Oph |Soft X-ray source. V1135 Oph |[Ca/H] = -0.74. V1141 Oph |P var? The light curve shape var? V1142 Oph |P var? The light curve shape var? V1146 Oph |P = 185.2d is possible. V1153 Oph |P = 153.0d is possible. V1157 Oph |B - V: +0.42, +0.66. V1161 Oph |P = 0.49d is possible [06438]. V1168 Oph |P var? The light curve shape var? V1170 Oph |P = 360d: is possible [06438]. V1174 Oph |P var? The light curve shape var? V1176 Oph |P = 269.0d is possible. V1179 Oph |P var? The light curve shape var? V1185 Oph |Other possible elements: Max = 2435630 + 177d*E [00001]. V1195 Oph |One more Max 2435637 (1956). Type M is possible. V1203 Oph |P = 315d is possible [06438]. V1204 Oph |P = 144d: or P = 191d: are possible. V1235 Oph |UV type is possible. V1240 Oph |P = 0.42136d is possible. V1244 Oph |The light curve shape var? V1258 Oph |P var? V1261 Oph |The light curve is not typical for the P in the Table [06438]. V1262 Oph |The light curve is not typical for the P in the Table [06438]. V1276 Oph |[Ca/H] = -0.1. V1296 Oph |[Ca/H] = -0.9. V1299 Oph |The light curve shape var? V1300 Oph |P = 235d: is possible. V1305 Oph |Min II 17.9:. V1307 Oph |The light curve shape var? Spurious period? [06438]. V1323 Oph |P var? V1332 Oph |[Ca/H] = -0.64. V1348 Oph |The light curve shape var? V1355 Oph |The light curve shape var? V1403 Oph |P = 215d? V1423 Oph |The light curve shape var? V1426 Oph |P var? V1451 Oph |P = 179.4d? V1474 Oph |P = 127d:? V1491 Oph |P = 328.0d? V1492 Oph |The light curve shape var? V1505 Oph |P = 86d:? V1512 Oph |The light curve shape var? V1526 Oph |P = 0.29745d? V1532 Oph |P = 144.4d? V1534 Oph |P = 198.8d? V1548 Oph |The minor planet (336) Lacadiera. V1554 Oph |P = 136.0d? V1568 Oph |P = 275.5d? V1571 Oph |P var? V1573 Oph |Type E? V1583 Oph |P - spurious? V1616 Oph |Type E? V1628 Oph |The light curve shape var? V1637 Oph |[Ca/H] = -0.44. V1661 Oph |The light curve shape var? V1666 Oph |P = 154.2d? V1676 Oph |Close optical companion? V1682 Oph |P = 118.0d? V1687 Oph |Type CW? V1702 Oph |P = 121d? V1705 Oph |P var? V1710 Oph |P = 0.37422d? V1731 Oph |The light curve shape var? V1736 Oph |P = 143.8d?, P = 244.5d? V1744 Oph |P = 191.6d? V1748 Oph |A var. Type CW? V1754 Oph |P = 128.4d? V1768 Oph |The light curve shape var? V1775 Oph |Type EW? V1793 Oph |P = 170d:? V1803 Oph |The star is not SVS 438. V1805 Oph |The light curve shape var? V1811 Oph |Min II 17.9:. V1814 Oph |P = 160.4d? V1822 Oph |P var? V1829 Oph |P = 143.2d? V1840 Oph |V 12 (NGC 6333 = M9). Cluster member. V1841 Oph |The light curve shape var? V1845 Oph |V7 (NGC 6333 = M9). Cluster member. V1853 Oph |The light curve shape var? V1860 Oph |[Ca/H] = -0.49. V1861 Oph |P = 142.0d? V1864 Oph |V3 (NGC 6333 = M9). Cluster member. V1886 Oph |The light curve shape var? V1889 Oph |P = 316.0d? V1895 Oph |The light curve shape var? V1905 Oph |P = 149.0d? V1919 Oph |P = 102.8d?, P = 227.0d? V1939 Oph |P = 330.0d? V1946 Oph |The light curve shape var? V1952 Oph |P = 248.0d? V1953 Oph |P = 199d:?, P = 235d:? V1954 Oph |P = 159.6d? V1973 Oph |P = 0.24154d? V1989 Oph |A var? V1990 Oph |P = 121d:? V1991 Oph |The light curve shape var? V1994 Oph |P = 170.0d? V1998 Oph |P = 270.5d? V2002 Oph |The light curve shape var? V2003 Oph |[Ca/H] = -0.96. V2009 Oph |V5 (NGC 6356). Cluster member. V2010 Oph |[CA/H] = -0.79. V2016 Oph |[CA/H] = -0.96. V2042 Oph |P var. Max = 2430146.478 + 0.5385d*E (JD2429100 - 30202); since V2042 Oph |JD2436700 - see Table. V2045 Oph |The chart in [05159] is wrong. V2048 Oph |SB2 [06598]. In the region of the open cluster Cr 359. Along with V2048 Oph |irregular light variations typical for be stars there are rapid V2048 Oph |flares with the amplitudes up to 1.8m ({lambda} eff = 5800 A) V2048 Oph |[06150]. It is not excluded that the flares occur on a fainter V2048 Oph |companion of the system. V2051 Oph |Usually - 15.0m with strong flickering of brightness (up to 0.4m is V2051 Oph |5 minutes) and rare flares. At the same time the eclipses are V2051 Oph |observed with depth to 2.5m with the elements: Min = 2444787.32124 V2051 Oph |+ 0.062427865d*E [09550]; D = 0.0088P:, d = 0.0065P. V2058 Oph |In the dark nebula in the {rho} Oph region. V2059 Oph |In the dark nebula in the {rho} Oph region. V2061 Oph |In the region of the globular cluster NGC 6171 (M 107). V2062 Oph |In the dark nebula in the {rho} Oph region. V2063 Oph |The minor planet (64) Angelina. V2064 Oph |In the dark nebula in the {rho} Oph region. V2101 Oph |In a dark nebula. V2102 Oph |In the region of the globular cluster NGC 6293. V2105 Oph |Vr = 100 km/s. V2106 Oph |Vr = -102 km/s. V2108 Oph |H2O, SiO maser. V2112 Oph |The primary oscillation with A1 = 0.0172m (see Table) is V2112 Oph |superimposed by the secondary one (A2 = 0.0061m) with the elements: V2112 Oph |Max = 2444114.531: + 0.1449461d*E. V2116 Oph |X-ray pulsar. The pulse period is decreasing: 135s (1971), 112.076s V2116 Oph |(1979), 109.668s (1980) [09553]. The spin-period may be twice V2116 Oph |longer. V2118 Oph |Probably rapidly rotating single spotted F type star. Max V2118 Oph |brightness epoch is given. V2119 Oph |In the region of the globular cluster NGC 6284. Not a member of the V2119 Oph |cluster. V2120 Oph |V6 (NGC 6284). In the region of the globular cluster NGC 6284. Not V2120 Oph |a member of the cluster. V2121 Oph |V10 (NGC 6284). In the region of the globular cluster NGC 6284. Not V2121 Oph |a member of the cluster. V2122 Oph |In the region of the globular cluster NGC 6284. Not a member of the V2122 Oph |cluster. V2123 Oph |V11 (NGC 6284). In the region of the globular cluster NGC 6284. Not V2123 Oph |a member of the cluster. V2124 Oph |In the region of the globular cluster NGC 6284. Not a member of the V2124 Oph |cluster. V2137 Oph |VB B (AB 3", 295{deg}). V2391 Oph |Porb = 88.13yr. Component B is a suspected variable star (NSV V2391 Oph |24260) and may be the cause of variations. V2561 Oph |Not a supernova. V2577 Oph |The results in [78246] do not refer to BE Oph [78236]. V2597 Oph |P var. V2600 Oph |MinII 12.6. Type EB according to [78011]. V2604 Oph |MinII 14.0:. V2609 Oph |P var. V2612 Oph |MinII 9.70. V2617 Oph |VB A (B 14.7mpg, 23", 166{deg}, 1999). The tabulated amplitude can V2617 Oph |be influenced by the companion. V2626 Oph |MinII - MinI = 0.44P. VB (8.6mHp, 10.1mHp, 1.4", 306{deg}, 1991). V2628 Oph |Period varies, the tabulated elements are valid for JD 2453000 - V2628 Oph |2454600. V2629 Oph |VB A (B 17.0mV, 13", 95{deg}, 2000). V2636 Oph |A twice shorter period is not excluded. V2638 Oph |A twice shorter period is not excluded. V2640 Oph |VB A (B 13.8m, 25", 168{deg}, 2000). V2642 Oph |A twice longer period is not excluded. V2664 Oph |Period varies, current elements are tabulated. V2666 Oph |VB AB (6.1mV, 7.0mV, 0.44", 308{deg}, 1992; a=1.19", Porb=294 V2666 Oph |years). V2683 Oph |Blazhko effect, P = 26.28d [80377]. V2690 Oph |Porb = 0.063791d. V2703 Oph |VB A (B 14.3m, 19", 27{deg}, 1997). V2707 Oph |VB B (A 4"n). The range in the table is for combined brightness. V2709 Oph |Blazhko effect, P = 22.18d. V2711 Oph |Multiperiodic. V2715 Oph |VB, a close companion to the north-west. V2718 Oph |Cluster non-member. V2719 Oph |Cluster non-member. Type RRC a twice shorter period is not V2719 Oph |excluded. V2720 Oph |Cluster non-member. Type EW with P=0.4225d is also possible. V2721 Oph |Cluster non-member. V2724 Oph |O'Connell effect. V2731 Oph |Intermediate polar. Variations with Porb (see Table) and Pspin = V2731 Oph |0.0014815d. V2742 Oph |Biperiodic, P2 = 0.84443d. V2744 Oph |The identification with NSV 09496 suggested in [80002] is wrong. V2770 Oph |A one-day alias, P = 0.10096d, is also possible. V2775 Oph |O'Connell effect. V2780 Oph |The light curve shape varies. V2787 Oph |O'Connell effect. V2817 Oph |VB B (A 12.4m; AB 10", 34{deg}, 2000). V2837 Oph |The period in the Table is that of spot variability. SB2, Porb = V2837 Oph |591d. VB A (B = V2252 Oph, 13", 123{deg}, 1998). V2857 Oph |O'Connell effect. V2862 Oph |VB A (B 19.7m, 2.5", 289{deg}). V2897 Oph |P = 129d is superposed. V2918 Oph |A twice shorter period is not excluded. V2925 Oph |P varies [81101]. V2930 Oph |Blazhko effect. V2947 Oph |VB A (B 14.0m, 12", 93{deg}, 1998). The magnitude at minimum in the V2947 Oph |Table can be influenced by the companion. V2970 Oph |Type EB with P = 0.749593d is not excluded. V2975 Oph |VB (about 3"). Probably the eastern component is the variable. V2976 Oph |Blazhko effect, P = 36d. V2980 Oph |VB A (B 5", 120{deg}, 1998). V2981 Oph |VB A (B 6", 23{deg}, 1998). V3002 Oph |Blazhko effect, P = 28.58d. V3003 Oph |Type EB with P = 0.713648d is not excluded. V3014 Oph |Several close companions. V3017 Oph |Several close companions. V3068 Oph |RRC type with a twice shorter period is also possible. V3072 Oph |RRC type with a twice shorter period is also possible. V3079 Oph |VB B (AB 4", 206{deg}, 2000). The magnitudes in the Table were V3079 Oph |influenced by the companion. V3095 Oph |A twice longer period is also possible. V3099 Oph |VB A (B 3.5", 256 {deg}, 1999). The magnitudes in the Table were V3099 Oph |influenced by the companion. V3128 Oph |VB A (B 7", 326{deg}, 2000). V3138 Oph |A twice longer period is also possible. V3141 Oph |Not red. V3149 Oph |VB A (B 14.1m, 11", 338{deg}, 1991). V3157 Oph |RRC type with a twice shorter period is also possible. V3158 Oph |VB A (B 14.4mV, 6.5", 86{deg}, 2000). V3169 Oph |RRC type with a twice shorter period is also possible. V3181 Oph |DSCT type with a twice shorter period is also possible. V3189 Oph |VB A (B 4", 188{deg}, 2000). The magnitudes in the Table were V3189 Oph |influenced by the companion. V3201 Oph |RRC type with a twice shorter period is also possible. V3203 Oph |A twice shorter period is also possible. V3232 Oph |Type RRC and P = 0.219324d are also possible. V3233 Oph |P = 0.357913d is also possible. V3273 Oph |P = 0.330540d is also possible. V3280 Oph |EW type with P = 0.842916d is also possible. V3290 Oph |Other possible periods: 0.399278d and 0.285235d. V3294 Oph |VB (3"). The south-eastern component varies. The magnitudes in the V3294 Oph |Table were influenced by the companion. V3301 Oph |EW type with P = 0.578142d is also possible. V3303 Oph |Type EA or EB with P = 1.10753d is also possible. V3312 Oph |P = 0.2948d is also possible. V3331 Oph |O'Connell effect. V3339 Oph |EW type with P = 0.32572d is also possible. V3368 Oph |The one-day alias, P = 0.052743d, is also possible. V3380 Oph |The one-day alias, P = 0.49813d, is also possible. V3409 Oph |A twice longer period is also possible. V3410 Oph |P = 0.285971 is also possible. V3415 Oph |Other possible periods: P = 0.309472d (RRC type) or P = 0.618943 V3415 Oph |(EW type). V3416 Oph |Other possible periods: 0.285741d (RRC type), 0.400063d (RRC type), V3416 Oph |0.444211d (EW type), 0.571481d (EW type). V3424 Oph |EW type with P = 0.200466d is also possible. V3430 Oph |RRC type with P = 0.301831d is also possible. V3470 Oph |RRC type with a twice shorter period is also possible. V3489 Oph |P = 0.323339d is also possible. V3502 Oph |VB A (B 4", 143{deg}, 2000). V3504 Oph |DSCT type with a twice shorter period is also possible. V3532 Oph |A twice longer period is also possible. V3533 Oph |A one-day alias, P = 0.397451d, is also possible. V3534 Oph |RRAB type with a twice shorter period is also possible. V3541 Oph |VB A (B 4", 268{deg}, 1999). The magnitudes in the Table were V3541 Oph |influenced with the companion. V3569 Oph |VB A (B 3", 329{deg}, 1999). V3577 Oph |A one-day alias, P = 0.378940d, is also possible. V3579 Oph |RRC type with a twice shorter period is also possible. V3583 Oph |A one-day alias, P = 0.081429d, is also possible. V3609 Oph |Blazhko effect, P = 53.4d. V3616 Oph |VB (companion 4", 293{deg}, 1999). V3617 Oph |VB A (B 15.4m, 5.5", 20{deg}, 1999). RRC type with P = 0.21753d is V3617 Oph |also possible. V3618 Oph |VB (companion 5", 139{deg}, 1999). V3627 Oph |Close companions. The light curve shape varies. RRC type with P = V3627 Oph |0.2746d is also possible. V3632 Oph |Close VB. V3637 Oph |VB A (B 5", 118{deg}, 1999). V3638 Oph |O'Connell effect. V3640 Oph |Close companions. V3642 Oph |O'Connell effect. V3650 Oph |Close VB. V3652 Oph |VB A (B 5", 337{deg}, 2000; other companions). V3653 Oph |Crowded. V3655 Oph |O'Connell effect. V3656 Oph |O'Connell effect. V3657 Oph |VB B (AB 6", 352{deg}, 1999). V3673 Oph |Cluster non-member. V3677 Oph |P = 72d is also possible. V3694 Oph |Possible additional pulsation with P = 0.294286d. V3716 Oph |P = 56.3d is superposed. V3722 Oph |P = 48d is superposed. V3723 Oph |P = 47.3d is superposed. V3726 Oph |MinII - MinI = 0.42P. Apsidal motion. V3732 Oph |Porb = 0.9400430d [840005]. V3737 Oph |Blazhko effect? V3740 Oph |Crowded. V3741 Oph |VB B (A 15.1mG, B 15.4mG; AB 4", 145{deg}, 2000). V3742 Oph |Crowded. V3743 Oph |Strongly crowded. P varies, dP/dt = 0.293 x 10^(-6) d per year. V3744 Oph |Crowded. V3745 Oph |VB A (15.3mG; B 15.4mG, 5", 98{deg}, 2000). V3746 Oph |VB A (15.5mG; B 15.5mG, 5", 74{deg}, 2000). V3748 Oph |VB B (A 15.3mG, B 15.4mG; AB 2.4", 17{deg}, 2000). V3749 Oph |VB B (A 15.5mG, B 14.6mG; AB 5", 144{deg}, 2000; other companions). V3752 Oph |Cluster non-member. V3756 Oph |P varies [g0155]. V3758 Oph |Cluster non-member. V3771 Oph |Cluster non-member? V3781 Oph |VB A (15.9mG; B = NGC 6266 V123, 16.0mG, 3.2", 8{deg}, 2000). V3782 Oph |VB B (A = NGC 6266 V122, 15.9mG; B 16.0mG; AB 3.2", 8{deg}, 2000). V3786 Oph |VB A (16.2mG; B 16.3mG, 4.5", 151{deg}, 2000). V3787 Oph |VB A (15.8mG, VB?; B 16.8mG, 4.7", 77{deg}, 2000). V3789 Oph |VB B (A 14.9mG, B 15.8mG; AB 4.2", 87{deg}, 2000; other V3789 Oph |components). V3790 Oph |Several close companions. V3792 Oph |VB A (15.8mG; B 16.5mG, 2.4", 76{deg}, 2000). V3793 Oph |Several close companions. V3794 Oph |VB B (A 15.7mG, B 15.8mG; AB 4.5", 95{deg}, 2000; other V3794 Oph |components). V3798 Oph |Blazhko effect? [g0001]. V3799 Oph |VB B (A 15.4mG, B 15.7mG; AB 3.5", 44{deg}, 2000). V3800 Oph |VB B (A 15.3mG, B 15.8mG; AB 4", 291{deg}, 2000). V3805 Oph |Cluster non-member? V3806 Oph |Photometry in [g0146], [g0147] is uncalibrated but shows reasonably V3806 Oph |good light curves. V3807 Oph |VB B (A 15.6mG, B 15.8mG; AB 3.9", 42{deg}, 2000). V3809 Oph |VB A (16.0mG; B 16.1mG, 2.8", 62{deg}, 2000; other companions). V3811 Oph |Several close companions. V3812 Oph |Red. Photometry in [g0146] is uncalibrated but shows a reasonably V3812 Oph |good light curve. V3815 Oph |Several close companions. V3817 Oph |Crowded. Brighter than other cluster RR Lyrae stars, cluster V3817 Oph |non-member? Possible proper-motion member. V3820 Oph |VB B (A 13.6mG, B 15.8mG; AB 1.8", 99{deg}, 2000). Photometry in V3820 Oph |[g0146] is uncalibrated but shows a reasonably good light curve. V3821 Oph |Crowded. V3823 Oph |VB B (A 14.8mG, B 16.0mG; AB 3.4", 359{deg}, 2000; other V3823 Oph |components). V3825 Oph |VB B (A 12.8mG, B 15.7mG, C 17.0mG; AB 4.7", 165{deg}, 2000; BC V3825 Oph |4.4", 197{deg}, 2000). V3826 Oph |VB A (15.6mG; B 16.1mG, 3.2", 298{deg}, 2000; other components). V3827 Oph |VB A (15.8mG; B 15.8mG, 5.0", 303{deg}, 2000; other companions). V3828 Oph |Cluster non-member? V3829 Oph |Several close companions. V3830 Oph |Photometry in [g0146] is uncalibrated but shows a reasonably good V3830 Oph |light curve. VB B (A 15.8mG, B 15.9mG; AB 2.3", 241{deg}, 2000). V3831 Oph |Crowded, Gaia EDR3 identification is uncertain. Photometry in V3831 Oph |[g0146] is uncalibrated but shows a reasonably good light curve. V3832 Oph |Several close companions. V3833 Oph |VB A (16.3mG; B 17.0mG, 3.3", 263{deg}, 2000). V3834 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3834 Oph |reasonably good light curve. V3836 Oph |VB B (A 13.3mG, B 15.8mG; AB 2.5", 342{deg}, 2000; other V3836 Oph |components). V3837 Oph |Crowded. V3838 Oph |Crowded. V3840 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3840 Oph |reasonably good light curve. V3841 Oph |VB A (16.2mG; B 16.6mG, 3.3", 115{deg}, 2000). V3843 Oph |VB A (16.1mG; B 17.2mG, 4.3", 69{deg}, 2000; other companions). V3844 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3844 Oph |reasonably good light curve. V3845 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3845 Oph |reasonably good light curve. V3846 Oph |Red. Photometry in [g0146] is uncalibrated but shows a reasonably V3846 Oph |good light curve. V3847 Oph |Several close companions. Photometry in [g0146] is uncalibrated but V3847 Oph |shows a reasonably good light curve. V3848 Oph |Crowded. V3849 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3849 Oph |reasonably good light curve. V3853 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3853 Oph |reasonably good light curve. V3854 Oph |Several close companions. Photometry in [g0146] is uncalibrated but V3854 Oph |shows a reasonably good light curve. V3855 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3855 Oph |reasonably good light curve. V3856 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3856 Oph |reasonably good light curve. V3857 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3857 Oph |reasonably good light curve. V3858 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3858 Oph |reasonably good light curve. V3861 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3861 Oph |reasonably good light curve. V3863 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3863 Oph |reasonably good light curve. V3864 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3864 Oph |reasonably good light curve. V3868 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3868 Oph |reasonably good light curve. V3869 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3869 Oph |reasonably good light curve. V3870 Oph |Red. Several close companions. Photometry in [g0146] is V3870 Oph |uncalibrated but shows a reasonably good light curve with slow V3870 Oph |variations. V3871 Oph |Crowded, Gaia EDR3 identification is uncertain. Photometry in V3871 Oph |[g0146] is uncalibrated but shows a reasonably good light curve. V3872 Oph |Several close companions, including V019 (NGC 6266). V3873 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3873 Oph |reasonably good light curve. V3874 Oph |Cluster non-member? V3875 Oph |Several close companions, including V093 (NGC 6266). Photometry in V3875 Oph |[g0146], [g0147] is uncalibrated but shows reasonably good light V3875 Oph |curves. V3876 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3876 Oph |reasonably good light curve. V3877 Oph |Several close companions. Photometry in [g0146] is uncalibrated but V3877 Oph |shows a reasonably good light curve. V3878 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3878 Oph |reasonably good light curve. V3879 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3879 Oph |reasonably good light curve. V3881 Oph |Several close companions. V3882 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3882 Oph |reasonably good light curve. V3883 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3883 Oph |reasonably good light curve. V3884 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3884 Oph |reasonably good light curve. V3885 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3885 Oph |reasonably good light curve. V3886 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3886 Oph |reasonably good light curve. V3887 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3887 Oph |reasonably good light curve. V3888 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3888 Oph |reasonably good light curve. V3889 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3889 Oph |reasonably good light curve. V3890 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3890 Oph |reasonably good light curve. V3891 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3891 Oph |reasonably good light curve. V3892 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3892 Oph |reasonably good light curve. V3893 Oph |Red. Photometry in [g0146] is uncalibrated but shows a reasonably V3893 Oph |good light curve. V3895 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3895 Oph |reasonably good light curve. V3896 Oph |Several close companions. Photometry in [g0146] is uncalibrated but V3896 Oph |shows a reasonably good light curve. V3897 Oph |Crowded, Gaia EDR3 identification is uncertain. Photometry in V3897 Oph |[g0146] is uncalibrated but shows a reasonably good light curve. V3898 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3898 Oph |reasonably good light curve. V3899 Oph |Crowded. Identification with Gaia-EDR3 is not quite certain. V3899 Oph |Photometry in [g0146] is uncalibrated but shows a reasonably good V3899 Oph |light curve. V3900 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3900 Oph |reasonably good light curve. V3901 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3901 Oph |reasonably good light curve. V3902 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3902 Oph |reasonably good light curve. V3903 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3903 Oph |reasonably good light curve. V3904 Oph |Several close companions. Photometry in [g0146] is uncalibrated but V3904 Oph |shows a reasonably good light curve. V3905 Oph |Red. Several close companions. Photometry in [g0146] is V3905 Oph |uncalibrated but shows a reasonably good light curve with slow V3905 Oph |variations. V3907 Oph |Red. Several close companions. Photometry in [g0146] is V3907 Oph |uncalibrated but shows a reasonably good light curve. V3908 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3908 Oph |reasonably good light curve. V3909 Oph |Several close companions. V3910 Oph |Several close companions. V3911 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3911 Oph |reasonably good light curve. V3912 Oph |Gaia EDR3 identification is uncertain. Red. Photometry in [g0146] V3912 Oph |is uncalibrated but shows a reasonably good light curve with slow V3912 Oph |variations. V3913 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3913 Oph |reasonably good light curve. V3914 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3914 Oph |reasonably good light curve. V3915 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3915 Oph |reasonably good light curve. V3916 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3916 Oph |reasonably good light curve. V3917 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3917 Oph |reasonably good light curve. V3918 Oph |Several close companions. V3919 Oph |Crowded, Gaia EDR3 identification is uncertain. Photometry in V3919 Oph |[g0146] is uncalibrated, but shows a moderately good light curve V3919 Oph |with a large scatter at minimum. V3920 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3920 Oph |reasonably good light curve. V3921 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3921 Oph |reasonably good light curve. V3922 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3922 Oph |reasonably good light curve. V3923 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3923 Oph |reasonably good light curve. V3924 Oph |Crowded. Red. Photometry in [g0146] is uncalibrated but shows a V3924 Oph |reasonably good light curve. V3925 Oph |VB B (A 15.5mG, B 15.9mG; AB 4.8", 91{deg}, 2000; other V3925 Oph |components). Photometry in [g0146] is uncalibrated but shows a V3925 Oph |reasonably good light curve. V3926 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3926 Oph |reasonably good light curve. V3927 Oph |Crowded. Red. Photometry in [g0146] is uncalibrated but shows a V3927 Oph |reasonably good light curve with slow variations. V3928 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3928 Oph |reasonably good light curve. V3929 Oph |Crowded. V3930 Oph |Crowded. V3931 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3931 Oph |reasonably good light curve. V3932 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3932 Oph |reasonably good light curve. V3933 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3933 Oph |reasonably good light curve. V3934 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3934 Oph |reasonably good light curve. V3935 Oph |Red. VB A (12.8mG; B 13.7mG, 3.7", 355{deg}, 2000; other V3935 Oph |components).Photometry in [g0146] is uncalibrated but shows a V3935 Oph |reasonably good light curve with slow variations. V3936 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3936 Oph |reasonably good light curve. V3937 Oph |Crowded. V3938 Oph |Crowded, reliable Gaia EDR3 identification was not possible. V3938 Oph |Photometry in [g0146] is uncalibrated but shows a reasonably good V3938 Oph |light curve. Blazhko effect? V3940 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3940 Oph |reasonably good light curve. V3941 Oph |Several close companions. Photometry in [g0146] is uncalibrated but V3941 Oph |shows a reasonably good light curve. V3943 Oph |Several close companions. Photometry in [g0146] is uncalibrated but V3943 Oph |shows a reasonably good light curve. V3944 Oph |VB B (A 15.7mG, B 16.2mG; AB 3.0", 95{deg}, 2000). V3945 Oph |Several close companions. V3946 Oph |Crowded. V3947 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3947 Oph |reasonably good light curve. V3948 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3948 Oph |reasonably good light curve. V3949 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3949 Oph |reasonably good light curve. V3950 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3950 Oph |reasonably good light curve. V3951 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3951 Oph |reasonably good light curve. V3952 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3952 Oph |reasonably good light curve. V3953 Oph |VB A (16.3mG; B 16.7mG, 3.5", 194{deg}, 2000). V3955 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3955 Oph |reasonably good light curve. V3956 Oph |Crowded. V3957 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3957 Oph |reasonably good light curve. V3959 Oph |Red. Photometry in [g0146] is uncalibrated but shows a reasonably V3959 Oph |good light curve. V3960 Oph |Crowded. V3961 Oph |VB A (15.9mG; B 16.7mG, 4.8", 224{deg}, 2000; other components). V3961 Oph |Photometry in [g0146] is uncalibrated but shows a reasonably good V3961 Oph |light curve. V3964 Oph |VB B (A 15.1mG, B 16.2mG; AB 4.1", 47{deg}, 2000). V3965 Oph |Crowded. Photometry in [g0146] is uncalibrated but shows a V3965 Oph |reasonably good light curve. V3966 Oph |Crowded. V3969 Oph |VB A (15.9mG; B 16.2mG, 3.6", 325{deg}, 2000; other components). V3970 Oph |Crowded. V3972 Oph |VB B (A 13.3mG, B 16.2mG; AB 3.8", 63{deg}, 2000). V3973 Oph |Several close companions. Photometry in [g0146], [g0147] is V3973 Oph |uncalibrated but shows reasonably good light curves. V3975 Oph |Several close companions. Photometry in [g0146] is uncalibrated but V3975 Oph |shows a reasonably good light curve. V3976 Oph |Several close companions. V3978 Oph |Several close companions. V3979 Oph |VB A (16.2mG; B 17.2mG, 3.4", 187{deg}, 2000). V3981 Oph |Several close companions. V3983 Oph |VB A (15.8mG; B 16.1mG, 2.3", 94{deg}, 2000). V3985 Oph |VB A (15.9mG; B 16.5mG, 4.0", 197{deg}, 2000; other components). V3986 Oph |VB A (16.1mG; B 16.2mG, 3.7", 348{deg}, 2000). V3987 Oph |VB B (A 13.8mG, B 15.9mG; AB 5.0", 177{deg}, 2000). V3989 Oph |VB A (16.1mG; B 16.8mG, 4.2", 253{deg}, 2000; other companions). V3990 Oph |VB A (16.0mG; B 17.2mG, 4.4", 37{deg}, 2000). V3992 Oph |VB A (16.1mG; B 17.5mG, 3.2", 136{deg}, 2000). V3993 Oph |VB B (A 15.9mG, B 15.0mG; AB 4.8", 48{deg}, 2000). V3996 Oph |Cluster non-member? V3998 Oph |VB A (16.1mG; B 17.5mG, 3.1", 230{deg}, 2000; other components). V3999 Oph |Crowded. V4001 Oph |VB A (15.7mG; B 16.4mG, 4.2", 64{deg}, 2000). V4005 Oph |VB B (A = PU Oph = NGC 6266 V29, 16.0mG; B 16.2mG; AB 4.3", 2{deg}, V4005 Oph |2000). V4007 Oph |VB A (16.0mG; B 16.0mG, 1.8", 0{deg}, 2000). V4011 Oph |P varies. VB B (A 15.8mG, B 16.1mG; AB 4.4", 0{deg}, 2000). V4013 Oph |Cluster non-member. VB A (16.7mG; B 16.8mG, 3.9", 113{deg}, 2000). V4017 Oph |Cluster non-member? V4018 Oph |Cluster non-member? V4020 Oph |VB A (16.0mG; B 16.2mG, 3.5", 88{deg}, 2000; other companions). V4022 Oph |VB A (16.2mG; B 17.6mG, 4.7", 349{deg}, 2000). Cluster non-member. V4023 Oph |Cluster non-member from the Gaia EDR3 proper motion. V4031 Oph |P varies? [g0160]. V4033 Oph |P varies. Gaia DR2 proper motion suggests that the star may be a V4033 Oph |cluster non-member. V4036 Oph |Cluster non-member. V4037 Oph |Cluster non-member? V4038 Oph |Cluster membership is uncertain. V4039 Oph |Crowded. V4041 Oph |Cluster non-member? V4042 Oph |Crowded. V4043 Oph |Crowded. V4051 Oph |P = 0.9769d is also possible. V4062 Oph |According to [g0165], also exhibits short-term variations. V4064 Oph |Listed as a suspected variable in [g0165]. V4068 Oph |Cluster non-member? V4069 Oph |Cluster non-member. V4071 Oph |Cluster non-member? V4072 Oph |VB B (A 16.0mG, B 16.1mG; AB 2.5", 144{deg}, 2000). V4073 Oph |Cluster non-member? V4074 Oph |VB B (A 14.4mG, B 16.1mG; AB 1.2", 9{deg}, 2000). V4075 Oph |VB C (A 14.0mG, B 14.9mG, C 16.0mG; AC 1.2", 101{deg}, 2000; BC V4075 Oph |3.7", 92{deg}, 2000). V4076 Oph |Heavily crowded field. P varies, dP/dt = +0.032 x 10^(-6) d/d. V4077 Oph |Crowded. V4078 Oph |Near the cluster center, crowded. V4079 Oph |Crowded. V4080 Oph |Near the cluster center. V4081 Oph |Near the cluster center. V4082 Oph |The elements in the Table are for the first overtone. Possible V4082 Oph |fundamental mode: P0 = 0.492734, P1/P0 = 0.7444. VB B (A 14.8mG, B V4082 Oph |16.0mG; AB 2.6", 69{deg}, 2000). V4084 Oph |Crowded. Blazhko effect? V4086 Oph |P varies, dP/dt = +0.013 x 10^(-6) d/d. VB C (A 14.8mG, B 15.1mG, C V4086 Oph |16.1mG; AC 3.5". 9{deg}, 2000; AB 2.5", 325{deg}, 2000). V4087 Oph |VB A (15.9mG; B 16.1mG, 1.6", 71{deg}, 2000; other components, also V4087 Oph |brighter ones, at larger distances). V4088 Oph |Blazhko effect. V4089 Oph |VB B (A 15.7mG, B 15.8mG; AB 2", 351{deg}, 2000; other components). V4091 Oph |Blazhko effect? V4094 Oph |Cluster non-member? VB A (15.8mG; B 16.9mG, 2", 102{deg}, 2000). V4108 Oph |Cluster non-member? V4110 Oph |Cluster non-member, background object? [0169]. Proper motion agrees V4110 Oph |with cluster members [g0001]. V4113 Oph |Multiperiodic. V4114 Oph |Cluster non-member? V4115 Oph |Cluster non-member? V4118 Oph |Cluster non-member. V4120 Oph |VB A (16.9mG; B 16.9mG, 5", 165{deg}, 2000). V4124 Oph |Cluster non-member. VB A (14.7mG; B 15.4mG, 3", 167{deg}, 2000). V4124 Oph |O'Connell effect in data from [g0170]. V4129 Oph |VB A (17.0mG; B 17.1mG, 3", 152{deg}, 2000). V4130 Oph |VB B (A 15.6mG, B 16.9mG; AB 2", 238{deg}, 2000; other companions). V4134 Oph |Several close companions. V4136 Oph |Several close companions. V4137 Oph |VB A (16.7mG; B 17.2mG, 3", 85{deg}, 2000). V4138 Oph |Several close companions. V4139 Oph |Several close companions. V4140 Oph |VB B (A 17.0mG, B 15.7mG; AB 2", 278{deg}, 2000). V4144 Oph |VB A (17.1mG; B = NGC 6402 V087, type CST, 17.2mG, 3", 53{deg}, V4144 Oph |2000). V4146 Oph |VB A (13.6mG; B 14.6mG, 3", 44{deg}, 2000). V4149 Oph |Crowded. V4152 Oph |Crowded. V4153 Oph |VB A (15.0mG; B 15.4mG, 3", 277{deg}, 2000; other companions). V4155 Oph |Several close companions. V4156 Oph |Several close companions. V4157 Oph |Crowded. V4158 Oph |Crowded. V4159 Oph |Several close companions. V4160 Oph |VB C (A 16.0mG, B 16.6mG, C 16.8mG; AB 3", 181{deg}, 2000; AC 4.5", V4160 Oph |198{deg}, 2000). V4161 Oph |Crowded. V4163 Oph |Crowded. V4164 Oph |Crowded. V4166 Oph |Several close companions. V4168 Oph |Strongly crowded. V4169 Oph |Crowded, brighter companion. V4170 Oph |Crowded. V4171 Oph |Several close companions. V4172 Oph |Several close companions. V4173 Oph |Crowded. V4174 Oph |Crowded. V4175 Oph |Several close companions. V4176 Oph |Several close companions. V4177 Oph |Several close companions. V4178 Oph |Strongly crowded. V4179 Oph |Blended? According to [g0170], RRAB (RR0), P = 0.52244d. V4180 Oph |Strongly crowded. V4181 Oph |VB B (A 14.7mG, B 16.9mG; AB 1.2", 276{deg}, 2000; other V4181 Oph |companions). V4183 Oph |Crowded. V4184 Oph |Crowded. V4185 Oph |Strongly crowded. V4186 Oph |Crowded. V4187 Oph |Several close companions. V4188 Oph |Crowded. V4190 Oph |Crowded. V4192 Oph |Crowded. V4193 Oph |Crowded, close bright companions. V4194 Oph |Crowded. V4195 Oph |VB B (A 15.6mG, B 17.0mG; AB 2", 166{deg}, 2000). V4196 Oph |Crowded. V4197 Oph |Several close companions. V4199 Oph |VB B (A 16.8mG, B 16.9mG; AB 4", 199{deg}, 2000). V4200 Oph |Strongly crowded. V4201 Oph |Crowded. V4204 Oph |Several close companions. V4206 Oph |Crowded. V4209 Oph |Several close companions. V4210 Oph |VB B (A 15.8mG, B 16.9mG; AB 2", 53{deg}, 2000). V4211 Oph |VB C (A 14.3mG, B 15.3mG, C 17.1mG; AC 1.3", 136{deg}, 2000; BC 3", V4211 Oph |163{deg}, 2000). V4214 Oph |Several close companions. V4215 Oph |VB B (A 14.8mG, B 16.8mG; AB 3", 321{deg}, 2000). V4216 Oph |Several close companions. V4218 Oph |VB A (13.3mG; B 14.5mG, 2.6", 180{deg}, 2000). V4219 Oph |VB A (17.0mG; B 17.1mG, 2.4", 179{deg}, 2000). V4222 Oph |Several close companions. V4226 Oph |VB B (A 15.1mG, B 17.0mG; AB 5", 186{deg}, 2000). V4230 Oph |VB A (16.8mG; B 18.0mG, 2.3", 341{deg}, 2000). V4231 Oph |Several close companions. V4234 Oph |VB C (A 14.6mG, B 16.6mG, C 16.9mG; AC 3.7", 73{deg}, 2000; BC V4234 Oph |5.6", 264{deg}, 2000). V4237 Oph |VB B (A 16.5mG, B 17.1mG, C 17.4mG; AB 3.7", 173{deg}, 2000; BC V4237 Oph |4.5", 82{deg}, 2000). V4241 Oph |Several close companions. V4242 Oph |VB C (A 14.6mG, B 15.8mG, C 16.9mG; AC 3.4", 292{deg}, 2000; BC V4242 Oph |6.7", 133{deg}, 2000). V4243 Oph |VB B (A 13.3mG, B 17.1mG, C 17.1mG; AB 4.9", 279{deg}, 2000; BC V4243 Oph |1.8", 10{deg}, 2000). V4254 Oph |Outside the cluster half-light radius, cluster non-member. V4255 Oph |Outside the cluster half-light radius, cluster non-member. V4256 Oph |Outside the cluster half-light radius, cluster non-member. V4257 Oph |VB B (A 13.9mG, B 15.8mG; AB 1.6", 68{deg}, 2000). Outside the V4257 Oph |cluster half-light radius, cluster non-member. V4258 Oph |Outside the cluster half-light radius, cluster non-member. V4259 Oph |Crowded. V4261 Oph |Several close companions. V4262 Oph |Several close companions. V4263 Oph |VB B (A 13.51mG, B 13.52mG; AB 2.2", 277{deg}, 2000). Outside the V4263 Oph |cluster half-light radius, cluster non-member. V4264 Oph |Outside the cluster half-light radius, cluster non-member. V4265 Oph |Several close companions. V4267 Oph |Outside the cluster half-light radius, probably cluster non-member. V4268 Oph |VB A (17.4mG; B 17.6mG, 5", 295{deg}, 2000). V4269 Oph |VB B (A 16.1mG, B 17.2mG; AB 1.8", 264{deg}, 2000). V4270 Oph |Crowded. V4271 Oph |Several close companions. V4273 Oph |Several close companions. V4274 Oph |Crowded. V4275 Oph |Several close companions. V4276 Oph |VB B (A 17.2mG, B 17.4mG; AB 2.5", 16{deg}, 2000; other V4276 Oph |components). V4277 Oph |Crowded. V4278 Oph |Crowded. V4279 Oph |Double-mode, also P = 0.2575d. One of the modes (or both) can be V4279 Oph |non-radial. Two objects separated by 0.6" in the Gaia EDR3 catalog; V4279 Oph |superposition of two variables? V4280 Oph |Crowded. V4281 Oph |Crowded. V4282 Oph |Crowded. V4284 Oph |VB B (A 16.9mG, B 17.9mG; AB 1.8", 38{deg}, 2000). V4285 Oph |Crowded. V4286 Oph |Crowded. V4287 Oph |Crowded. V4288 Oph |Crowded. V4289 Oph |Crowded. V4290 Oph |Crowded. V4291 Oph |Crowded. V4292 Oph |Outside the cluster half-light radius, cluster non-member. V4293 Oph |Crowded. V4294 Oph |Outside the cluster half-light radius, probably cluster non-member. V4294 Oph |Crowded. V4295 Oph |VB B (A 16.4mG, B 17.3mG; AB 2.2", 24{deg}, 2000). V4296 Oph |VB B (A 15.7mG, B 17.3mG; AB 3.7", 201{deg}, 2000; other V4296 Oph |components). V4297 Oph |Several close companions. V4298 Oph |VB C (A 14.6mG, B 17.1mG, C 17.3mG; AB 4.8", 132{deg}, 2000; AC V4298 Oph |3.0", 117{deg}, 2000). V4299 Oph |Several close companions. V4300 Oph |Several close companions. Cluster non-member? V4301 Oph |Several close companions. V4302 Oph |Several close companions. V4304 Oph |VB A (16.0mG; B 16.3mG, 2.4", 329{deg}, 2000; other components). V4305 Oph |Crowded. V4306 Oph |Cluster non-member? V4308 Oph |Crowded. V4309 Oph |Crowded. V4310 Oph |VB B (A 15.8mG, B 17.3mG; AB 1.7", 307{deg}, 2000). V4311 Oph |VB B (A 17.2mG, B 17.3mG; AB 3.7", 123{deg}, 2000). V4312 Oph |Several close companions. V4313 Oph |Crowded. V4315 Oph |Crowded. V4316 Oph |P = 0.26205d is also possible. V4318 Oph |First overtone: see Table. Fundamental mode: P = 0.54194d. P1/P0 = V4318 Oph |0.7452. A1/A0 = 2.06. V4322 Oph |VB A (17.9mG, 18.5mG, 4.6", 28{deg}, 2000). V4324 Oph |P varies? Light curve shape varies? V4325 Oph |VB B (A 17.3mG, B 17.9mG; AB 2.4", 95{deg}, 2000). V4326 Oph |VB A (17.9mG, 18.9mG, 2.5", 299{deg}, 2000). V4327 Oph |Several close companions. V4328 Oph |VB A (18.0mG, 19.0mG, 2.4", 255{deg}, 2000). V4331 Oph |Cluster non-member? tet Oph |SB1 (Porb = 11.44d [06597]). The basic oscillation (see Table) is tet Oph |superimposed by oscillations with the periods: P1 = 0.092551d, P2 = tet Oph |0.069452d, P3 = 0.0555d, P4 = 0.0464d, P02 = 0.137255d, P13 = tet Oph |0.13845d, P24 = 0.13990d, P03 = 0.09185d. khi Oph |SB 1 (Porb = 138.8d [09558]). ome Oph |P = 1.5d? R Ori |SC 5/9.5 E. P var. Max = 2399420 + 378d*E (JD2395600 - 99500); Max R Ori |= 2412687 + 378.1d*E (JD2403200 - 12700); Max = 2414230 + 366.5d*E R Ori |(JD2413800 - 16800); Max = 2417943 + 378.1d*E (JD2416800 - 21350); R Ori |Max = 2421352 + 384.9d*E (JD2421350 - 24100); since JD2424100 - see R Ori |Table. S Ori |VB A (B 10.9m, 47", 228{deg}). SiO maser. P var. Max = 2404538 + S Ori |412.00d*E (JD2404520 - 13600); Max = 2414014 + 427.15d*E (JD2414000 S Ori |- 19150); Max = 2419567 + 416.11d*E (JD2419570 - 22890); Max = S Ori |2423312 + 407.10d*E (JD2423320 - 31050); Max = 2431454 + 438.53d*E S Ori |(JD2431500 - 39000) [03765]; since JD2439000 - see Table. T Ori |In the T-association of the Orion nebula. Connected with a cometary T Ori |nebula. U Ori |SiO, OH, H2O maser. P var. Max = 2409881 + 374.5d*E (JD2409800 - U Ori |15900); Max = 2415871 + 367.9d*E (JD2415900 - 21000); Max = 2421016 U Ori |+ 376.0d*E (JD2421000 - 29300); Max = 2428164 + 368.3d*E (JD2428100 U Ori |- 32900) [00960]; Max = 2433336 + 372.7d*E (JD2432900 - 43800); U Ori |since JD2443800 - see Table. V Ori |P var. Max = 2413656 + 264.8d*E (JD2411800 - 18700); Max = 2418987 V Ori |+ 271.7d*E (JD2418700 - 24600); Max = 2424695 + 263.7d*E (JD2424600 V Ori |- 29400) [00960]; Max = 2430769 + 269.9d*E (JD2430700 - 36200); V Ori |since JD2437700 - see Table. W Ori |Mean magnitude varies with P = 2450d. Z Ori |Min II 9.9; d = 0.013P. RS Ori |P var. Max = 2428073.205 + 7.566836d*E (JD2416500 - 33000); since RS Ori |JD2435000 - see Table. RT Ori |Mean magnitude varies with P = 3200d. RU Ori |In the region of the nebula IC 434. RV Ori |In the region of the nebula IC 434. RW Ori |In the region of the nebula IC 434. RX Ori |In the region of the Orion nebula T-association. RZ Ori |In the region of the Orion nebula T-association. SS Ori |In the region of the Orion nebula T-association. ST Ori |In the region of the Orion nebula T-association. SU Ori |In the region of the Orion nebula T-association. SV Ori |In the region of the Orion nebula T-association. SW Ori |In the region of the Orion nebula T-association. SX Ori |In the region of the Orion nebula T-association. SY Ori |In the region of the Orion nebula T-association. SZ Ori |In the region of the Orion nebula T-association. TT Ori |In the region of the Orion nebula T-association. TU Ori |In the region of the Orion nebula T-association. TV Ori |In the region of the Orion nebula T-association. TW Ori |In the region of the Orion nebula T-association. TX Ori |VB A (B = TY Ori, 42.4", 45{deg}); in the region of the nebula IC TX Ori |434. TY Ori |VB B (A = TX Ori); in the region of the nebula IC 434. TZ Ori |In the region of the nebula IC 434. UW Ori |Min II 11.6. UY Ori |In the region of the Orion nebula T-association. UZ Ori |In the region of the Orion nebula T-association. VV Ori |Min II 5.50; dI = 0.055P; dII = 0.064P. There is third component in VV Ori |the system (Porb = 119.09d [08045]). VW Ori |In the region of the Orion nebula T-association. VX Ori |In the region of the Orion nebula T-association. VY Ori |VB A (B = 16.6mV, 16", 135{deg}). In the region of the Orion nebula VY Ori |T-association. VZ Ori |In the region of the Orion nebula T-association. WW Ori |In the region of the Orion nebula T-association. WX Ori |VB A (B 17m, 11", 10{deg}). In the region of the Orion nebula WX Ori |T-association. WY Ori |In the region of the Orion nebula T-association. WZ Ori |In the region of the Orion nebula T-association. XX Ori |In the region of the Orion nebula T-association. XY Ori |In the region of the Orion nebula T-association. XZ Ori |The periodicity in light variations is possible. In the region of XZ Ori |the Orion nebula T-association. YY Ori |Emission. In the region of the Orion nebula T-association. YZ Ori |In the region of the Orion nebula T-association. ZZ Ori |In the region of the Orion nebula T-association. AA Ori |In the region of the Orion nebula T-association. AB Ori |In the region of the Orion nebula T-association. AC Ori |In the region of the Orion nebula T-association. AE Ori |In the region of the Orion nebula T-association. AF Ori |In the region of the Orion nebula T-association. AG Ori |VB A (B 16.4mV, 16", 185{deg}). In the region of the Orion nebula AG Ori |T-association. AH Ori |In the region of the Orion nebula T-association. AI Ori |In the region of the Orion nebula T-association. AK Ori |In the region of the Orion nebula T-association. AL Ori |In the region of the Orion nebula T-association. AM Ori |VB A (B 20.3mV, 3.5", 320{deg}). In the region of the Orion nebula AM Ori |T-association. AN Ori |In the region of the Orion nebula T-association. AO Ori |In the region of the Orion nebula T-association. AP Ori |In the region of the Orion nebula T-association. AQ Ori |In the region of the Orion nebula T-association. AR Ori |VB A (B 2", 240{deg}). In the region of the Orion nebula AR Ori |T-association. AS Ori |In the region of the Orion nebula T-association. AT Ori |In the region of the Orion nebula T-association. AU Ori |In the region of the Orion nebula T-association. AV Ori |VB A (B 18.7mV, 6", 305{deg}). In the region of the nebula AV Ori |T-association. AW Ori |In the region of the Orion nebula T-association. AX Ori |In the region of the Orion nebula T-association. AY Ori |In the region of the Orion nebula T-association. AZ Ori |In the region of the Orion nebula T-association. BB Ori |In the region of the Orion nebula T-association. BC Ori |In the region of the Orion nebula T-association. BD Ori |In the region of the Orion nebula T-association. BE Ori |In the region of the Orion nebula T-association. BF Ori |In the region of the Orion nebula T-association. BG Ori |In the region of the nebula IC 434. BH Ori |In the region of the Orion nebula T-association. BK Ori |P var. Max = 2422016 + 338.0d*E (JD2413550 - 22100); Max = 2428880 BK Ori |+ 326.5d*E (JD2422300 - 28880); Max = 2429940 + 345.3d*E (JD2428880 BK Ori |- 29940); Max = 2432892 + 327.7d*E (JD2429940 - 32900); Max = BK Ori |2438800 + 346.3d*E (JD2432900 - 38800); since JD2438800 - see BK Ori |Table. BM Ori |In the region of the Orion nebula T-association. In the cluster NGC BM Ori |1976. Orion Trapezium member: teta**1 Ori B (A = V1016 Ori; B 8.7", BM Ori |32{deg}; C 5.13m, 13.1", 131{deg}; D 6.70m, 21.6", 96{deg}). d = BM Ori |0.05P; Min II 7.98. Shape of the light curve and depths of minima BM Ori |vary. BO Ori |In the region of the Orion nebula T-association. BP Ori |In the region of the Orion nebula T-association. BS Ori |In the region of the Orion nebula T-association. BT Ori |In the region of the Orion nebula T-association. BU Ori |In the region of the Orion nebula T-association. BV Ori |In the region of the Orion nebula T-association. BW Ori |In the region of the Orion nebula T-association. BX Ori |In the region of the Orion nebula T-association. BY Ori |In the region of the Orion nebula T-association. BZ Ori |In the region of the Orion nebula T-association. CC Ori |In the region of the Orion nebula T-association. CD Ori |In the region of the Orion nebula T-association. CE Ori |In the region of the Orion nebula T-association. CF Ori |In the region of the Orion nebula T-association. CG Ori |In the region of the Orion nebula T-association. CH Ori |In the region of the Orion nebula T-association. CI Ori |VB A (B 9.70m, 12.9", 88{deg}). CM Ori |P var? CN Ori |Porb = 0.163097d. Light curve is superposed by oscillations with CN Ori |the following elements: Max0 = 2444941.5032 + 0.163097d*E (A0 = CN Ori |0.2m), Max1 = 2444941.573 + 0.15946d*E (A1 = 0.1m) [09471]. CN Ori |Sometimes smaller rapid light oscillations are also observed with CN Ori |periods 24.3s - 29.5s (A<1%). CO Ori |Member of the T-association CO Ori. VB A (B 13m, 1", 280{deg}). CP Ori |Min II 11.2. P var [02545]. CT Ori |SRD? P = 68d? [09496]. CW Ori |Min II 13.2. DK Ori |In the region of the Orion nebula T-association. VB (ro < 3"). DL Ori |In the region of the Orion nebula T-association. DM Ori |In the region of the Orion nebula T-association. DN Ori |Min II 9.9; d = 0.026P. P var. Min I = 2428497.51 + 12.9649d*E DN Ori |(JD2425200 - 28600); since JD2435570 - see Table. DY Ori |B - V: +0.58, +1.72. EG Ori |d = 0.086P. P var? EQ Ori |Min II 10.3. P var. Min I = 2425889.706 + 1.74608d*E (JD2425600 - EQ Ori |26700) [02839]; Min I = 2429219.467 + 1.74611d*E (JD2427700 - EQ Ori |31000) [00001]; since JD2431000 - see Table. ER Ori |VB A (B 13.6", 0{deg}). Min II 9.97. P var. Min I = 2426336.6485 + ER Ori |0.4233955d*E (JD2426330 - 33920) [00279]; Min I = 2434765.6306 + ER Ori |0.42340620d*E (JD2433920 - 35475) [02278]; Min I = 2436508.7851 + ER Ori |0.4234009d*E (JD2435475 - 40000) [03787]; since JD2440000 - see ER Ori |Table. Shape of the light curve varies. ET Ori |Min II 11.3. P var? EW Ori |Min II 10.5; Min II - Min I = 0.529P. In the region of the open EW Ori |cluster CR 70. In [00007] Min II are accepted to be Min I, and vice EW Ori |versa (Min II - Min I = 0.47P). For decisive choice of the Min I EW Ori |epoch photoelectric observations are necessary. P var? Min II = EW Ori |2429974.810 + 6.9368005d*E [00007]; since JD2430000 - see Table. EY Ori |Min II 9.54; d = 0.003P. In the region of the Orion nebula EY Ori |T-association. P var. Min I = 2427310.420 + 16.787450d*E [00007]; EY Ori |since JD2427500 - see Table. EZ Ori |In the region of the Orion nebula T-association. FF Ori |Min II 10.3. FH Ori |d = 0.035P. P var. FI Ori |VB A (B 10.5m, 5", 323{deg}). Shape of the light curve varies, FI Ori |probably periodically [03790,05475]. FK Ori |P var. Min = 2427773.390 + 1.947447d*E (JD2426900 - 37500); since FK Ori |JD2437500 - see Table. FL Ori |P var. Min = 2427452.271 + 1.550971d*E (JD2427450 - 29600) [03115]; FL Ori |Min = 2430400.649 + 1.55093d*E (JD2429600 - 30400);Min = FL Ori |2432517.755 + 1.550991d*E (JD2430400 - 32900); Min = 2434459.571 + FL Ori |1.550965d*E (JD2432900 - 35050); Min = 2436649.568 + 1.550995d*E FL Ori |(JD2435050 - 40600); since JD2440600 - see Table. FO Ori |Min II 9.7; d = 0.005P. FR Ori |Min II 11.1. FT Ori |Min II 9.60; DII = 0.08P; Min II - Min I = 0.73P. P var. Min I = FT Ori |2433009.553 + 3.150404d*E (JD2426380 - 38000) [02758]; since FT Ori |JD2438000 - see Table. The period of apsidal motion 520 +- 100 FT Ori |years [07358]. FU Ori |Member of FU Ori T-association. In the dark globule B35. Connected FU Ori |with a bright cometary nebula and the bright hydrogen nebula S 280. FU Ori |Light maximum was in summer 1937. IN 1980 - 10.6m B. FZ Ori |Min II 11.2. GG Ori |Min II 11.1; Min II - Min I = 0.427P. GP Ori |SC 7/8- . GQ Ori |VB A (B 9.7m, 31", 324{deg}). GW Ori |In the T-association CO Ori. GX Ori |In the T-association CO - Ori. GY Ori |In the T-association CO - Ori. GZ Ori |In the region of the Orion nebula T-association. HH Ori |In the region of the Orion nebula T-association. HI Ori |In the T-association CO - Ori. HK Ori |In the T-association CO - Ori. Connected with a bright cometary HK Ori |nebula. CO, CH, OH emission. HL Ori |In the region of the Orion nebula T-association. HM Ori |In the T-association CO - Ori. HN Ori |In the region of the Orion nebula T-association. HO Ori |In the region of the Orion nebula T-association. HP Ori |In the region of the Orion nebula T-association. HQ Ori |In the region of the Orion nebula T-association. HR Ori |In the region of the Orion nebula T-association. HS Ori |In the region of the Orion nebula T-association. HT Ori |In the region of the Orion nebula T-association. HU Ori |In the region of the Orion nebula T-association. HV Ori |In the region of the Orion nebula T-association. HW Ori |In the region of the Orion nebula T-association. HX Ori |In the region of the Orion nebula T-association. HY Ori |In the region of the Orion nebula T-association. HZ Ori |In the region of the Orion nebula T-association. II Ori |In the region of the Orion nebula T-association. IK Ori |In the region of the Orion nebula T-association. IL Ori |In the region of the Orion nebula T-association. IM Ori |In the region of the Orion nebula T-association. IN Ori |In the region of the Orion nebula T-association. IO Ori |In the region of the Orion nebula T-association. IP Ori |In the region of the Orion nebula T-association. IQ Ori |In the region of the Orion nebula T-association. IR Ori |In the region of the Orion nebula T-association. IS Ori |In the region of the Orion nebula T-association. IT Ori |In the region of the Orion nebula T-association. IU Ori |In the region of the Orion nebula T-association. IV Ori |In the region of the Orion nebula T-association. IW Ori |In the region of the Orion nebula T-association. IX Ori |In the region of the Orion nebula T-association. IY Ori |In the region of the Orion nebula T-association. IZ Ori |In the region of the Orion nebula T-association. KK Ori |In the region of the Orion nebula T-association. KL Ori |In the region of the Orion nebula T-association. KM Ori |In the region of the Orion nebula T-association. KN Ori |In the region of the Orion nebula T-association. KO Ori |In the region of the Orion nebula T-association. KP Ori |In the region of the Orion nebula T-association. KQ Ori |In the region of the Orion nebula T-association. KR Ori |In the region of the Orion nebula T-association. KS Ori |In the region of the Orion nebula T-association. KT Ori |In the region of the Orion nebula T-association. KU Ori |In the region of the Orion nebula T-association. KV Ori |In the region of the Orion nebula T-association. KW Ori |In the region of the Orion nebula T-association. KX Ori |In the region of the Orion nebula T-association. KY Ori |In the region of the Orion nebula T-association. KZ Ori |In the region of the Orion nebula T-association. LL Ori |In the region of the Orion nebula T-association. LM Ori |In the region of the Orion nebula T-association. LN Ori |In the region of the Orion nebula T-association. LO Ori |In the region of the Orion nebula T-association. LP Ori |In the region of the Orion nebula T-association. LQ Ori |In the region of the Orion nebula T-association. LR Ori |In the region of the Orion nebula T-association. LS Ori |In the region of the Orion nebula T-association. LT Ori |In the region of the Orion nebula T-association. LU Ori |In the region of the Orion nebula T-association. LV Ori |In the region of the Orion nebula T-association. LW Ori |In the region of the Orion nebula T-association. LX Ori |In the region of the Orion nebula T-association. LY Ori |In the region of the Orion nebula T-association. LZ Ori |VB B (A 10.3m; B 14.1", 219{deg}). In the region of the Orion LZ Ori |nebula T-association. MM Ori |In the region of the Orion nebula T-association. MN Ori |In the region of the Orion nebula T-association. MO Ori |In the region of the Orion nebula T-association. MP Ori |In the region of the Orion nebula T-association. MQ Ori |In the region of the Orion nebula T-association. MR Ori |In the region of the Orion nebula T-association. MS Ori |In the region of the Orion nebula T-association. MT Ori |In the region of the Orion nebula T-association. MU Ori |In the region of the Orion nebula T-association. MV Ori |In the region of the Orion nebula T-association. MW Ori |In the region of the Orion nebula T-association. MX Ori |In the region of the Orion nebula T-association. MY Ori |In the region of the Orion nebula T-association. MZ Ori |In the region of the Orion nebula T-association. NN Ori |In the region of the Orion nebula T-association. NO Ori |In the region of the Orion nebula T-association. NP Ori |In the region of the Orion nebula T-association. NQ Ori |In the region of the Orion nebula T-association. NR Ori |In the region of the Orion nebula T-association. NS Ori |In the region of the Orion nebula T-association. NT Ori |In the region of the Orion nebula T-association. NU Ori |In the region of the Orion nebula T-association. In the nebula NGC NU Ori |1982. Dust shell. NV Ori |In the region of the Orion nebula T-association. NW Ori |In the region of the Orion nebula T-association. NX Ori |In the region of the Orion nebula T-association. NY Ori |VB B (A = V566 Ori; B 5", 135{deg}). In the region of the Orion NY Ori |nebula T-association. NZ Ori |In the region of the Orion nebula T-association. OO Ori |In the region of the Orion nebula T-association. OP Ori |In the region of the Orion nebula T-association. OQ Ori |In the region of the Orion nebula T-association. OR Ori |In the region of the Orion nebula T-association. OT Ori |In the region of the Orion nebula T-association. OU Ori |In the region of the Orion nebula T-association. OV Ori |In the region of the Orion nebula T-association. OW Ori |In the region of the Orion nebula T-association. OX Ori |In the region of the Orion nebula T-association. OY Ori |In the region of the Orion nebula T-association. OZ Ori |In the region of the Orion nebula T-association. PP Ori |In the region of the Orion nebula T-association. PQ Ori |In the region of the nebula IC 434. PR Ori |In the region of the Orion nebula T-association. PS Ori |In the region of the Orion nebula T-association. PT Ori |In the region of the Orion nebula T-association. PU Ori |In the region of the nebula IC 434. PV Ori |In the region of the Orion nebula T-association. PW Ori |In the region of the Orion nebula T-association. PX Ori |Vr = + 298 km/s [09511]. In the region of the Orion nebula PX Ori |T-association. PY Ori |In the region of the Orion nebula T-association. PZ Ori |In the region of the Orion nebula T-association. QQ Ori |In the region of the Orion nebula T-association. QR Ori |In the region of T-association FU Ori. QT Ori |P var? Elements given in the Table are valid in the interval QT Ori |JD2429640 - 35550. V0340 Ori |Epoch of Min brightness is given. V0343 Ori |Min II 11.0. Shape of the light curve and depth of Min II vary. V0347 Ori |In the region of the Orion nebula T-association. V0348 Ori |In the region of the Orion nebula T-association. V0349 Ori |In the region of the Orion nebula T-association. V0353 Ori |In the region of the Orion nebula T-association. V0354 Ori |In the region of the Orion nebula T-association. V0355 Ori |In the region of the Orion nebula T-association. V0356 Ori |In the region of the Orion nebula T-association. V0357 Ori |In the region of the Orion nebula T-association. V0358 Ori |In the region of the Orion nebula T-association. V0359 Ori |In the region of the Orion nebula T-association. Epoch of Min HEI V0359 Ori |line intensity is given. According to [09512], P = 14.612d. V0360 Ori |In the region of the Orion nebula T-association. V0361 Ori |VB C (A 4.8m; B 6.1m, 52.4", 93{deg}; C 129", 97{deg}). In the V0361 Ori |region of the Orion nebula T-association. V0362 Ori |In the region of the Orion nebula T-association. V0363 Ori |In the region of the Orion nebula T-association. V0364 Ori |In the region of the Orion nebula T-association. V0365 Ori |In the region of the Orion nebula T-association. V0366 Ori |In the region of the Orion nebula T-association. V0367 Ori |In the region of the Orion nebula T-association. V0368 Ori |In the region of the Orion nebula T-association. V0369 Ori |In the region of the Orion nebula T-association. V0370 Ori |In the T-association CO - Ori. V0371 Ori |{mu} = 0.28", ro = 238{deg}. V0372 Ori |In the region of the Orion nebula T-association. V0373 Ori |In the region of the Orion nebula T-association. V0374 Ori |In the region of the Orion nebula T-association. V0375 Ori |In the region of the Orion nebula T-association. V0376 Ori |In the region of the Orion nebula T-association. V0377 Ori |In the region of the Orion nebula T-association. V0378 Ori |In the region of the Orion nebula T-association. V0379 Ori |In the region of the Orion nebula T-association. V0380 Ori |In the nebula NGC 1999. In the region of the Orion nebula V0380 Ori |T-association. Spectrum description [04002]. OH, CH emission. V0381 Ori |In the region of the Orion nebula T-association. V0382 Ori |P var. MAX = 2431146 + 227.8d*E (JD2429300 - 31200); Mean period is V0382 Ori |given in the Table (JD2428100 - 33700). V0383 Ori |In the region of the Orion nebula T-association. V0384 Ori |In the region of the Orion nebula T-association. V0385 Ori |In the region of the Orion nebula T-association. V0386 Ori |In the region of the Orion nebula T-association. V0387 Ori |In the region of the Orion nebula T-association. V0388 Ori |In the region of the Orion nebula T-association. V0389 Ori |In the region of the Orion nebula T-association. V0390 Ori |In the region of the Orion nebula T-association. V0391 Ori |In the region of the Orion nebula T-association. V0393 Ori |In the region of the Orion nebula T-association. V0394 Ori |In the region of the Orion nebula T-association. V0395 Ori |In the region of the Orion nebula T-association. V0396 Ori |In the region of the Orion nebula T-association. V0397 Ori |In the region of the Orion nebula T-association. V0398 Ori |In the region of the Orion nebula T-association. V0399 Ori |In the region of the Orion nebula T-association. V0400 Ori |In the region of the Orion nebula T-association. V0401 Ori |In the region of the Orion nebula T-association. V0402 Ori |In the region of the Orion nebula T-association. V0403 Ori |In the region of the Orion nebula T-association. V0404 Ori |In the region of the Orion nebula T-association. V0405 Ori |In the region of the Orion nebula T-association. V0406 Ori |In the region of the Orion nebula T-association. V0407 Ori |In the region of the Orion nebula T-association. V0408 Ori |In the region of the Orion nebula T-association. V0409 Ori |In the region of the Orion nebula T-association. V0410 Ori |In the region of the Orion nebula T-association. V0411 Ori |In the region of the Orion nebula T-association. V0412 Ori |In the region of the Orion nebula T-association. V0413 Ori |In the region of the Orion nebula T-association. V0414 Ori |In the region of the Orion nebula T-association. V0415 Ori |In the region of the Orion nebula T-association. V0416 Ori |In the region of the Orion nebula T-association. V0417 Ori |In the region of the Orion nebula T-association. V0418 Ori |In the region of the Orion nebula T-association. V0419 Ori |In the region of the Orion nebula T-association. V0420 Ori |In the region of the Orion nebula T-association. V0421 Ori |In the region of the Orion nebula T-association. V0422 Ori |In the region of the Orion nebula T-association. V0423 Ori |In the region of the Orion nebula T-association. V0424 Ori |In the region of the Orion nebula T-association. V0425 Ori |In the region of the Orion nebula T-association. V0426 Ori |In the region of the Orion nebula T-association. V0427 Ori |In the region of the Orion nebula T-association. V0428 Ori |In the region of the Orion nebula T-association. V0432 Ori |{Delta}(S) = 0. V0435 Ori |P var. Max = 2430350 + 186d*E (JD2429600 - 30730); Max = 2431373 + V0435 Ori |186d*E (JD2431370 - 3250) [02279]; since JD2434000 - see Table. V0436 Ori |In the T-association CO Ori. V0437 Ori |In the T-association CO Ori. V0438 Ori |In the T-association CO Ori. V0439 Ori |In the T-association CO Ori. V0441 Ori |In the T-association CO Ori. V0442 Ori |VB A (B 16.6m, 20", 73{deg}). In the T-association CO Ori. V0443 Ori |In the T-association CO Ori. V0444 Ori |In the T-association CO Ori. V0445 Ori |In the T-association CO Ori. V0446 Ori |In the T-association CO Ori. V0447 Ori |In the T-association CO Ori. V0448 Ori |In the T-association CO Ori. V0449 Ori |In the T-association CO Ori. In [08289] was considered as an EW V0449 Ori |type variable with the elements: Min I = 2430259.622 + 0.441990d*E V0449 Ori |(JD2430250 - 5550), 14.8m - 15.7m pg. V0450 Ori |In the T-association CO Ori. V0452 Ori |In the T-association CO Ori. V0453 Ori |In the T-association CO Ori. V0454 Ori |In the T-association CO Ori. V0455 Ori |In the T-association CO Ori. V0456 Ori |In the T-association CO Ori. V0457 Ori |In the T-association CO Ori. V0458 Ori |In the T-association CO Ori. V0460 Ori |In the T-association CO Ori. V0461 Ori |In the T-association CO Ori. V0463 Ori |In the T-association CO Ori. V0464 Ori |In the T-association CO Ori. V0465 Ori |In the T-association CO Ori. V0466 Ori |In the region of the Orion nebula T-association. V0467 Ori |In the T-association CO Ori. V0468 Ori |In the region of the Orion nebula T-association. V0470 Ori |In the region of the Orion nebula T-association. Star Pi 1411. Near V0470 Ori |to WY Ori = Pi 1396. V0473 Ori |In the region of the Orion nebula T-association. V0474 Ori |In the region of the Orion nebula T-association. V0475 Ori |In the region of the Orion nebula T-association. V0476 Ori |In the region of the open cluster {lambda} Ori. V0477 Ori |In the region of the open cluster {lambda} Ori. V0478 Ori |In the region of the Orion nebula T-association. V0479 Ori |In the region of the Orion nebula T-association. In the infrared V0479 Ori |A>1.5m. V0480 Ori |In the region of the Orion nebula T-association. In the infrared V0480 Ori |A>1.5m. V0481 Ori |In the region of the Orion nebula T-association. V0482 Ori |In the region of the Orion nebula T-association. V0484 Ori |In the region of the Orion nebula T-association. In the infrared V0484 Ori |A>1.0m. V0485 Ori |In the region of the Orion nebula T-association. In the infrared V0485 Ori |A>1.0m. V0486 Ori |In the region of the Orion nebula T-association. V0487 Ori |In the region of the Orion nebula T-association. V0489 Ori |In the region of the Orion nebula T-association. In the infrared V0489 Ori |A>1.0m. V0490 Ori |In the region of the Orion nebula T-association. In the infrared V0490 Ori |A>1.0m. V0491 Ori |In the region of the Orion nebula T-association. In the infrared V0491 Ori |A>1.0m. V0492 Ori |In the region of the Orion nebula T-association. Northern component V0492 Ori |of the close pair of infrared stars. In the infrared A = 1m. V0493 Ori |In the region of the Orion nebula T-association. In the infrared V0493 Ori |A>1.0m. V0494 Ori |In the region of the Orion nebula T-association. V0495 Ori |In the region of the Orion nebula T-association. Close binary (ro = V0495 Ori |0.24"). It is unknown which of the components varies. V0496 Ori |In the region of the Orion nebula T-association. In the infrared V0496 Ori |A>1.0m. V0497 Ori |In the region of the Orion nebula T-association. In the infrared V0497 Ori |A>1.0m. V0498 Ori |In the region of the Orion nebula T-association. V0500 Ori |In the region of the Orion nebula T-association. V0501 Ori |In the region of the Orion nebula T-association. V0502 Ori |In the region of the Orion nebula T-association. V0504 Ori |Min II 15.4. V0505 Ori |In the region of the nebula IC 434. V0507 Ori |In the region of the nebula IC 434. V0508 Ori |In the region of the nebula IC 434. V0509 Ori |In the region of the nebula IC 434. V0510 Ori |In the region of the nebula IC 434. V0511 Ori |In the region of the nebula IC 434. V0514 Ori |In the region of the nebula IC 434. V0516 Ori |Max = 2430325 + 139d*E (JD2430250 - 5350); P = 70d (JD2435350 - V0516 Ori |550). V0519 Ori |Min II 12.9. V0522 Ori |In the region of the nebula IC 434. V0523 Ori |In the region of the nebula IC 434. V0525 Ori |Min II 14.7. V0526 Ori |In the region of T-association FU Ori. V0529 Ori |Nova Ori 1678? Recurrent outburst was possibly observed at 1894 V0529 Ori |[02866]. Earlier the object was considered as nova Ori [1667 2862, V0529 Ori |2863, 2867, 2868], its existence being considered as doubtful V0529 Ori |[03813]. V0537 Ori |In the region of the open cluster {lambda} Ori. V0538 Ori |In the region of the Orion nebula T-association. V0539 Ori |In the region of the Orion nebula T-association. V0540 Ori |In the region of the Orion nebula T-association. V0541 Ori |In the region of the Orion nebula T-association. V0542 Ori |In the region of the Orion nebula T-association. V0544 Ori |In the region of the Orion nebula T-association. V0545 Ori |In the region of the Orion nebula T-association. V0546 Ori |In the region of the Orion nebula T-association. V0547 Ori |In the region of the Orion nebula T-association. V0548 Ori |In the region of the open cluster {lambda} Ori. V0549 Ori |In the region of the open cluster {lambda} Ori. V0550 Ori |In the region of the Orion nebula T-association. V0551 Ori |In the region of the Orion nebula T-association. V0552 Ori |In the region of the Orion nebula T-association. V0553 Ori |In the region of the Orion nebula T-association. V0554 Ori |In the region of the Orion nebula T-association. V0555 Ori |In the region of the Orion nebula T-association. V0556 Ori |In the region of the Orion nebula T-association. V0557 Ori |In the region of the Orion nebula T-association. V0559 Ori |In the region of the Orion nebula T-association. V0560 Ori |In the region of the Orion nebula T-association. V0561 Ori |In the region of the Orion nebula T-association. V0562 Ori |In the region of the Orion nebula T-association. V0563 Ori |In the region of the Orion nebula T-association. V0564 Ori |In the region of the Orion nebula T-association. V0565 Ori |In the region of the Orion nebula T-association. V0566 Ori |In the region of the Orion nebula T-association. V0567 Ori |In the region of the Orion nebula T-association. V0568 Ori |In the region of the Orion nebula T-association. V0569 Ori |In the region of the Orion nebula T-association. V0570 Ori |In the region of the Orion nebula T-association. V0571 Ori |In the region of the Orion nebula T-association. V0572 Ori |In the region of the open cluster {lambda} Ori. V0573 Ori |In the region of the Orion nebula T-association. V0574 Ori |In the region of the Orion nebula T-association. V0575 Ori |In the region of the Orion nebula T-association. V0576 Ori |In the region of the Orion nebula T-association. V0577 Ori |In the region of the Orion nebula T-association. V0578 Ori |In the region of the Orion nebula T-association. V0579 Ori |In the region of the Orion nebula T-association. V0580 Ori |In the region of the Orion nebula T-association. V0581 Ori |In the region of the Orion nebula T-association. V0582 Ori |In the region of the Orion nebula T-association. V0584 Ori |In the region of the Orion nebula T-association. V0585 Ori |In the region of the Orion nebula T-association. V0586 Ori |In the region of the Orion nebula T-association. V0587 Ori |In the region of the Orion nebula T-association. V0588 Ori |In the region of the Orion nebula T-association. V0589 Ori |In the region of the Orion nebula T-association. V0590 Ori |In the region of the Orion nebula T-association. V0591 Ori |In the region of the Orion nebula T-association. V0592 Ori |In the region of the Orion nebula T-association. V0593 Ori |In the region of the Orion nebula T-association. V0594 Ori |In the region of the Orion nebula T-association. V0595 Ori |In the region of the nebula IC 434. V0596 Ori |In the region of the open cluster {lambda} Ori. V0597 Ori |In the region of the nebula IC 434. V0598 Ori |In the region of the open cluster {lambda} Ori. V0599 Ori |In the region of the Orion nebula T-association. V0600 Ori |In the region of the nebula IC 434. V0601 Ori |In the region of the nebula IC 434. V0602 Ori |In the region of the nebula IC 434. V0603 Ori |In the region of the nebula IC 434. V0604 Ori |In the region of the nebula IC 434. V0605 Ori |In the region of the nebula IC 434. V0606 Ori |In the region of the nebula IC 434. V0607 Ori |In the region of the nebula IC 434. V0608 Ori |In the region of the nebula IC 434. V0610 Ori |In the region of the nebula IC 434. V0611 Ori |In the region of the nebula IC 434. V0612 Ori |VB, SE-comp.; NW-comp.=NSV 02555. In the region of the nebula IC V0612 Ori |434. V0614 Ori |In the region of T-association FU Ori. V0615 Ori |In the region of the nebula IC 434. V0616 Ori |In the region of the nebula IC 434. V0617 Ori |In the region of the nebula IC 434. V0618 Ori |In the region of the nebula IC 434. V0619 Ori |In the region of the nebula IC 434. V0620 Ori |In the region of the nebula IC 434. V0621 Ori |In the region of the nebula IC 434. V0622 Ori |In the region of the nebula IC 434. V0623 Ori |In the region of the nebula IC 434. V0625 Ori |In the region of T-association FU Ori. V0626 Ori |In the region of T-association FU Ori. V0627 Ori |In the region of T-association FU Ori. V0628 Ori |In the region of T-association FU Ori. V0629 Ori |In the region of T-association FU Ori. V0630 Ori |In the region of T-association FU Ori. V0631 Ori |In the region of T-association FU Ori. V0632 Ori |In the region of T-association FU Ori. V0634 Ori |In the region of T-association FU Ori. V0635 Ori |In the region of T-association FU Ori. V0636 Ori |In the region of T-association FU Ori. V0637 Ori |In the region of T-association FU Ori. V0638 Ori |In the region of T-association FU Ori. V0639 Ori |In the region of T-association FU Ori. V0640 Ori |d <= 0.02P. V0641 Ori |Min II 14.5. V0642 Ori |d = 0.05P?. V0643 Ori |P = 26.2075d? V0647 Ori |Min II 11.9. P var. Min I = 2418005.035 + 0.977575d*E (JD2414660 - V0647 Ori |23230); since JD2423230 - see Table. V0648 Ori |Min II 12.2. V0649 Ori |In the T-association CO - Ori. VB A (B 15m, 2", 0{deg}). V0650 Ori |In the region of the open cluster {lambda} Ori. V0652 Ori |In the region of the Orion nebula T-association. V0654 Ori |In the region of the Orion nebula T-association. V0655 Ori |In the region of the Orion nebula T-association. V0656 Ori |In the region of the Orion nebula T-association. V0657 Ori |In the region of the Orion nebula T-association. V0658 Ori |In the region of the Orion nebula T-association. V0659 Ori |In the region of the Orion nebula T-association. V0667 Ori |Min II 15.0. V0676 Ori |In the region of the Orion nebula T-association. V0677 Ori |In the region of the Orion nebula T-association. V0678 Ori |In the region of the Orion nebula T-association. V0679 Ori |In the region of the Orion nebula T-association. V0680 Ori |In the region of the Orion nebula T-association. V0681 Ori |In the region of the Orion nebula T-association. V0682 Ori |In the region of the Orion nebula T-association. V0683 Ori |In the region of the Orion nebula T-association. V0684 Ori |In the region of the Orion nebula T-association. V0685 Ori |In the region of the Orion nebula T-association. A(U) = 1.0m. V0686 Ori |In the region of the Orion nebula T-association. V0687 Ori |In the region of the Orion nebula T-association. V0688 Ori |In the region of the Orion nebula T-association. V0689 Ori |In the region of the Orion nebula T-association. V0690 Ori |In the region of the Orion nebula T-association. V0691 Ori |In the region of the Orion nebula T-association. V0692 Ori |In the region of the Orion nebula T-association. V0693 Ori |In the region of the Orion nebula T-association. V0694 Ori |In the region of the Orion nebula T-association. V0695 Ori |In the region of the Orion nebula T-association. V0696 Ori |In the region of the Orion nebula T-association. V0697 Ori |In the region of the Orion nebula T-association. V0698 Ori |In the region of the Orion nebula T-association. V0699 Ori |In the region of the Orion nebula T-association. V0700 Ori |In the region of the Orion nebula T-association. V0701 Ori |In the region of the Orion nebula T-association. V0702 Ori |In the region of the Orion nebula T-association. V0703 Ori |In the region of the Orion nebula T-association. V0704 Ori |In the region of the Orion nebula T-association. V0705 Ori |In the region of the Orion nebula T-association. V0706 Ori |In the region of the Orion nebula T-association. V0707 Ori |In the region of the Orion nebula T-association. V0708 Ori |In the region of the Orion nebula T-association. V0709 Ori |In the region of the Orion nebula T-association. V0710 Ori |In the region of the Orion nebula T-association. V0711 Ori |In the region of the Orion nebula T-association. V0712 Ori |In the region of the Orion nebula T-association. V0713 Ori |In the region of the Orion nebula T-association. A(U) = 4.0m. V0714 Ori |In the region of the Orion nebula T-association. V0715 Ori |In the region of the Orion nebula T-association. V0716 Ori |In the region of the Orion nebula T-association. V0717 Ori |In the region of the Orion nebula T-association. V0718 Ori |In the region of the Orion nebula T-association. Probably the V0718 Ori |sf-component of a very close pair. V0719 Ori |In the region of the Orion nebula T-association. V0720 Ori |In the region of the Orion nebula T-association. V0721 Ori |In the region of the Orion nebula T-association. V0722 Ori |In the region of the Orion nebula T-association. V0723 Ori |In the region of the Orion nebula T-association. V0724 Ori |In the region of the Orion nebula T-association. V0725 Ori |In the region of the Orion nebula T-association. V0726 Ori |In the region of the Orion nebula T-association. V0727 Ori |In the region of the Orion nebula T-association. V0728 Ori |In the region of the Orion nebula T-association. V0729 Ori |In the region of the Orion nebula T-association. V0730 Ori |In the region of the Orion nebula T-association. V0731 Ori |In the region of the Orion nebula T-association. V0732 Ori |In the region of the Orion nebula T-association. V0733 Ori |In the region of the Orion nebula T-association. V0734 Ori |In the region of the Orion nebula T-association. V0735 Ori |In the region of the Orion nebula T-association. V0736 Ori |In the region of the Orion nebula T-association. V0737 Ori |In the region of the Orion nebula T-association. A(U) > 2.4m. V0738 Ori |In the region of the Orion nebula T-association. V0739 Ori |In the region of the Orion nebula T-association. V0740 Ori |In the region of the Orion nebula T-association. A(pg) > 4.0m. V0741 Ori |In the region of the Orion nebula T-association. V0742 Ori |In the region of the Orion nebula T-association. V0744 Ori |In the region of the Orion nebula T-association. V0745 Ori |In the region of the Orion nebula T-association. V0746 Ori |In the region of the Orion nebula T-association. V0747 Ori |In the region of the Orion nebula T-association. V0748 Ori |In the region of the Orion nebula T-association. V0749 Ori |In the region of the Orion nebula T-association. V0750 Ori |In the region of the Orion nebula T-association. V0751 Ori |In the region of the Orion nebula T-association. V0752 Ori |In the region of the Orion nebula T-association. V0753 Ori |In the region of the Orion nebula T-association. V0754 Ori |In the region of the Orion nebula T-association. V0755 Ori |In the region of the Orion nebula T-association. V0756 Ori |In the region of the Orion nebula T-association. V0757 Ori |In the region of the Orion nebula T-association. V0758 Ori |In the region of the Orion nebula T-association. V0759 Ori |In the region of the Orion nebula T-association. V0760 Ori |In the region of the Orion nebula T-association. V0761 Ori |In the region of the Orion nebula T-association. V0762 Ori |In the region of the Orion nebula T-association. V0763 Ori |In the region of the Orion nebula T-association. V0764 Ori |In the region of the Orion nebula T-association. V0765 Ori |In the region of the Orion nebula T-association. V0766 Ori |In the region of the Orion nebula T-association. V0767 Ori |In the region of the Orion nebula T-association. A(U) = 1.5m. V0768 Ori |In the region of the Orion nebula T-association. V0770 Ori |In the region of the Orion nebula T-association. V0771 Ori |In the region of the Orion nebula T-association. V0772 Ori |In the region of the Orion nebula T-association. V0773 Ori |In the region of the Orion nebula T-association. V0774 Ori |In the region of the Orion nebula T-association. V0775 Ori |In the region of the Orion nebula T-association. V0776 Ori |In the region of the Orion nebula T-association. V0777 Ori |In the region of the Orion nebula T-association. V0778 Ori |In the region of the Orion nebula T-association. A(pg) = 1.6m. V0779 Ori |In the region of the Orion nebula T-association. V0780 Ori |In the region of the Orion nebula T-association. A(U) = 1.0m. V0781 Ori |In the region of the Orion nebula T-association. V0782 Ori |In the region of the Orion nebula T-association. V0783 Ori |In the region of the Orion nebula T-association. A(pg) = 3.0m. V0784 Ori |In the region of the Orion nebula T-association. V0785 Ori |In the region of the Orion nebula T-association. V0786 Ori |In the region of the Orion nebula T-association. V0787 Ori |In the region of the Orion nebula T-association. V0788 Ori |In the region of the Orion nebula T-association. V0789 Ori |In the region of the Orion nebula T-association. V0790 Ori |In the region of the Orion nebula T-association. V0791 Ori |In the region of the Orion nebula T-association. V0792 Ori |In the region of the Orion nebula T-association. V0793 Ori |In the region of the Orion nebula T-association. V0794 Ori |In the region of the Orion nebula T-association. V0795 Ori |In the region of the Orion nebula T-association. V0796 Ori |In the region of the Orion nebula T-association. V0797 Ori |In the region of the Orion nebula T-association. V0798 Ori |In the region of the Orion nebula T-association. V0799 Ori |In the region of the Orion nebula T-association. V0800 Ori |In the region of the Orion nebula T-association. V0801 Ori |In the region of the Orion nebula T-association. V0802 Ori |In the region of the Orion nebula T-association. V0803 Ori |In the region of the Orion nebula T-association. V0804 Ori |In the region of the Orion nebula T-association. V0805 Ori |In the region of the Orion nebula T-association. V0806 Ori |In the region of the Orion nebula T-association. V0807 Ori |In the region of the Orion nebula T-association. V0808 Ori |In the region of the Orion nebula T-association. V0810 Ori |In the region of the Orion nebula T-association. V0811 Ori |In the region of the Orion nebula T-association. V0812 Ori |In the region of the Orion nebula T-association. V0813 Ori |In the region of the Orion nebula T-association. V0814 Ori |In the region of the Orion nebula T-association. V0815 Ori |In the region of the Orion nebula T-association. V0816 Ori |In the region of the Orion nebula T-association. V0817 Ori |In the region of the Orion nebula T-association. V0818 Ori |In the region of the Orion nebula T-association. V0819 Ori |In the region of the Orion nebula T-association. V0820 Ori |In the region of the Orion nebula T-association. V0821 Ori |In the region of the Orion nebula T-association. V0822 Ori |In the region of the Orion nebula T-association. V0823 Ori |In the region of the Orion nebula T-association. V0824 Ori |In the region of the Orion nebula T-association. V0825 Ori |In the region of the Orion nebula T-association. V0826 Ori |In the region of the Orion nebula T-association. V0827 Ori |In the region of the Orion nebula T-association. V0828 Ori |In the region of the Orion nebula T-association. V0829 Ori |In the region of the Orion nebula T-association. V0830 Ori |In the region of the Orion nebula T-association. V0831 Ori |In the region of the Orion nebula T-association. V0832 Ori |In the region of the Orion nebula T-association. V0833 Ori |In the region of the Orion nebula T-association. V0834 Ori |In the region of the Orion nebula T-association. V0835 Ori |In the region of the Orion nebula T-association. V0836 Ori |In the region of the Orion nebula T-association. A(U) > 1.5m. V0837 Ori |In the region of the Orion nebula T-association. V0838 Ori |In the region of tbe Orion nebula T-association. V0839 Ori |In the region of tbe Orion nebula T-association. V0840 Ori |In the region of the Orion nebula T-association. A(pg) = 0.7m. V0841 Ori |In the region of the Orion nebula T-association. V0842 Ori |In the region of the Orion nebula T-association. V0843 Ori |In the region of the Orion nebula T-association. V0844 Ori |In the region of the Orion nebula T-association. V0845 Ori |In the region of the Orion nebula T-association. V0846 Ori |In the region of the Orion nebula T-association. V0847 Ori |In the region of the Orion nebula T-association. V0848 Ori |In the region of the Orion nebula T-association. V0849 Ori |In the region of the Orion nebula T-association. V0850 Ori |In the region of the Orion nebula T-association. V0851 Ori |In the region of the Orion nebula T-association. V0852 Ori |In the region of the Orion nebula T-association. V0853 Ori |In the region of the Orion nebula T-association. V0854 Ori |In the region of the Orion nebula T-association. V0855 Ori |In the region of the Orion nebula T-association. A(U) > 2.0m. V0856 Ori |In the region of the Orion nebula T-association. V0857 Ori |In the region of the Orion nebula T-association. A(pg) > 5.0m. V0858 Ori |In the region of the Orion nebula T-association. V0859 Ori |In the region of the Orion nebula T-association. V0860 Ori |In the region of the Orion nebula T-association. V0861 Ori |In the region of the Orion nebula T-association. V0862 Ori |In the region of the Orion nebula T-association. V0863 Ori |In the region of the Orion nebula T-association. V0864 Ori |In the region of the Orion nebula T-association. V0865 Ori |In the region of the Orion nebula T-association. V0866 Ori |In the region of the Orion nebula T-association. V0867 Ori |In the region of the Orion nebula T-association. A(pg)>3.0m. V0868 Ori |In the region of the Orion nebula T-association. V0869 Ori |In the region of the Orion nebula T-association. V0870 Ori |In the region of the Orion nebula T-association. V0871 Ori |In the region of the Orion nebula T-association. V0872 Ori |In the region of the Orion nebula T-association. V0873 Ori |In the region of the Orion nebula T-association. V0874 Ori |In the region of the Orion nebula T-association. V0875 Ori |In the region of the Orion nebula T-association. V0876 Ori |In the region of the Orion nebula T-association. Southem component V0876 Ori |of a close pair. V0877 Ori |In the region of the Orion nebula T-association. V0878 Ori |In the region of the Orion nebula T-association. V0879 Ori |In the region of the Orion nebula T-association. V0880 Ori |In the region of the Orion nebula T-association. V0881 Ori |In the region of the Orion nebula T-association. V0882 Ori |In the region of the Orion nebula T-association. V0883 Ori |In the region of the Orion nebula T-association. In the apex of a V0883 Ori |cometary nebula. V0884 Ori |In the region of the Orion nebula T-association. V0885 Ori |In the region of the Orion nebula T-association. V0886 Ori |In the region of the Orion nebula T-association. A(pg) > 3.5m. V0888 Ori |In the region of the Orion nebula T-association. V0889 Ori |In the region of the Orion nebula T-association. V0890 Ori |In the region of the Orion nebula T-association. V0891 Ori |In the region of the Orion nebula T-association. V0892 Ori |In the region of the Orion nebula T-association. Southern component V0892 Ori |of a pair (ro = 3"). V0893 Ori |In the region of the Orion nebula T-association. A(U) = 2.0m. V0894 Ori |In the region of the Orion nebula T-association. V0895 Ori |In the region of the Orion nebula T-association. V0896 Ori |In the region of the Orion nebula T-association. V0897 Ori |In the region of the Orion nebula T-association. V0898 Ori |In the region of the Orion nebula T-association. V0899 Ori |In the region of the Orion nebula T-association. V0900 Ori |In the region of the Orion nebula T-association. A(pg) > 2.5m. V0901 Ori |In the region of the nebula IC 434. V0902 Ori |In the region of the Orion nebula T-association. V0904 Ori |In the region of the Orion nebula T-association. V0905 Ori |In the region of the Orion nebula T-association. V0906 Ori |In the region of the Orion nebula T-association. V0907 Ori |In the region of the Orion nebula T-association. V0908 Ori |In the region of the Orion nebula T-association. V0909 Ori |In the region of the Orion nebula T-association. V0916 Ori |P = 0.28297d? Member of the open cluster NGC 2169. V0917 Ori |Member of the open cluster NGC 2169. V0918 Ori |In the region of the Orion nebula T-association. V0919 Ori |In the region of the Orion nebula T-association. V0920 Ori |In the region of the Orion nebula T-association. V0921 Ori |In the region of the Orion nebula T-association. V0922 Ori |In the region of the Orion nebula T-association. V0923 Ori |In the region of the Orion nebula T-association. V0924 Ori |In the region of the Orion nebula T-association. V0926 Ori |In the region of the Orion nebula T-association. V0927 Ori |In the region of the Orion nebula T-association. V0928 Ori |In the region of the Orion nebula T-association. V0929 Ori |In the region of the Orion nebula T-association. V0930 Ori |In the region of the Orion nebula T-association. V0931 Ori |In the region of the Orion nebula T-association. V0932 Ori |In the region of the Orion nebula T-association. V0933 Ori |In the region of the Orion nebula T-association. V0934 Ori |In the region of the Orion nebula T-association. V0935 Ori |In the region of the Orion nebula T-association. V0937 Ori |In the region of the Orion nebula T-association. V0938 Ori |In the region of the Orion nebula T-association. V0939 Ori |In the region of the Orion nebula T-association. V0941 Ori |In the region of the Orion nebula T-association. V0942 Ori |In the region of the Orion nebula T-association. V0943 Ori |In the region of the Orion nebula T-association. V0945 Ori |In the region of the Orion nebula T-association. V0946 Ori |In the region of the Orion nebula T-association. V0947 Ori |In the region of the Orion nebula T-association. V0948 Ori |In the region of the Orion nebula T-association. V0949 Ori |In the region of the Orion nebula T-association. V0950 Ori |In the region of the Orion nebula T-association. V0951 Ori |In the region of the Orion nebula T-association. V0952 Ori |In the region of the Orion nebula T-association. V0953 Ori |In the region of the nebula IC 434. V0956 Ori |In the region of the nebula IC 434. V0957 Ori |In the region of the nebula IC 434. V0958 Ori |In the region of the Orion nebula T-association. V0960 Ori |In the region of the nebula IC 434. V0961 Ori |In the region of the Orion nebula T-association. V0964 Ori |P var. Max = 2415800.389 + 0.5046772d*E (JD2415800 - 21010); Max = V0964 Ori |2424500.446 + 0.50466477d*E (JD2424500 - 30500); since JD2431500 - V0964 Ori |see Table. V0966 Ori |In the region of the Orion nebula T-association. V0967 Ori |In the region of the Orion nebula T-association. V0968 Ori |In the region of the Orion nebula T-association. V0969 Ori |In the region of the Orion nebula T-association. V0970 Ori |In the region of the Orion nebula T-association. V0971 Ori |In the region of the Orion nebula T-association. V0972 Ori |In the region of the Orion nebula T-association. V0973 Ori |In the region of the Orion nebula T-association. V0974 Ori |In the region of the Orion nebula T-association. V0975 Ori |In the region of the Orion nebula T-association. V0976 Ori |In the region of the Orion nebula T-association. V0977 Ori |In the region of the Orion nebula T-association. V0978 Ori |In the region of the Orion nebula T-association. V0979 Ori |In the region of the Orion nebula T-association. V0980 Ori |In the region of the Orion nebula T-association. V0981 Ori |In the region of the Orion nebula T-association. V0982 Ori |In the region of the Orion nebula T-association. V0983 Ori |In the region of the Orion nebula T-association. V0984 Ori |In the region of the Orion nebula T-association. V0985 Ori |In the region of the Orion nebula T-association. V0986 Ori |In the region of the Orion nebula T-association. V0987 Ori |In the region of the Orion nebula T-association. V0988 Ori |In the region of the Orion nebula T-association. V0989 Ori |In the region of the Orion nebula T-association. V0990 Ori |In the region of the Orion nebula T-association. V0991 Ori |In the region of the Orion nebula T-association. V0992 Ori |In the region of the Orion nebula T-association. V0994 Ori |In the region of the Orion nebula T-association. V0995 Ori |In the region of the Orion nebula T-association. V0996 Ori |In the region of the Orion nebula T-association. V0997 Ori |In the region of the Orion nebula T-association. V0998 Ori |{mu} = 0.28", ro = 221{deg}. V0999 Ori |In the region of the Orion nebula T-association. V1000 Ori |In the region of the Orion nebula T-association. V1001 Ori |In the region of the Orion nebula T-association. V1002 Ori |In the region of the Orion nebula T-association. V1003 Ori |{mu} = 0.272", ro = 60.8{deg}. V1004 Ori |VB A (B 10.57m, 37", 204{deg}); SB (P = 2.74d). V1005 Ori |The range of light variations (characteristic for BY Dra type V1005 Ori |variability) between the flares is given in the Table; the V1005 Ori |amplitude of the flares A(U) can reach 3.2m. V1006 Ori |In the region of the Orion nebula T-association. V1007 Ori |In the region of the Orion nebula T-association. V1016 Ori |In the region of the Orion nebula T-association. In the cluster NGC V1016 Ori |1976. Orion Trapezium member: teta1 Ori A (B = BM Ori, 8.7", V1016 Ori |32{deg}; C 5.13m, 13.1", 131{deg}; D 6.70m, 21.6", 96{deg}). d = V1016 Ori |0.001P. V1017 Ori |In the region of the Orion nebula T-association. V1018 Ori |In the region of the Orion nebula T-association. V1019 Ori |In the region of the Orion nebula T-association. V1020 Ori |In the region of the Orion nebula T-association. V1022 Ori |In the region of T-association FU Ori. V1028 Ori |P = 6d? V1029 Ori |In the region of the Orion nebula T-association. V1030 Ori |In the region of the nebula IC 434. (sig Ori) E (A 4.1m; B 5.1m, A V1030 Ori |= 0.247", P = 170yr; C 8.79m, 11.2", 238{deg}; D 6.66m, 12.9", V1030 Ori |84{deg}; E 41.6", 61{deg}). Min I (HeI) = 2442802.48 + 1.19080d*E. V1030 Ori |Unusual helium variable. Epoch of Min I brightness is given in the V1030 Ori |Table (Min II 6.71, Min II - Min I = 0.43P). This epoch is being V1030 Ori |observed by 0.18P later than the epoch of minimum strength of the V1030 Ori |HeI {lambda} 4026 A line. According to [09524], light minima are V1030 Ori |due to "eclipses" of the star surface by two isolated clouds V1030 Ori |(consisting of hydrogen and helium), which are located almost V1030 Ori |oppositely near the intersections of the magnetic And rotational V1030 Ori |equator. V1031 Ori |VB (0.159", 104{deg}, 1980.7). Min II 6.32; DII = 0.017P. V1034 Ori |Epoch of light minimum is given. V1035 Ori |In the region of the Orion nebula T-association. V1036 Ori |In the region of the Orion nebula T-association. V1037 Ori |In the region of the Orion nebula T-association. V1038 Ori |In the region of the Orion nebula T-association. V1039 Ori |In the region of the Orion nebula T-association. V1040 Ori |In the region of the Orion nebula T-association. V1041 Ori |In the region of the Orion nebula T-association. V1042 Ori |In the region of the Orion nebula T-association. V1043 Ori |In the region of the Orion nebula T-association. V1044 Ori |In the region of the Orion nebula T-association. V1045 Ori |In the region of the Orion nebula T-association. V1046 Ori |In the region of the Orion nebula T-association. SB 1. Min II 6.58. V1046 Ori |Possibly an ellipsoidal variable, its light variations being V1046 Ori |superimposed by light variations of the primary component of SX Ari V1046 Ori |type: Min (HeI) = 2442812.23 + 0.9015d*E [08054]. V1047 Ori |In the region of the Orion nebula T-association. V1048 Ori |In the region of the Orion nebula T-association. V1049 Ori |In the region of the Orion nebula T-association. V1050 Ori |In the region of the Orion nebula T-association. V1052 Ori |In the region of the Orion nebula T-association. V1053 Ori |In the region of the Orion nebula T-association. V1054 Ori |Epoch of light minimum is given. P = 8.596d?, P = 8.674d? V1055 Ori |P(X) = 5.2d [09528]. V1056 Ori |VB A (B 9.8m, 28.7", 58{deg}). V1058 Ori |In the region of the Orion nebula T-association. V1059 Ori |In the region of the Orion nebula T-association. V1060 Ori |In the region of the Orion nebula T-association. V1061 Ori |In the region of the Orion nebula T-association. V1062 Ori |In the region of the Orion nebula T-association. V1063 Ori |In the region of the Orion nebula T-association. V1064 Ori |In the region of the Orion nebula T-association. V1065 Ori |In the region of the Orion nebula T-association. V1066 Ori |In the region of the Orion nebula T-association. V1067 Ori |In the region of the Orion nebula T-association. V1068 Ori |In the region of the Orion nebula T-association. V1069 Ori |In the region of the Orion nebula T-association. V1070 Ori |In the region of the Orion nebula T-association. V1071 Ori |In the region of the Orion nebula T-association. V1072 Ori |In the region of the Orion nebula T-association. V1073 Ori |In the region of the Orion nebula T-association. V1074 Ori |In the region of the Orion nebula T-association. V1075 Ori |In the region of the Orion nebula T-association. V1076 Ori |In the region of the Orion nebula T-association. V1077 Ori |In the region of the Orion nebula T-association. V1078 Ori |In the region of the Orion nebula T-association. V1079 Ori |In the region of the Orion nebula T-association. V1080 Ori |In the region of the Orion nebula T-association. V1081 Ori |In the region of the Orion nebula T-association. V1082 Ori |In the region of the Orion nebula T-association. V1083 Ori |In the region of the Orion nebula T-association. V1084 Ori |In the region of the Orion nebula T-association. V1377 Ori |SB?, Porb ~ 5.5 to 6.5d. V1380 Ori |In a bright nebula. V1647 Ori |The nebula brightened to 14.0, the central star's magnitude is V1647 Ori |given. V1650 Ori |The magnitude in Min light is from [78130]. V1804 Ori |VB (A 7.7m; B 7.9m, 5", 5{deg}, 1991). V1811 Ori |A twice shorter period is not excluded. V1814 Ori |SB2, Porb = 19.48136d. V1818 Ori |In the head of the nebula GN 05.51.4. V1820 Ori |Blazhko effect, P(Bl) = 28d [79169]. V1833 Ori |Min II = 10.53. Changing O'Connell effect. V1834 Ori |Min II = 6.87. VB AB (A 7.0m; B 9.1m, 1".8, 340{deg}, 2007). V1840 Ori |VB A (B 13.1m, 13", 211{deg}, 2001). V1847 Ori |Amplitude(Min II)= 0.24mag. V1848 Ori |Min II = 11.65. V1851 Ori |Min II = 13.05 :. V1853 Ori |Min II = 12.20 :. V1859 Ori |SB2, Porb = 5.935d. V1865 Ori |Min II = 12.8. V1871 Ori |Min II = 12.9. V1872 Ori |SB2, Porb = 7.672d. V1878 Ori |SB2, Porb = 40.57d. V1882 Ori |SB2, Porb = 46.85d. V1883 Ori |VB B (A = NEXT GCVS NAME; AB 9", 262{deg}, 2000). V1884 Ori |VB A (B = PREVIOUS GCVS NAME, 9", 262{deg}, 2000). V1885 Ori |VB AB (1"). V1928 Ori |VB B (A 9.05m; AB 7", 163{deg}, 2001). V1931 Ori |VB A (B 13.51m, 8", 359{deg}, 2001). V1934 Ori |VB B (A = IM Ori, 12.67m; AB 6", 337{deg}, 2001). V1935 Ori |VB A (B 13.88m, 6", 71{deg}, 2001). V1952 Ori |VB B (A 10.4m; AB 12", 32{deg}, 2001). V1953 Ori |The amplitude of out-of-flare variations is 0.04m. V1994 Ori |VB B (A = V1000 Ori, 11.70m; AB 6", 194{deg}, 2001). V1995 Ori |VB B (A 9.59mJ; B 13.98mJ, 24", 31{deg}, 2001; C 14.25mJ, BC 7", V1995 Ori |214{deg}, 2001; also other components). V1999 Ori |Amplitude(Min II)= 0.3mag. V2008 Ori |VB A (B = V1694 Ori, 12.31mJ, 8", 191{deg}, 2001). V2014 Ori |VB AB (7.7mV, 8.2mV, 1".7, 282{deg}, 2006). V2024 Ori |VB B (A 13.13m; AB 6", 305{deg}, 2001). V2027 Ori |VB A (B 13.87m, 5", 342{deg}, 2001). V2030 Ori |VB A (B 16.0m, 5", 133{deg}, 2001). V2038 Ori |VB B (A = KK Ori, 11.26m; AB 5", 89{deg}, 2001). V2039 Ori |VB A (B 13.11m, 11", 322{deg}, 2001). V2084 Ori |VB B (A = NSV 02252, 8.61m; AB 11", 130{deg}, 2001). V2085 Ori |VB A (B 12.84m, 10", 36{deg}). V2086 Ori |VB B (A = V1474 Ori, 13.30m; AB 19", 291 {deg}, 2001; C 15.78m; BC V2086 Ori |6", 117{deg}, 2001). V2088 Ori |VB C (A = V1316 Ori, 12.74m, B 14.40m; AB 8", 353{deg}, AC 13", V2088 Ori |15{deg}, 2001). V2090 Ori |VB B (A = V1317 Ori, 14.04m; AB 7", 141{deg}, 2001). V2094 Ori |VB A (B 13.20m, 6", 279{deg}, 2001). V2099 Ori |Multiple (V1318 Ori 12.75m, 13", 312{deg}, 2001 and other V2099 Ori |companions). V2102 Ori |VB B (A = KS Ori, 9.51m; AB 5", 69{deg}, 2001). V2107 Ori |VB A (B = KR Ori, 10.23m; AB 15", 99{deg}, 2001). V2109 Ori |VB A (B 12.87m, 5", 353{deg}, 2001). V2110 Ori |VB B (A = V1479 Ori, 12.49m; AB 9", 346{deg}, 2001). V2113 Ori |VB B (A = NSV 16386, 13.34m; AB 8", 127{deg}, 2001). V2114 Ori |VB B (A = V1319 Ori, 10.91m; AB 6", 270{deg}, 2001). V2118 Ori |VB B (A 11.54m; AB 11", 218{deg}, 2001). V2120 Ori |VB B (A 12.70m; AB 18", 294{deg}, 2001; C 13.14m; BC 12", 185{deg}, V2120 Ori |2001; D 13.54m; BD 11", 277{deg}, 2001). V2121 Ori |VB A (B 13.69m, 5", 309 {deg}, 2001). V2133 Ori |VB B (A 8.74m, 20", 346{deg}, 2001). V2136 Ori |Type E is not excluded. V2139 Ori |VB A (B 14.13m, 8", 150{deg}, 2001). V2141 Ori |VB A (B 11.64:m, 6", 252{deg}, 2001). V2142 Ori |VB B (A 12.72m, 7", 11{deg}, 2001). V2143 Ori |VB A (B = V1482 Ori, 12.08m, 10", 274{deg}, 2001; C = V1322 Ori, V2143 Ori |12.11m, 13", 320{deg}, 2001; D = V1323 Ori, 12.26m, 15", 352{deg}, V2143 Ori |2001). V2150 Ori |VB B (A = V480 Ori, 11.38m, AB 10", 326{deg}, 2001; C = GCVS NAME V2150 Ori |FROM NEXT REMARK, 13.18m, AC 6", 306{deg}, 2001). V2152 Ori |VB C (A = V480 Ori, 11.38m, B = GCVS NAME FROM PREVIOUS REMARK; AB V2152 Ori |10", 326{deg}, AC 6", 306{deg}, 2001). V2164 Ori |VB B (A 11.53m, K5; AB 10", 189{deg}, 2001; C 13.44m, M3.5e, AC 5", V2164 Ori |153{deg}, 2001; other components). V2167 Ori |VB A (B 16.35m, 8", 83{deg}, 2001). V2175 Ori |VB A (B = NSV 16405, 13.31m, 9", 106{deg}, 2001). V2177 Ori |VB B (A = REMARK AFTER NEXT, 12.96m; AB 4", 238{deg}, 2001). V2178 Ori |VB A (B 15.25m, 8", 111{deg}, 2001). V2179 Ori |VB A (B = REMARK BEFORE PREVIOUS, 14.72m, 4" 238{deg}, 2001). V2181 Ori |VB B (A 12.69m; AB 7", 330{deg}, 2001). V2183 Ori |VB B (A 13.36m; AB 8", 111{deg}, 2001). V2185 Ori |VB A (B 12.84m, 7", 330{deg}, 2001). V2189 Ori |VB B (A 14.43m; AB 6", 297{deg}, 2001). V2191 Ori |VB C (A = LR Ori, 9.70m, B 12.92m; AB 10", 160{deg}, AC 14", 248 V2191 Ori |{deg}, 2001; other components). V2192 Ori |VB B (A 12.88m; AB 6", 317{deg}, 2001). V2194 Ori |VB A (B 16.48m, 7", 163{deg}, 2001). V2198 Ori |VB B (A 12.04m; AB 5", 65{deg}, 2001). V2205 Ori |VB A (B 16.07m, 7", 108{deg}, 2001). V2212 Ori |Amplitude(Min II)= 0.1mag. V2213 Ori |Multiple (V1487 Ori 9.42m, 13". 233{deg}, 2001; other components, V2213 Ori |including NSV 16420). V2214 Ori |VB A (B 13.55m, 11", 118{deg}, 118{deg}). V2215 Ori |VB B (A 12.32m; AB 9", 272{deg}, 2001; other components). V2216 Ori |VB A (B 15.54m, 11", 353{deg}, 2001). V2217 Ori |Multiple (LU Ori 8.74mKs, 9", 182{deg}, 2001; other components). V2218 Ori |VB B (A = LU Ori, 9.98mJ; AB 7", 158{deg}, 2001). V2220 Ori |VB A (B 3" s). V2222 Ori |VB B (A 12.11m; AB 7", 149{deg}, 2001). V2225 Ori |Multiple (NSV 16423 14" np; other components). V2228 Ori |Multiple (NSV 16426 13.58m, 9", 356{deg}, 2001; GCVS NAME FOR NSV V2228 Ori |16429 12.37m, 11", 147{deg}, 2001; other components). V2232 Ori |VB A (B 13.64:m, 8", 40{deg}, 2001; other components). V2233 Ori |VB B (A = GCVS NAME FOR No. 8384; AB 5", 276{deg}, 2001). V2236 Ori |Multiple. V2237 Ori |VB A (B 12.80m, 6", 123{deg}, 2001). V2239 Ori |VB A (B = V1491 Ori, 11.29m, 16", 229{deg}, 2001). V2241 Ori |Multiple. V2242 Ori |VB C (A = GCVS NAME FOR NSV 16438, 12.80m, B = GCVS NAME FOR NSV V2242 Ori |16437, 13.37m; AB 13", 191{deg}, AC 9", 208{deg}, 2001). V2243 Ori |VB A (B = GCVS NAME FOR No. 8355, 5", 276{deg}, 2001). V2245 Ori |VB B (A = GCVS NAME FOR NSV 16438, 12.80m; AB 13", 191{deg}, 20001; V2245 Ori |C = GCVS NAME FOR No. 8381, AC 9", 208{deg}, 2001). V2246 Ori |VB A (B 13.24m, 12", 235{deg}, 2001). V2247 Ori |VB A (B = GCVS NAME FOR NSV 16437, 13.37m, 13", 191{deg}, 2001; C = V2247 Ori |GCVS NAME FOR No. 8381, AC 9", 208{deg}, 2001). V2248 Ori |VB A (B = NSV 16441, 8.16:m, 17", 150{deg}, 2001; C = V1496 Ori, V2248 Ori |8.78m, 7", 180{deg}, 2001). V2251 Ori |VB C (A 13.52m, B 14.96m; AB 6", 229{deg}, AC 5", 23{deg}, 2001). V2252 Ori |VB B (A = NSV 16435, 11.05m; AB 7", 66{deg}, 2001). V2254 Ori |Multiple. V2255 Ori |Multiple (GCVS NAME FOR NSV 16443 11", 122{deg}, 2001; other V2255 Ori |components). V2256 Ori |VB B (A = V1495 Ori, 12.24m; AB 9", 71{deg}, 2001). V2257 Ori |VB C (A 11.05m, B 11.44m; AB 7", 66{deg}, AC 13", 137{deg}, 2001). V2261 Ori |VB A (B = GCVS NAME FOR NEXT REMARK, 6", 17{deg}, 2001). V2263 Ori |VB B (A = GCVS NAME FOR PREVIOUS REMARK; AB 6", 17{deg}, 2001). V2266 Ori |Multiple (GCVS NAME FOR No. 8478 11", 302 {deg}, 2001; other V2266 Ori |components). V2270 Ori |Multiple (NSV 16454 10.96m, 10", 65{deg}, 2001; other components). V2271 Ori |VB (B = JW 474, 2.4", 24{deg}, 1961). V2272 Ori |VB A (B 13.63m, 12", 331{deg}, 2001). V2276 Ori |VB B (A 14.49m; AB 7", 173{deg}, 2001). V2279 Ori |VB A (B = AC Ori 3" s). V2280 Ori |VB A (B 12.57m, 5", 215{deg}, 2001). V2283 Ori |VB B (A 13.00m; AB 9", 259{deg}, 2001). V2284 Ori |Multiple. V2288 Ori |Multiple. V2291 Ori |VB A (B 13.47m, 7", 18{deg}, 2001). V2292 Ori |Multiple (NSV 16466 12.56m, 12", 68:{deg}). V2294 Ori |VB B (A 12.44m, 10", 59{deg}, 2001). V2297 Ori |NSV 16469 9" nf. V2299 Ori |VB A (B 4" s). V2300 Ori |VB B (A = V1812 Ori, 10.60m; AB 9", 244{deg}, 2001). V2301 Ori |VB C (A 8.76m, B = LZ Ori, 9.30m; AB 14", 220{deg}, AC 25", V2301 Ori |226{deg}, 2001). V2304 Ori |Multiple. V2309 Ori |VB B (A 13.63m; AB 5", 300{deg}, 2001). V2314 Ori |VB A (B 12.32m, 5", 16{deg}, 2001). V2317 Ori |VB A (B 15.50m, 5", 300{deg}, 2001). V2318 Ori |VB A (B 14.04m, 10", 69{deg}, 2001). V2321 Ori |VB (2"). Multiple (V1336 Ori 5", 133{deg}, 1961; NSV 16467 10.10m, V2321 Ori |10", 286{deg}, 2001; other components). V2325 Ori |Multiple. V2326 Ori |VB B (A 10.91m; AB 12", 115{deg}, 2001). V2330 Ori |VB B (A 10.15m; AB 10", 69{deg}, 2001). V2333 Ori |Multiple. V2336 Ori |Multiple. V2338 Ori |Multiple. V2343 Ori |VB A (B = NSV 16486, 13.43:m, 9", 68{deg}, 2001). V2346 Ori |VB B (A = GCVS NAME FOR NSV 16495; AB 10", 275{deg}, 2001). V2350 Ori |V1516 Ori 11"nf. V2352 Ori |VB B (A 13.65m; AB 6", 127{deg}, 2001). V2353 Ori |Multiple. V2354 Ori |VB A (B 6" sf). V2355 Ori |VB B (A = GCVS NAME FOR NSV 2307; AB 13", 214{deg}, 2001; NSV 16490 V2355 Ori |close to A). V2359 Ori |VB (0.8"). V2360 Ori |VB A (B = GCVS NAME FOR No. 9248, 10", 275{deg}, 2001; C 14.71m, V2360 Ori |14", 240{deg}, 2001). V2362 Ori |VB A (B 13.54m, 7", 83{deg}, 2001). V2363 Ori |VB A (B = V1521 Ori; AB 7", 264{deg}, 2001). V2364 Ori |VB A (B = GCVS NAME FOR No. 9305, 13", 214{deg}, 2001; NSV 16490 3" V2364 Ori |n). V2366 Ori |VB B (A 12.01m; AB 11", 6{deg}, 2001). V2372 Ori |VB A (B 10.98m, 8", 1{deg}, 2001). V2373 Ori |VB B (A = V1521 Ori; AB 6", 90{deg}, 2001). V2374 Ori |VB AB (0.7"). Multiple (NSV 16503 11.42mJ, 6", 330{deg}, 2001; V2374 Ori |other components). V2377 Ori |VB B (A = NSV 16506, 13.64m; AB 4", 40{deg}, 1991). V2378 Ori |VB B (A = AG Ori; AB 12", 185{deg}, 2001). V2383 Ori |Multiple (V1524 Ori 9", 225{deg}, 2001; other components). V2384 Ori |Min II = 14.81. MinII - MinI = 0.67P. V2387 Ori |VB B (A 13.80m; AB 7", 78{deg}, 2001). V2389 Ori |VB A (B 6" sf). V2401 Ori |VB B (A 13.05m; AB 5", 321{deg}, 2001). V2404 Ori |VB B (A = V561 Ori, 11.78m; AB 9", 250{deg}, 2001). V2405 Ori |VB A (B 14.81m, 5", 285{deg}, 2001). V2410 Ori |VB B (A = V1531 Ori; AB 7", 163{deg}, 2001). V2413 Ori |VB A (B 3" f). V2414 Ori |VB B (A = V1017 Ori; AB 10", 283{deg}, 2001). V2415 Ori |VB B (A = NSV 16523 8" sp). V2417 Ori |VB AB (1"). V2423 Ori |VB A (B = V1400 Ori, 6", 43{deg}, 2001). V2425 Ori |Multiple (NSV 16535 12" nf; other components). V2435 Ori |VB A (B 15.3m, 6", 138{deg}, 2001). V2442 Ori |VB C (A 11.63m, B 11.70m; AB 3", 257{deg}, AC 10", 349{deg}, 2001). V2444 Ori |VB A (B = GCVS NAME FOR NSV 16541, 6", 144{deg}, 2001). V2448 Ori |VB B (A = GCVS NAME FROM PREVIOUS REMARK; AB 6", 144{deg}, 2001). V2449 Ori |VB (AK Ori 9" s). V2451 Ori |VB B (A 2.9mV, C = NSV 2342, 9.7mV; AB 11", 141{deg}, AC 49", V2451 Ori |103{deg}, 2002). V2454 Ori |VB A (B 10" np). V2458 Ori |VB C (A = GCVS NAME FOR NEXT REMARK, B 11.34m; AB 9", 286{deg}, AC V2458 Ori |6", 349{deg}, 2001). V2460 Ori |VB A (B 11.34m, C = GCVS NAME FOR PREVIOUS REMARK; AB 9", 286{deg}, V2460 Ori |AC 6", 349{deg}, 2001). V2464 Ori |VB B (A 11.29m; AB 11", 14{deg}, 2001). V2467 Ori |VB B (A = NSV 02331, 11.77m, C 13.91:m; AB 7", 20{deg}, AC 11", V2467 Ori |13{deg}, 2001). V2476 Ori |VB A (B 13.70m, 11", 230{deg}, 2001). V2479 Ori |VB B (A = V1549 Ori, AB 6", 117{deg}, 2001). V2481 Ori |VB A (B 15.02m, 6", 13{deg}, C 16.39m, 10", 139{deg}, 2001). V2483 Ori |VB A (B 14.76m, 9", 19{deg}, 2001). V2484 Ori |VB A (B 12.38m, 7", 2{deg}, 2001). V2491 Ori |VB A (B 13.12m, 6", 37{deg}, 2001). V2492 Ori |VB B (A = GCVS NAME FOR NEXT REMARK; AB 8", 344{deg}, 2001). V2494 Ori |VB A (B = GCVS NAME FOR PREVIOUS REMARK, 8", 344{deg}, 2001). V2495 Ori |VB B (A = GCVS NAME FOR NSV 2341; AB 11", 342{deg}, 1961; also V2495 Ori |fainter components). V2497 Ori |VB B (A = NSV 2340, 11.23m, C 13.82m; AB 8", 160{deg}, AC 7", V2497 Ori |258{deg}, 2001). V2499 Ori |VB A (B = GCVS NAME FOR No. 10729, 11", 342{deg}, 1961; also V2499 Ori |fainter components). V2500 Ori |VB A (B 8" n). V2509 Ori |NU Ori 20" np. VB A (B 12.36m, 8", 147{deg}, 2001). V2514 Ori |VB B (A = V565 Ori, 10.17m; AB 9", 7{deg}, 2001). V2516 Ori |The periodic variations were reported for the bright state (above V2516 Ori |14m J). V2521 Ori |VB B (A = V359 Ori, C 11.28; AB 10", 290{deg}; AC 14", 306{deg}, V2521 Ori |2001). V2537 Ori |VB A (B 14.35m, 7", 215{deg}, 2001). V2543 Ori |VB B (A = AM Ori, AB 4", 330{deg}, 2001). V2568 Ori |VB A (B 13.86m, 11", 168{deg}, 2001). V2575 Ori |VB B (A 7.98m; AB 15", 232{deg}, 2001). V2592 Ori |Min II = 8.20. MinII - MinI = 0.40P. V2602 Ori |VB A (B 13.65m, 11", 63{deg}, 2001). V2603 Ori |VB A (B 14.98m, 7", 282{deg}, 2001). V2608 Ori |VB A (B 13.70m, 7", 350{deg}, 2001). V2615 Ori |VB B (A = OV Ori, 11.51m; AB 7", 287{deg}, 2001). V2620 Ori |VB B (A 10.34m; AB 12", 170{deg}, 2001). V2630 Ori |VB A (B 15.27m, 8", 310{deg}, C 15.84m, 8", 144{deg}, 2001). V2651 Ori |VB B (A = NSV 2412, 11.48:m; AB 9", 219{deg}, 2001). V2655 Ori |VB B (A 12.56m; AB 10", 48{deg}, 2001). V2677 Ori |VB A (B 13.80m, 10", 152{deg}, 2001). V2678 Ori |Multiple. V2679 Ori |VB B (A = NSV 2424, 11.01m; AB 14", 46{deg}, 2001). V2689 Ori |Type from [80034]. V2712 Ori |Min II = 12.7. V2729 Ori |VB C (A 12.57m, B 16.17m; AB 16", 117{deg}, AC 18", 132{deg}, V2729 Ori |1999). V2735 Ori |Min II = 9.43. V2743 Ori |Min II = 13.9. V2749 Ori |SB2, Porb = 18.74d. V2751 Ori |SB1. V2752 Ori |Type from [80034]. V2757 Ori |Min II = 10.12. V2758 Ori |SB2, Porb = 4.99d. V2759 Ori |Min II = 10.62. V2762 Ori |Min II = 10.31. V2766 Ori |Amplitude(Min II)= 0.7mag. V2767 Ori |Min II = 13.2 :. V2768 Ori |Amplitude(Min II)= 0.4mag. V2769 Ori |Amplitude(Min II)= 0.4mag:. V2772 Ori |Min II = 12.35. V2776 Ori |VB A (B 16.9m R, 6", 31{deg}, 1999). V2777 Ori |VB A (B 16.0m R, 9", 88{deg}, 1999). V2778 Ori |Min II = 10.50:. MinII - MinI = 0.44P. V2780 Ori |Min II = 12.12. VB A (B 5", 139{deg}, 1999). V2783 Ori |Min II = 10.63. VB A (B 12.9m, 7", 25{deg}, 1999). V2784 Ori |Min II = 13.7. V2787 Ori |Min II = 10.28. V2788 Ori |Min II = 10.82:. V2789 Ori |Min II = 11.4. V2790 Ori |Min II = 11.64. V2793 Ori |Min II = 13.6. V2797 Ori |Multiperiodic. V2834 Ori |P1 is presented in the Table. P0 = 0.488575d; P1/P0 = 0.7428. V2846 Ori |According to [82044], a flare to 15.7mpg from 17.4 mpg was observed V2846 Ori |on 1996 November 17. V2853 Ori |P1 is presented in the Table. P2 = 0.2653979d; P2/P1 = 0.7990. V2855 Ori |Double-mode pulsator, P2 = 0.0448278d. VB A (B 5", 99{deg}, 1999). V2856 Ori |MinII - MinI = 0.52P. alf Ori |VB A (B 14.5m, 39.8", 110{deg}). Min = 2410600 + 2070d*E (1840 - alf Ori |1929) [01012]. Since 1929 - see Table. The main variation is alf Ori |superimposed by the waves with P = 200 - 400d. Dust-gaseous shell alf Ori |(r = 50") [09529]. del Ori |VB A (A 0.217", 144{deg}, 1980; B 14.0m, 33.1", 227{deg}; C 6.84m, del Ori |53.5", 359{deg}). Orion Belt cluster member. Min II 2.20. Apsidal del Ori |motion (P = 210 yr). Shape of the light curve varies. The intrinsic del Ori |brightness variability of the components is possible. eps Ori |Orion Belt cluster member. eta Ori |VB Aab (AC 0.037", 111{deg}, 1979.0, P = 9.219 yr [09535]; B 4.8m, eta Ori |1.60", 76{deg}, 1976.0; C 9.4m, 115", 51{deg}). EA/DM. Min II 3.57. eta Ori |The range of combined light variation of the components AAb (SB 2, eta Ori |P = 7.989268d), AC, and B is given in the Table. Outside eclipses eta Ori |there are sinusoidal light variations of the system with A(V) = eta Ori |0.05m due to pulsations of the component Ab [09535] with P = eta Ori |0.30197d [09536] or 0.30145d [09537]. According to [08566] these eta Ori |variations were not observed between 1970 and 1976. pi. 5 Ori |Min II 3.73. The period is improved using radial velocities pi. 5 Ori |[04627]. psi Ori |VB A (B 11.1m, 2.7", 323{deg}; C 13.88m, 83", 196{deg}). Min II psi Ori |4.58. The period is determined on the base of radial velocities psi Ori |[09541]. R Pav |Pvar. Max = 2411219 + 228.34d (JD2411000 - 18500); Max = 2418527 + R Pav |230.95d*E (JD2418500 - 30000); since JD2430000 - see Table. S Pav |P var. Max = 2421479 + 389.64d*E(JD2421000 - 31000); since S Pav |JD2431000 - see Table. {Delta}(m) var strongly. Min II is sometimes S Pav |observed after Max I. T Pav |P var. Max = 2413328 + 243.45d*E(JD2405700 - 25500); Max = 2425499 T Pav |+ 245.11d*E(JD2425500 - 32500); since JD2432500 - see Table. V Pav |VBA (B 14.0m vis, 15", 327{deg}). Mean brightness var, P2 = 3735d, V Pav |9.7m - 10.7m. W Pav |P var. Before JD2431000 Max = 2413778 + 282.92d*E; since JD2431000 W Pav |- see Table. RT Pav |Mean light var, 10.4m - 11.1m 1649, P2 = 757d. SU Pav |P var. Max = 2430036 + 245.18d*E (JD2411000 - 30100) [00001]; SU Pav |during JD247700 - 40000 - see Table. TW Pav |Before JD2420400 Max = 2417760 + 397.d*E. YY Pav |{Delta}(m) var strongly. P possibly is twice longer, in that case YY Pav |Min II 14.4. AR Pav |Depth of eclipses {Delta}(m) = 2m B, d = 0.05P. Expanding shell. BD Pav |Only one outburst was observed [00629]. Brightness flickering. BD Pav |Eclipses according to the elements Min I = 2444412.676 + BD Pav |0.1793015d*E, {Delta}(m) ~0.5m [09191]. Outside outburst, 15.40m - BD Pav |16.21m. BF Pav |Min II 11.9. BI Pav |Min II ({Delta}(m) ~0.05m) is possible. DF Pav |Epoch of min is given. Light curve shape strongly var. DN Pav |{Delta}(S) = 8:. DW Pav |Min II 16.3. EG Pav |Twice shorter P is possible [00001]. EL Pav |Min II 15.5. EN Pav |Elements need confirmation. EQ Pav |Red. FY Pav |Min II? JD2436784.37. HL Pav |Blazhko effect? HP Pav |Min II 15.5. HQ Pav |Min II 12.7. HY Pav |Min II 12.1. IL Pav |RRC type is possible. KR Pav |Min II 14.1. KZ Pav |VB A (B 8.7m, 6.7", 119{deg}, 1971; C 9.2m, BC 1.0", 329{deg}, KZ Pav |1971). P var. Min = 2430448.617 + 0.949880d*E (JD2416000 - 30000) KZ Pav |[00001]; since JD2430000 - see Table. Min II is present. LL Pav |Min II 15.1. LO Pav |Min II 16.5. LR Pav |Min II 15.3. LT Pav |Min II 12.2. LV Pav |Min II 14.3. LY Pav |Min II 14.9. MQ Pav |Epoch of Min is given. EW/KW type with twice longer P is possible. MR Pav |Possible elements Max = 2436731.40 + 0.3737d*E [00001]. MS Pav |Min II 14.1. MW Pav |d = 0.08P. Min II 8.92, dII = 0.11P. NP Pav |Deep Min II. NW Pav |[A/H] = -0.7. OY Pav |The chart in [06286] is wrong. V0382 Pav |Type EW: is also possible. V0399 Pav |Symbiotic spectrum. V0400 Pav |MinII 9.23. V0413 Pav |P varies, dP/dt =+1.29 x 10^(-5) d/yr. V0416 Pav |P0 is tabulated, P1 = 0.36574d. V0430 Pav |Type EW with P=0.444342d is not excluded. V0449 Pav |Blazhko effect, P = 61.3d. V0471 Pav |P = 68.6d is superposed. V0472 Pav |P = 43d is superposed. V0475 Pav |VB B (AB 7", 287{deg}, 2000). V0483 Pav |VB (15.22mG, 16.08mG, 3", 137{deg}, 2000); the range in the Table V0483 Pav |is for combined brightness. V0484 Pav |Possible secondary period 48d. V0491 Pav |P = 59.7d is superposed. V0494 Pav |Blazhko effect. V0500 Pav |P varies. V0537 Pav |Blazhko effect? V0538 Pav |Long period: P = 675d. V0541 Pav |Pulsation period P = 48.4d. V0546 Pav |VB A (14.45mG; B 14.5mG, 16", 286{deg}, 2000). V0551 Pav |VB A (15.0mG; B 15.1mG, 11", 210{deg}, 2000). kap Pav |P var. Max = 2419619.38 + 9.0898d*E (JD2411930 - 22550); Max = kap Pav |2425987.12 + 9.1028d*E (JD2422550 - 26980); Max = 2430530.67 + kap Pav |9.0833d*E (JD2426980 - 31345); Max = 2433239.87 + 9.0956d*E kap Pav |(JD2431345 - 34045); Max = 2434693.11 + 9.0653d*E (JD2434045 - kap Pav |37000); since JD2440000 - see Table. [Fe/H] = 0.0/ - 0.4. kap Pav |Moderately high Z coordinate (IZI ~240 pc provided the period - kap Pav |luminosity relation for DCEP stars is valid), low radial velocity. kap Pav |The period is not typical for CW stars. Ca II emission was noticed kap Pav |in the spectrum. lam Pav |VB A (B 12.4m, 63.1", 206{deg}). rho Pav |The main light variation P1 (see Table) with a semiamplitude rho Pav |{delta}(y) = 0.0069m is superposed by oscillations with P2 = rho Pav |0.1131d ({delta}(y) = 0.0031m), P3 = 0.1612d ({delta}(y) = rho Pav |0.0029m). R Peg |OH, H2O, SiO maser. P var. Max = 2396327 + 381.9d*E (JD2396300 - R Peg |2408200); Max = 2413012 + 371.4d*E (JD2413000 - 19800); Max = R Peg |2420092 + 379.77d*E (JD2420000 - 31100) [00960]; since JD2431100 - R Peg |see Table. T Peg |P var. Max = 2398452 + 371.0d*E (JD2398400 - 2408900); Max = T Peg |2413697 + 386.8d*E (JD2413600 - 18700); Max = 2421016 + 362.5d*E T Peg |(JD2420900 - 28000) [00960]; Max = 2434343 + 376.0d*E (JD2428300 - T Peg |34300); Max = 2440984 + 368.7d*E (JD2434300 - 41000); since T Peg |JD2441000 - see Table. U Peg |Min II 9.73. P var. There is a square term in the elements: U Peg |-2.468D*10**(-11)*E**2. 0 - C = 0.00323d*sin((2{pi}/16330)E + U Peg |0.418{pi}). Shape of the light curve varies. W Peg |SiO maser. P var. Max = 2413819 + 343.2d*E (JD2413800 - 26600); Max W Peg |= 2427162 + 345.5d*E (JD2426600 - 32100) [00960]; Max = 2439690 + W Peg |348.75d*E (JD2432300 - 39700) [00001]; since JD2441400 - see Table. X Peg |P var. Max = 2414713 + 200.3d*E (JD2414700 - 21300); Max = 2420105 X Peg |+ 204.3d*E (JD2420100 - 23800); Max = 2423570 + 199.8d*E (JD2423600 X Peg |- 31000) [00960]; Max = 2432006 + 208d*E (JD2431000 - 32100); Max = X Peg |2434206 + 200.0d*E (JD2432100 - 39300); since JD2438400 - see X Peg |Table. Z Peg |P var. Max = 2415433 + 318.9d*E (JD2398800 - 2420550); Max = Z Peg |2420207 + 328.0d*E (JD2420200 - 32000) [00960]; Max = 2432005 + Z Peg |325.8d*E (JD2432000 - 37900); Max = 2437870 + 319d*E (JD2437500 - Z Peg |40100); Max = 2442086 + 328.0d*E (JD2440100 - 43100); since Z Peg |JD2442100 - see Table. RR Peg |P var. Max = 2417582 + 268.3d*E (JD2416700 - 17850) [00001]; Max = RR Peg |2417859 + 260.8d*E (JD2417850 - 21000) [00960]; since JD2421000 - RR Peg |see Table. RS Peg |P var. Max = 2415846 + 431.5d*E (JD2415800 - 18450); Max = 2418434 RS Peg |+ 404.1d*E (JD2418400 - 24200); Max = 2424514 + 413.4d*E (JD2424500 RS Peg |- 34900) [00960]; Max = 2436496 + 403.4d*E (JD2435700 - 38600) RS Peg |[00001]; since JD2438500 - see Table. RT Peg |VB A (B 10.5m, 15.6", 291{deg}). P var. Max = 2423609 + 215.0d*E RT Peg |(JD2416000 - 24300); Max = 2428149 + 216.6d*E (JD2424300 - 32100); RT Peg |since JD2432100 - see Table. RU Peg |VB A (B 12.5m, 12", 18{deg}); SB2 (Porb = 0.3746d [09570]). There RU Peg |are also light oscillations with P = 11.6s and 50s [09571]. RV Peg |Emission. Light curve (1907 - 1973) [09572]. P var. Max = 2428735 + RV Peg |388.4d*E (JD2417000 - 32640); Max = 2430680 + 390.9d*E (JD2430200 - RV Peg |38900); since JD2438800 - see Table. RW Peg |P var. Max = 2419393 + 208.4d*E (JD2412700 - 19400); Max = 2421520 RW Peg |+ 213.0d*E (JD2419390 - 21550); Max = 2427133 + 208.0d*E (JD2421500 RW Peg |- 27150); since JD2427300 - see Table. RX Peg |P2 = 110d:. RY Peg |VB B (A = RZ Peg; B 20", 252{deg}). RZ Peg |VB A (B = RY Peg:20", 252{deg}). SC 6/9 - e. P var. Max = 2423361 + RZ Peg |441.4d*E (JD2411400 - 26450); Max = 2431215 + 434.0d*E (JD2426400 - RZ Peg |33000); since JD2433000 - see Table. SS Peg |P var. Max = 2416390 + 410.8d*E (JD2415500 - 20000); Max = 2422235 SS Peg |+ 423.8d*E (JD2420000 - 27000); Max = 2427270 + 403.4d*E (JD2427000 SS Peg |- 29000); Max = 2437218 + 416.35d*E (JD2428500 - 43000); since SS Peg |JD2443000 - see Table. SV Peg |H2O emission. SX Peg |S 2.5/6 e. P var. Max = 2436043 + 306.56d*E (JD2414800 - 38300); SX Peg |since JD2438300 - see Table. TU Peg |P var. Max = 2417800 + 320.8d*E (JD2404300 - 18450); Max = 2420730 TU Peg |+ 328.4d*E (JD2418450 - 20800); Max = 2428080 + 319.6d*E (JD2420800 TU Peg |- 31600); since JD2432800 - see Table. TW Peg |H2O maser. The basic light variation with the period given in the TW Peg |Table is superimposed by small oscillations with P = 94.13d. TY Peg |Min II 10.2. P var. Min I hel = 2419520.476 + 3.0922754d*E TY Peg |(JD2412300 - 19600) [02389]; Min I hel = 2425918.348 + 3.092252d*E TY Peg |(JD2419600 - 26000) [00001]; since JD2426000 - see Table. TZ Peg |P var? Max = 2425892 + 213.7d*E (JD2410000 - 28000); since TZ Peg |JD2430000 - see Table. UU Peg |OH, H2O maser. UW Peg |According to [08837] P = 60d. UX Peg |P var. Min = 2428428.386 + 1.544618d*E (JD2422100 - 28430) [00230]; UX Peg |Min = 2431273.597 + 1.544632d*E (JD2428420 - 34000) [00001]; since UX Peg |JD2434000 - see Table. VV Peg |{Delta}(S) = 8. P var. Max = 2420105.296 + 0.48837765d*E (JD2420000 VV Peg |- 28900); Max = 2433217.268 + 0.48838307d*E (JD2432800 - 38000) VV Peg |[03506]; since JD2438000 - see Table. VW Peg |P = 2.341295d? VX Peg |The basic light variation is superimposed by the secondary one with VX Peg |P = 80 - 90d:. VZ Peg |[Fe/H] = -1.75. WW Peg |P var. Max = 2433142 + 371.6d*E (JD2415670 - 33200) [00001]; since WW Peg |JD2436800 - see Table. ZZ Peg |Min II 12.5. AE Peg |P var. Max = 2415470.866 + 0.4967388d*E (JD2415500 - 21000); Max = AE Peg |2426161.544 + 0.496725d*E (JD2425400 - 31500); Max = 2432632.809 + AE Peg |0.496692d*E (JD2431500 - 36000) [00001]; during JD2436000 - 40000 - AE Peg |see Table. {Delta}(S) = 6.3. AG Peg |SB2 (Porb = 820d [09580]). Maximum of brightness was in 1870, then AG Peg |the very slow light decrease was observed that was superimposed AG Peg |since 1935 by periodical light oscillations with A = 0.4m V and P = AG Peg |Porb: Min = 2428250 + 827.d*E ( JD2428000-43000) [09587]. After AG Peg |JD2442300 the period probably has changed: Min = 2442370 + 760d*E AG Peg |[09587]. In 1962 - 1979 the range of brightness was 7.95m - 8.55m AG Peg |V; M - m = 0.50P. Light minima correspond to the epochs of inferior AG Peg |conjunction of M 3 III component. Spectrum var: Beq (1893 - 1919); AG Peg |since 1922 the spectrum is symbiotic one, the M star spectrum being AG Peg |more noticeable. Surrounded by a radio nebula with 1" half-power AG Peg |diameter. AN Peg |P var. Max = 2428045 + 274.1d*E (JD2424500 - 38500) [09581]; since AN Peg |JD2438500 - see Table. AO Peg |{Delta}(S) = 4.3. AQ Peg |Min II 10.47; d = 0.030P. P var. Min I = 2424749.335 + 5.548419d*E AQ Peg |(JD2424000 - 34000) [00980]; since JD2434000 - see Table. AS Peg |Of the two stars circled in the chart in [06286], the southern AS Peg |component varies. AT Peg |Min II 9.04. P var. Min I = 2425862.337 + 1.1460988d*E (JD2425800 - AT Peg |37500) [00001]; Min I = 2437497.542 + 1.146080d*E (JD2437490 - AT Peg |40000) [06101]; Min I = 2440407*4370 + 1.1461007d*E (JD2440000 - AT Peg |42400) [00001]; since JD2442400 - see Table. AU Peg |Cepheid in a close binary system. SB1 (Porb = 53.319d, K1 = 41.8 AU Peg |km/s, {gamma} = -4.1 km/s, E = 0.12 [09582]). [Fe/H] = 0.1. P var. AU Peg |Max = 2428729.76 + 2.3978d*E (JD2426500 - 28750) [00916]; Max = AU Peg |2433151.976 + 2.38934d*E (JD2433150 - 35800); Max = 2439039.08 + AU Peg |2.39079d*E (JD2435800 - 39100) [00001]; since JD2441700 - see AU Peg |Table. There is a square term in the elements given in the Table: AU Peg |+2.246d*10**(-6)*E**2. The shape of the light curve varies: 0.20P < AU Peg |M - m < 0.47P. AV Peg |P var. Max = 2416347.713 + 0.39036510d*E (JD2414000 - 26500) AV Peg |[00752]; Max = 2426582.301 + 0.39037015d*E (JD2426500 - 36000) AV Peg |[09584]; since JD2436000 - see Table. [Fe/H] = +0.02. AW Peg |d = 0.07P, Min II 7.60. BB Peg |Depth of Min II 0.60m. There is a square term in the elements given BB Peg |in the Table: +2.3d*10**(-11)*E**2. dI = 0.05P; dII = 0.00P. BF Peg |P var. Max = 2426589.293 + 0.495796d*E + 2.8d*10**(-9)*E**2 BF Peg |(JD2426500 - 28800) [00522]; Max = 2433200.312 + 0.495796d*E BF Peg |(JD2429400 - 33200) [00001]; Max = 2437583.343 + 0.495674d*E BF Peg |(JD2437500 - 39400) [00001]; since JD2442650 - see Table. BG Peg |P var. Min = 2427386.3705 + 1.952452d*E (JD2426000 - 35000) BG Peg |[03567]; Min = 2436453.509 + 1.95238d*E (JD2435000 - 43500) BG Peg |[03624]; since JD2443500 - see Table. BH Peg |P var. Max = 2426596.535 + 0.64101381d*E (JD2426500 - 28200) BH Peg |[01038]; since JD2434400 - see Table. Blazhko effect. A var. Max (O BH Peg |- C) = 2442929.03 + 39.8d*N [09588]. (k - b)2 = 0.09; {Delta}(S) = BH Peg |5. BI Peg |Waves with a cycle of 60 - 80d are superimposed. BK Peg |Min II 10.47. BO Peg |Min II 11.6. P var. Min I = 2427655.460 + 0.5804342d*E (JD2426500 - BO Peg |35100) [02263]; since JD2444000 - see Table. BP Peg |P1 = 0.084510d; P1:P0 = 0.77. Beat period Pb = 0.3698d [06604]. BS Peg |The chart in [06286] is wrong. BU Peg |Observations are represented by the elements in the intervals BU Peg |JD2432000 - 34000, JD2438200 - 41400. BX Peg |Depth of Min II 0.62m; dI = 0.05P; dII = 0.00P. P var. Min I = BX Peg |2431323.278 + 0.2804238d*E (JD2424700 - 39000) [00279]; since BX Peg |JD2439000 - see Table. BY Peg |P var. Min I = 2424745.75 + 0.34193403d*E (JD2424700 - 35400); BY Peg |since JD2435000 - see Table. CC Peg |Min II 12.9. CG Peg |{Delta}(S) = 2. P var? CU Peg |d = 0.010P. P var. Min = 2433895.463 + 3.8801345d*E (JD2425500 - CU Peg |34000) [00001]; Min = 2434221.392 + 3.880196d*E (JD2434000 - 36500) CU Peg |[07929]; since JD2436500 - see Table. CZ Peg |Min II 13.9. DF Peg |Min II 9.2. DG Peg |P var. Max = 2425857 + 148.15d*E (JD2425500 - 33500); since DG Peg |JD2433500 - see Table. DH Peg |P var. Max = 2414981.537 + 0.25550478d*E (JD2414000 - 24000) DH Peg |[01158]; Max = 2427695.390 + 0.2555107d*E (JD2424000 - 33500) DH Peg |[09590]; since JD2433500 - see Table. [Fe/H] = -0.9. DI Peg |Min II 9.59. P var. Min I = 2425644.315 + 0.7118144d*E (JD2425500 - DI Peg |30000) [02431]; Min I = 2437559.4096 + 0.7118182d*E (JD2430000 - DI Peg |40000) [09592]; Min I = 2440159.6796 + 0.71181417d*E (JD2440000 - DI Peg |44500); since JD2444500 - see Table. DK Peg |d = 0.04P. P var. Min = 2427745.388 + 1.631801d*E (JD2427700 - DK Peg |33700); since JD2433700 - see Table. DM Peg |d = 0.03P; Min II 11.0. DN Peg |Mean brightness varies with cycles 800 - 1400d and A = 0.2m - 0.4m. DO Peg |P var. Min = 2434272.350 + 2.61394d*E (JD2428000 - 34700) [00485]; DO Peg |since JD2434700 - see Table. DV Peg |Min II 12.1. DY Peg |P var. Max = 2432751.9624 + 0.072926372d*E (JD2429000 - 38000); DY Peg |since JD2438000 - see Table. The basic pulsation is superimposed by DY Peg |the secondary one with P1 = 0.05570d [09594]. A var, M - m var (Pi DY Peg |= 0.2358d): 0.55m < A < 0.67m, 0.24P < M - m < 0.42P. {Delta}(S) = DY Peg |6. DZ Peg |P var. Max = 2429127.211 + 0.6073407d*E (JD2419000 - 28800); Max = DZ Peg |2429127.189 + 0.6073761d*E (JD2429100 - 33500); since JD2433500 - DZ Peg |see Table. EE Peg |Min II 7.06. The third body (Porb = 1464d, T0 = 2443120). EF Peg |VB B (A 14.0m; B 5", 305{deg}). EH Peg |d = 0.08P. EQ PegA |VB A (B = EQb Peg; A = 6.87", Porb = 359 yr, E = 0.20. [09597]); EQ PegA |{mu} = 0.560", P = 91.7{deg}. A (B) >= 1.4m. EQ PegB |VB B (A = EQa Peg). a = 6.87'' P orb = 1464d, T0 = 2443120. A(U) >= EQ PegB |1.9m. ET Peg |{Delta}(S) = 4. EU Peg |Min II 12.3. EZ Peg |On 1943 November 16 the spectrum of the star was B [02875]; EZ Peg |probably at that time the star had a flare. FL Peg |Min II 14.0. FU Peg |Blazhko effect (Pi = 150d); A var; 15.2m <= Max <= 15.8m; 0.15P <= FU Peg |M - m <= 0.50P. GH Peg |Depth of Min II 0.13m. GR Peg |P var. Max = 2436492 + 69.93d*E (JD2436420 - 38740); since GR Peg |JD2440470 - see Table. GT Peg |{mu} = 0.51", P = 96{deg}. Epoch of the light minimum is given. GT Peg |During the flares A(U) < 3.6m. GV Peg |{Delta}(S) = 5:. GW Peg |Min II 15.1. GX Peg |SB1 (Porb = 2.340939d [06103]). GZ Peg |VB A (B 10.6m, A3V, 32.7", 198{deg}). HN Peg |[Fe/H] = -0.09. Epoch of light minimum is given. The variability of HN Peg |emission in H and K call lines with P = 4.63d was detected [09600]. HP Peg |Vr = -381 km/s. HR Peg |S4+/1+ . HZ Peg |Min II 17.6. II Peg |{mu} = 0.575", p = 86.5{deg}. SB1 (T0 = 2443030.396 + 6.724464d*E); II Peg |T0 is the epoch of the inferior conjunction of K-star. The epoch of II Peg |the distortion wave maximum is given in the Table. Mean brightness II Peg |of the system varies. IK Peg |SB1 (Porb = 21.724d). Multiperiodicity [09609]. IM Peg |SB1 (Porb = 24.649d). OX Peg |VB A (B 9.4m V, 12.8", 265{deg}, 2018). QQ Peg |Variability needs confirmation. V0341 Peg |SB, Porb = 2.1779d. V0342 Peg |Suspected SB. V0405 Peg |Type ZAND is also possible. V0407 Peg |MinII 9.69. O'Connell effect. V0415 Peg |VB (8.9m, 9.1m, 0.2", 316{deg}, 1996). V0416 Peg |VB (8.1m, 10.0m, 4", 36{deg}, 1991). V0418 Peg |SB2, Porb = 135.19d. V0421 Peg |Min II = 8.63. V0429 Peg |Blazhko effect, P = 80.2d. V0437 Peg |The object 1WASP J213004.12+120428.8 = 2RXP J213005.4+120426 = GSC V0437 Peg |1127.1390 was named V0437 Peg in 2013 (type BY, P= 0.5837:d). V0437 Peg |Howerer, because of the low resolution of SuperWASP data, this (non V0437 Peg |really variable star in 30" to the north, V15(NGC7078), cluster V0437 Peg |member. P varies. Streng Blazhko effect. V0443 Peg |Blazhko effect from Catalina data [80001]. V0444 Peg |Superhumps: P = 0.097762d [80233]. V0460 Peg |The period of ellipsoidal variations is tabulated. Pulsational V0460 Peg |periods: 0.06479d and 0.06337d. The A8 component pulsates. V0473 Peg |O'Connell effect. V0479 Peg |Period varies. V0492 Peg |P = 0.11068d for the main DSCTC mode. Multiperiodic, several other V0492 Peg |GDOR and DSCTC periods. V0499 Peg |VB A (A 10.90mJ; B 11.50mJ, 9", 324{deg}, 2000). V0510 Peg |Multiperiodic. V0513 Peg |Porb = 0.17918d. V0517 Peg |Blazhko effect? V0521 Peg |Porb = 0.05986d. V0533 Peg |VB AB (A 9.7mJ; B 11.3mJ, 4", 1 {deg}, 1998). V0537 Peg |Porb = 0.42234d. V0550 Peg |Blazhko effect. V0553 Peg |Blazhko effect? V0585 Peg |Multiperiodic. V0598 Peg |Porb is tabulated. Pspin = 0.02893d. V0615 Peg |Porb = 0.240946d from spectroscopy. V0624 Peg |SB, Porb = 0.05865d. High proper motion. V0627 Peg |A close southern companion of GSC 02197-00866. High proper motion. V0643 Peg |Double-mode pulsation. P2 = 0.73025d. V0648 Peg |Double-mode pulsation. P2 = 0.220793d. V0674 Peg |P = 0.3632d is not excluded. V0691 Peg |P1 is presented in the Table. P0 = 0.488102d, P1/P0 = 0.7451. V0713 Peg |P1 is presented in the Table. P0 = 0.555216d, P1/P0 = 0.7468. V0714 Peg |P1 is presented in the Table. P0 = 0.478308d, P1/P0 = 0.7439. V0716 Peg |P1 is presented in the Table. P0 = 0.485087d, P1/P0 = 0.7442. V0718 Peg |VB A (B = NEXT STAR IN PEGASUS, 12", 55{deg}, 2000). V0719 Peg |VB B (A = PREVIOUS STAR IN PEGASUS; AB 12", 55{deg}, 2000). V0720 Peg |P1 is presented in the Table. P0 = 0.544770d, P1/P0 = 0.7457. V0723 Peg |P = 55.2d is superposed. V0727 Peg |P1 is presented in the Table. P0 = 0.492575d, P1/P0 = 0.7450. V0730 Peg |VB B (A 15.6mG, B 15.7mG; AB 11", 116{deg}, 2000). V0732 Peg |VB B (A 15.3mG, B 15.8mG; BA 6", 246{deg}, 2000). The variability V0732 Peg |range in the Table is for combined light. V0733 Peg |P1 is presented in the Table. P0 = 0.532732d, P1/P0 = 0.7460. V0734 Peg |P1 is presented in the Table. P0 = 0.545923d, P1/P0 = 0.7456. V0736 Peg |VB A (15.3mG; B 16.3mG, 6", 166{deg}, 2000). P1 is presented in the V0736 Peg |Table. P0 = 0.539620d, P1/P0 = 0.7463. The variability range is for V0736 Peg |combined light. V0737 Peg |P1 is presented in the Table. P0 = 0.492187d, P1/P0 = 0.7452. V0740 Peg |VB A (17.5mG; B 18.8mG, 5", 79{deg}, 2000). P1 is presented in the V0740 Peg |Table. P0 = 0.521470d, P1/P0 = 0.7456. V0742 Peg |P1 is presented in the Table. P0 = 0.480465d, P1/P0 = 0.7446. V0743 Peg |P1 is presented in the Table. P0 = 0.478391d, P1/P0 = 0.7443. V0744 Peg |P1 is presented in the Table. P0 = 0.536693d, P1/P0 = 0.7464. V0745 Peg |P1 is presented in the Table. P0 = 0.498880d, P1/P0 = 0.7447. V0746 Peg |P1 is presented in the Table. P0 = 0.469896d, P1/P0 = 0.7433. V0752 Peg |Blazhko effect, P = 138d:. V0753 Peg |P1 is presented in the Table. P0 = 0.503623d, P1/P0 = 0.7460. V0755 Peg |P1 is presented in the Table. P0 = 0.467317d, P1/P0 = 0.7438. V0756 Peg |Additional non-radial mode: P = 0.3122540d, P(Blazhko) = 14.0d. V0756 Peg |Another non-radial mode, with P = 0.321512d, is also possible. V0758 Peg |P varies, the elements in the Table are for JD 2455600 - 2456600. V0758 Peg |Additional non-radial mode: P = 0.260058. Amplitudes of both V0758 Peg |oscillations vary. V0759 Peg |P1 is presented in the Table. P0 = 0.549317d, P1/P0 = 0.7463. V0761 Peg |Multiperiodic. The Table presents light elements for the V0761 Peg |first-overton mode. P0 = 0.1419385d, P2 = 0.0876715d. V0764 Peg |P1 is presented in the Table. P0 = 0.498405d, P1/P0 = 0.7446. V0766 Peg |Porb = 0.07824d. V0768 Peg |P1 is presented in the Table. P0 = 0.492663d, P1/P0 = 0.7447. V0771 Peg |Additional non-radial mode: P = 0.310512d, P(Blazhko) = 8.2d. V0772 Peg |Blazhko effect, P = 53d. bet Peg |VB A (B 11.2m, 109", 211{deg}). eps Peg |VB A (B 12.66m, 81", 325{deg}; C 8.65m, 140", 321{deg}). Usually eps Peg |varies in the range 2.29m - 2.44m V. On 1972 september 26/27 in the eps Peg |interval 23h58m - 00h02m UT it was bright (0.7m V), then at 00h09m eps Peg |UT decreased to 2.4m V [06875]. On 1847 November 5 the star was eps Peg |3.5m, then the brightness increased but on November 6 it was still eps Peg |fainter than normal [09606]. tau Peg |P2 = 0.04895d; PB = 0.4943d. S Per |In the region of the open cluster h, {chi} Per. OH, H2O, SiO maser. S Per |In 1920 - 1969 there were secondary waves with cycles of 300d - S Per |700d and {Delta}(m) ~1m [08630]; in 1935 - 1961 P1 = 807d, P2 = S Per |930d [09694]. T Per |Other periodicities were noted. In the region of open cluster h, T Per |{chi} Per. U Per |P var. Max = 2411683 + 316.10d*E (before JD2422500); Max = 2422748 U Per |+ 326.53d*E (JD2422500 - 34000); since JD2434000 - see Table. V Per |VB A (B 14m, 28", 278{deg}). W Per |P2 = 2667d +- 460d is superimposed. X Per |3U 0352 + 30. LX/Lopt = 10**(-2). ADS 2859 A (B = V397 Per, M3III, X Per |22.5", 12{deg}). SB. IR excess. X-ray pulsar (P = 13.93m). Further X Per |periodicities were noticed in X-ray, optical, spectroscopic X Per |observations: 22.4h, 308.33d, 580.7d. Y Per |P var. Max = 2414990 + 254.74d*E (JD2415000 - 18000); Max = 2418049 Y Per |+ 246.25d*E (JD2418000 - 22000); Max = 2422242 + 253.62d*E Y Per |(JD2422000 - 41000); since JD2441000 - see Table. Z Per |d = 0.028P; Min II 9.8. P var. Min = 2418173.663 + 3.056422d*E Z Per |(JD2415000 - 19000) [01961]; Min = 2425481.416 + 3.05636d*E Z Per |(JD2419000 - 31000) [00978]; since JD2431000 - see Table. RR Per |P var. Max = 2424280 + 392.01d*E (JD2416000 - 28500); since RR Per |JD2428500 - see Table. RS Per |In the region of the open cluster h, {chi} Per. According to RS Per |[01053], P = 152d. RT Per |Min II 10.67. P var. Min = 2411963.2995 + 0.84941322d*E (JD2411317 RT Per |- 19400); Min = 2419702.3124 + 0.84940248d*E (JD2419400 - 29300); RT Per |Min = 2429751.6066 + 0.84941274d*E (JD2429300 - 33000); since RT Per |JD2433000 - see Table. RV Per |Min II 10.4. P var. Min = 2417972.345 + 1.973489d*E (JD2417000 - RV Per |25500); since JD2432500 - see Table. RW Per |The light curve shape var, d = 0.03P - 0.000P. Min II 9.78. P var. RW Per |Before JD2425720 Min = 2425720.0185 + 13.198910d*E; Min = RW Per |2429217.5946 + 13.198399d*E (JD2425720 - 36700); since JD2436700 - RW Per |see Table. RY Per |d = 0.014P; Min II 8.65. RZ Per |S 3/7 e. P var. Before JD2430500 Max = 2415034 + 353.19d*E; since RZ Per |JD2430500 - see Table. ST Per |VB A (B 12.1m, 11.6", 6{deg}, 1928). d = 0.014P, Min II 9.62. P ST Per |var. Min = 2419030.5038 + 2.6483615d*E (JD2418500 - 27000) [09740]; ST Per |Min = 2429528.5897 + 2.6483488d*E (JD2427000 - 34600) [02389]; Min ST Per |= 2439091.716 + 2.648353d*E (JD2439000 - 42400); since JD2442400 - ST Per |see Table. SU Per |In the region of the open cluster h, {chi} Per. SV Per |[A/H] = 0.6. SB2, hot companion. P var? Before JD2435000 Max = SV Per |2419055.145 + 11.12875d*E [02431]; since JD2435000 - see Table. SX Per |[A/H] = 0. The chart in [08300] SY Per |In the region of the open cluster NGC 1528. TU Per |{Delta}(m), P var. Before JD2427200 Max = 2418572.288 + TU Per |0.6070775d*E; Max = 2427119.334 + 0.6070643d*E (JD2427200 - 36000); TU Per |since JD2436000 - see Table. TV Per |P2 = 1080d is superimposed. TX Per |[Fe/H] = -0.88. OH maser. TZ Per |VB A (B14m, 13", 290{deg}). Mu {alpha} = +0.012", {mu} {delta} = TZ Per |-0.050". In the region of the open cluster h, {chi} Per. UX Per |[A/H] = -0.3. UY Per |[A/H] = -0.3. In the region of the open clusters King 4, Czernik 8. UZ Per |P2 = 91d is superimposed. VV Per |Twice shorter P is possible [00960]. VX Per |In the region of the open cluster h, {chi} Per. [A/H] = -0.2. P VX Per |var. Since JD2431000 - see Table. VY Per |In the region of the open cluster h, {chi} Per. [A/H] = -0.3. VZ Per |VB A (B 16.9m pg, 17", 180{deg}). In the region of the open cluster VZ Per |Tr 2. WY Per |P var. Min = 2425234.460 + 3.327126d*E (JD2421500 - 26000) [01072]; WY Per |since JD2441500 - see Table. XX Per |VB A (B 9.7m vis, 21", 176{deg}, 1909). Mean brightness var, P = XX Per |4100d. XY Per |ADS 2788 AB ({delta}(mV) = 0.6m - 2.5m, 1.4", 75{deg}, SpA = A2II, XY Per |SpB = B6e). IR excess. XZ Per |Min II 11.6. P var? Min = 2425150.439 + 1.1516282d*E (JD2425000 - XZ Per |29000) [00522]; Min = 2437932.411 + 1.1516347d*E + XZ Per |0.005d*sin(0.09091{deg}*E) (JD2432000 - 38000) [00001]; since XZ Per |JD2438000 - see Table. YZ Per |In the region of the open cluster h, {chi} Per. ZZ Per |The coordinates are possibly erroneous. AB Per |d = 0.045P; Min II 10.5. VB ({Delta}(m) = 0.0m vis, 0.20", AB Per |86.4{deg}, 1978). AD Per |Mean brightness var, P = 2950d. In the region of the open cluster AD Per |h, {chi} Per. AE Per |P2 = 2150d is superimposed. AG Per |ADS 2990 A (B {Delta}(m) = 2.0m, 0.9", 225{deg}, 1975; C 12.6m, AG Per |36", 118{deg}, 1948). The combined brightness AB is given. Min II AG Per |7.00, DII = 0.10P, dII = 0. Apsidal motion: Min II - Min I = AG Per |1.01435d + 0.0884d*sin(0.0278{deg}*E + 49.1{deg}). AR Per |P var, nonlinear term: +1.18d*10**(-11)*E**2. [Fe/H] = -0.17. AS Per |{Delta}(m) var, d ({Delta}(B))/dt = -0.01m/yr. AV Per |P = 250 - 300d. AW Per |SB2, companion B6V, {Delta}(m) (companion - AW) = 2.8m vis. AX Per |Epoch of Min is given. The variability with {Delta}(m) up to 0.7m AX Per |pg is caused probably by the orbital motion. Outburst activity is AX Per |superimposed. AY Per |d = 0.009P. BE Per |In the region of the open cluster CR 39. BI Per |In the region of the open cluster Berk 9. BL Per |P = 125 - 130d. BM Per |[Fe/H] = -0.04. BP Per |Min II = Min I. In the region of the open cluster Cr 39. BU Per |Max brightness var, P = 8.1yr [01085]. In the region of the open BU Per |cluster h, {chi} Per. CC Per |Min II 14.1. CI Per |P var (3.35d - 3.40d), possibly with a period of 4000d. The light CI Per |curve shape var. CK Per |d = 0.05P:. CM Per |d = 0.052P. In the region of the open cluster Stock 2. CO Per |In the region of the open cluster Stock 2. CR Per |Elements need confirmation. In the region of the open cluster Stock CR Per |2. CS Per |In the region of the open cluster Stock 2. CZ Per |In the region of the open cluster h, {chi} Per. DE Per |d = 0.01P? DF Per |In the region of the open cluster h, {chi} Per. DG Per |d = 0.021P. DK Per |The depth of Min II 0.05m. In the region of the open cluster h, DK Per |{chi} Per. DM Per |Min II 8.02, DII = 0.17P. Depths of Minima, the shape of Min II DM Per |var. In the region of the open cluster h, {chi} Per. DO Per |In the region of the open cluster h, {chi} Per. DP Per |In the region of the open cluster h, {chi} Per. DR Per |In the region of the open cluster h, {chi} Per. DS Per |In the region of the open cluster h, {chi} Per. DT Per |In the region of the open cluster h, {chi} Per. DU Per |In the region of the open cluster h, {chi} Per. DV Per |Min II 14.5. DY Per |In the region of the open cluster Tr 2. DZ Per |Min II 14.7. In the region of the open cluster Tr 2. EL Per |Before JD2428900 Max = 2427980 + 167d*E; during JD2428900 - 31000 - EL Per |see Table. EO Per |IR excess? ER Per |Mean brightness var, P ~900d. EU Per |Min brightness var, P ~900d. EW Per |Superimposed waves 70d - 180d. In the region of the open cluster EW Per |Stock 4. EX Per |Min II 12.5. FM Per |VB A (B 12.1m, 3", 285{deg}). P var? Max = 2429982.268 + FM Per |0.489199d*E (JD2428000 - 30600); During JD2433700 - 36000 - see FM Per |Table. FR Per |In the region of the open cluster NGC 1528. FV Per |Cycles 300 - 350d, 1800d:. FX Per |d = 0.04P. In the region of the open cluster NGC 1582. FY Per |Possible periods 0.0702d, 0.4407d. Photometric spectral type B1V. FZ Per |In the region of the open cluster h, {chi} Per. GH Per |P = 220d is possible. GK Per |SB2 (sdBE + K2IVp). The following types of activity are being GK Per |observed after the return to the normal brightness: rapid irregular GK Per |variations ({Delta}(m) ~0.1m in several minutes); irregular GK Per |fluctuations from night to night ({Delta}(m) up to 0.3m); slow GK Per |irregular variations ({Delta}(m) = 1.5m in several dozen days); GK Per |bursts with light increase in 10d - 30d and decrease in 10d - 40d, GK Per |{Delta}(m) up to 3.5m, the mean interval between bursts being GK Per |{delta}(t) = 820d [09686,09788]. According to [10198], the radial GK Per |velocities are represented with the elements Max (Vr > 0) = GK Per |2444912.966 + 1.996803d*E (Kabs = 124 km/s, Kem = 34 km/s). GK Per |According to [10199], the 2d variation is modulated with a period GK Per |of 0.131623d, Max ({delta}(Vr)) ~2443787.995 (Kabs = 15 km/s, Kem = GK Per |20 km/s). During a burst the sinusoidal modulation of X-ray flux GK Per |was recorded, Tmax = 24455555.67456 + 0.004066443d*E [09786]. GK Per |ExpAnding envelope (0.454"/yr, 1948 - 1964; 0.432"/yr, 1964 - 1981, GK Per |[09787]). GP Per |[A/H] = -0.5. GQ Per |According to [00021], Sp K0. HQ Per |[A/H] = -0.3. HS Per |In the region of the open cluster Stock 4. HV Per |d ~0.03P. HW Per |Min II 13.3. Min II - Min I = 0.45P:. HY Per |Three of the four min in [01079] are not satisfied with the HY Per |elements. HZ Per |[A/H] = -0.8. B_V: +1.93, +2.34. II Per |Min II 13.6. In the region of the open cluster NGC 1582. IK Per |Min II 11.6. IM Per |Min II 12.7. The elements need confirmation. In the region of the IM Per |open cluster Cr 39. IO Per |H2O maser. IP Per |IR excess. IQ Per |dI = 0.02P. Min II 7.88, DII = 0.12P, dII = 0.03P, Min II - Min I = IQ Per |0.53P. P var? VB A (B = BD + 47{deg} 921, 9.30m, A0V np:, 39.3", IQ Per |175{deg}); SB1. IT Per |dI = 0.06P. Min II 10.0, DII = 0.24P:, dII = 0.16P:. VB ({Delta}(m) IT Per |= 1.7m, 12", 37{deg}). The range of the combined brightness is IT Per |given. IW Per |SB1. Min II 5.83. IX Per |The depth of Min II 0.02m. VB A (B 10.6m, 5", 208{deg}). IZ Per |Min II 8.3. KK Per |In the region of the open cluster h, {chi} Per. KP Per |Beat phenomenon: P1 - see Table, A1 = 0.0323m B; P2 = 0.1980855d, KP Per |A2 = 0.0235M B; P3 = 0.2270986d, A3 = 0.0072M B. KR Per |Min II 11.1. KS Per |SB (Porb = 360.47d). The main component is a helium star. Besides KS Per |the semiregular variability (see Table), variations were noted with KS Per |P = 50 - 100 Min and {Delta}(m) of several hundredths of a KS Per |magnitude. IR excess. Variable polarization (P - 1%). KT Per |Quasi-periodic oscillations during outbursts: P = 22.9s - 29.5s KT Per |[05959], 82s, 90s, 147s [09791], {Delta}(m) up to ~0.01m. KV Per |[Fe/H] = -0.96. P var. Max = 2428950.400 + 0.24942d*E (JD2428950 - KV Per |29200); since JD2429500 - see Table. KW Per |Min II 10.8. P var. Min = 2426295.450 + 0.931255d*E (JD2423400 - KW Per |39500) [04009]; since JD2440000 - see Table. KY Per |In the region of the open cluster h, {chi} Per. KZ Per |In the region of the open cluster h, {chi} Per. LL Per |In the region of the open cluster h, {chi} Per. LM Per |In the region of the open cluster h, {chi} Per. LN Per |In the region of the open cluster h, {chi} Per. LO Per |In the region of the open cluster h, {chi} Per. LP Per |In the region of the open cluster h, {chi} Per. LQ Per |In the region of the open cluster h, {chi} Per. LR Per |Very red. In the region of the open cluster h, {chi} Per. LX Per |DII = 0.05P. Migrating distortion wave: P = 475d [09792], LX Per |{Delta}(m) up to 0.04m. MS Per |Min II 12.1. MX Per |IR excess. NP Per |Min II 13.0. NR Per |P var. Max = 2416780 + 323.0d*E (JD2415750 - 24550); Max = 2435060 NR Per |+ 340.2d*E (JD243350 - 35400); since JD2436700 - see Table. NU Per |A close pair, var is the southern star. OV Per |D ~2h. PP Per |In the region of the open cluster h, {chi} Per. PR Per |In the region of the open cluster h, {chi} Per. QR Per |Red. QU Per |d = 0.03P. QW Per |Min II 14.7:. QX Per |Min II 16.1. V0345 Per |In the nebula NGC 1579. V0346 Per |In the nebula NGC 1579. V0347 Per |In the nebula NGC 1579. V0351 Per |In the region of the open cluster h, {chi} Per. V0352 Per |In the region of the open cluster h, {chi} Per. V0354 Per |In the region of the open cluster h, {chi} Per. V0355 Per |In the region of the open cluster h, {chi} Per. V0356 Per |In the region of the open cluster h, {chi} Per. V0357 Per |In the region of the open cluster h, {chi} Per. P = 0.21955d is V0357 Per |possible. V0358 Per |In the region of the open cluster h, {chi} Per. V0359 Per |In the region of the open cluster h, {chi} Per. V0360 Per |In the region of the open cluster h, {chi} Per. Other possible V0360 Per |periods: 0.40036d, 0.40154d. V0361 Per |In the region of the open cluster h, {chi} Per. V0363 Per |Red. V0364 Per |Min II 15.6, Max II 14.8. V0365 Per |Min II 14.3:. V0376 Per |P2 = 0.09165d, A2 = 0.016m; P1 - see Table, A1 = 0.037m. A var. V0380 Per |SB (Porb = 26d?). The epoch of Min light is given. V0382 Per |In the region of the open cluster h, {chi} Per. V0392 Per |The southern component of a very close pair. V0394 Per |H2O maser. V0395 Per |VB A (B 3.5", 90{deg}). V0396 Per |In the region of the open cluster {alpha} Per. Observations are V0396 Per |also satisfied by P ~1.678d. According to [07586], P = 2.4928d or V0396 Per |1.6857d. V0397 Per |ADS 2859 B (A = X Per; B 22.5", 12{deg}). V0398 Per |IN type is also possible. V0403 Per |In the region of the open cluster h, {chi} Per. V0409 Per |Epoch of Min is given. V0423 Per |ADS 2433 A (B 11.9m, 30.8", 99.2{deg}); SB. Porb is given. V0424 Per |In the region of the open cluster h, {chi} Per. IR excess. V0425 Per |VB A(B 12.8m, 3.6", C 14.3m, 6.8"). In the region of the open V0425 Per |cluster h, {chi} Per. V0428 Per |According to [08639], type IS? V0432 Per |Min II 11.6. V0434 Per |Min II 14.9. V0436 Per |Min II 5.74; Min II - Min I = 0.413P; D II = 0.03P. V0437 Per |In the region of the open cluster NGC 744. V0438 Per |In the region of the open cluster h, {chi} Per. VB (8.7m, 10.9m, V0438 Per |1".2, 26{deg}). Min II 8.34. The range of combined brightness V0438 Per |variation is given. The bright component is considered to be V0438 Per |variable. This suggestion needs verification. V0439 Per |In the region of the open cluster h, {chi} Per. V0440 Per |In the region of the open cluster h, {chi} Per. ADS 1820 A (B V0440 Per |14.5m, 8".3, 122{deg}). V0449 Per |Min II 13.3. V0451 Per |Min II 15.8. V0459 Per |In the {alpha} Per cluster. V0461 Per |In the {alpha} Per cluster. V0462 Per |Min II 14.0. V0465 Per |P2 = 0.030d is superimposed. V0466 Per |Superposition of P1 = 5300d +- 250d, P2 = 475d +- 35d ({Delta}(m) = V0466 Per |1.1m), P3 = 0.26d ({Delta}(m) = 0.5). V0468 Per |P1 = 925s, P2 = 1022s. {mu} = 0".29, p = 170{deg}. V0469 Per |Changes of line profiles with periods 0.150d, 0.188d, 0.304d, V0469 Per |0.476d, 0.608d, 1.88d [09814]. In 1978/1979 non-radial pulsations V0469 Per |were observed: P1 = 1.74d. P2 = 2.04d [04173,04180]. V0470 Per |VB A (B 18.8m B, 1" - 2"). V0471 Per |The central star of the planetary nebula M1-2 = VV8. According to V0471 Per |[09815,09816], const. V0547 Per |High proper motion (LTT 10610) not confirmed by HIPPARCOS data. V0580 Per |The variability may be due to the fainter (B) component. V0582 Per |A single deep minimum at the bottom of the small-amplitude (5.63 - V0582 Per |5.64) wave. V0592 Per |VB (0".2, 197 {deg}, 1989.7). V0680 Per |MinII 14.07. V0732 Per |A twice shorter period is not excluded. V0751 Per |Min II = 11.90 :. MinII - MinI = 0.450P. V0752 Per |Beperiodic, P2 = 0.0265d. V0753 Per |Min II = 13.71. V0754 Per |Min II = 12.30. MinII - MinI = 0.412P. V0756 Per |Min II = 12.90. V0757 Per |Multiperiodic. The range is in the Geneva B passband. VB A (B V0757 Per |12.2mV, 7", 185{deg}, 2007). V0758 Per |Min II = 10.70. V0789 Per |Min II = 13.4. V0871 Per |Min II = 11.38. V0873 Per |Min II = 11.5. V0874 Per |VB AB (4", 215{deg}, 1998). V0876 Per |Min II = 14.1. V0877 Per |Min II = 14.0. V0880 Per |Min II = 13.7. Type EA with D = 0.11P is not excluded. V0881 Per |Min II = 11.01. O'Connell effect. V0882 Per |Min II = 12.10. V0884 Per |Min II = 11.21. V0885 Per |Min II = 13.45. V0886 Per |Min II = 14.1. V0887 Per |Min II = 10.30. V0888 Per |A twice longer period is possible. V0889 Per |Multiperiodic. SB, Porb = 31.9456d. V0890 Per |Min II = 12.05. V0894 Per |Min II = 10.95. Type EB is not completely excluded. V0899 Per |Min II = 13.17. V0901 Per |Min II = 10.70. V0912 Per |Min II = 12.5. V0919 Per |VB B (A = V711 Per, 15.4mI; B 15.8mI, 8", 321{deg}, 1999). V0920 Per |VB A (B = V716 Per, 14.1m, 9", 293{deg}, 1999). V0929 Per |Outside the cluster tidal radius. V0930 Per |Outside the cluster tidal radius. V0931 Per |Outside the cluster tidal radius. V0932 Per |Outside the cluster tidal radius. V0934 Per |Min II = 15.85. O'Connell effect. V0935 Per |Outside the cluster tidal radius. V0936 Per |Min II = 15.2. V0939 Per |Outside the cluster tidal radius. V0943 Per |Outside the cluster tidal radius. V0944 Per |Min II = 16.78. Outside the cluster tidal radius. V0945 Per |Min II = 16.20. Outside the cluster tidal radius. V0947 Per |Min II = 13.95. V0951 Per |Min II = 13.14. V0958 Per |A twice longer period is possible. V0959 Per |Min II = 10.7 :. V0960 Per |Min II = 11.83. V0963 Per |Min II = 13.7. V0964 Per |Min II = 12.90. V0966 Per |MinII - MinI = 0.33P. e = 0.284. V0982 Per |MinII - MinI = 0.38P. V1024 Per |VB A (B 4", 168{deg}, 1989). V1035 Per |Type DSCT with P = 0.1441d is also possible. V1036 Per |Type SR with P = 71d is not excluded. V1041 Per |Type SR with P = 160d is not excluded. V1043 Per |The epoch in the Table corresponds to the eclipse-like feature of V1043 Per |the light curve but not to the overall brightness minimum. V1056 Per |VB A (B 6", 80{deg}, 2000; other companions). The magnitudes in the V1056 Per |Table are for combined brightness; if corrected for neighbors, the V1056 Per |approximate range is 11.75 - (12.4m*. V1057 Per |Type ELL with a twice longer period is not excluded. V1058 Per |O'Connell effect. V1060 Per |VB A (B 6", 1{deg}, 1999). V1066 Per |O'Connell effect. V1078 Per |Multiperiodic. P0 is presented in the Table. P1 = 0.143832d. bet Per |Multiple system (Eclipsing pair = Algol AB; Algol C 4.7m, Am, a = bet Per |0".10, Porb = 1.862a); Algol AB = ADS 2362 A (B 12.7m, 57".5, bet Per |156{deg}, 1920). P var. P = 2.8673442d (1784 - 1835); P = bet Per |2.8673012d (1835 - 1854); P = 2.8672775d (1854 - 1901); P = bet Per |2.8672967d (1901 - 1913); P = 2.8672506d (1913 - 1915) [06156]; Min bet Per |I = 2424477.806 + 2.86730236d*E (JD2420500 - 25000); Min = bet Per |2425917.203 + 2.86732697d*E (JD2425000 - 277000); Min I = bet Per |2433194.454 + 2.86731667d*E (JD2427700 - 33600); Min I = bet Per |2433928.4944 + 2.86732442d*E (JD2433600 - 37000); Min I = bet Per |2437598.6766 + 2.86733732d*E (JD2437000 - 42200); since JD2442200 - bet Per |see Table. Porb (Algol C) = 1.862a may be traced in the deviations; bet Per |a period of 32a may also be real. Depth of Min I var. Variable bet Per |polarization, changes in hydrogen line profiles, sometimes bet Per |emissions in the spectrum. Radio source with frequent burst of bet Per |different amplitude, faint X-ray source. del Per |Variable emission {lambda} 1650 A [06905]. Vr var, A = 16 km/s. ksi Per |In the far IR range ({lambda} = 10 mkm) {Delta}(m) > 1m. In the far ksi Per |IR range ({lambda} = 10 mkm ) {Delta}(m) > 1m; the variability is ksi Per |related to mass loss. omi Per |VB A (B 8.4m, 0.96'', 29.7{deg},1972). Possible superposition of omi Per |BCEP type oscilations. rho Per |A slower variation of the mean light is possible. phi Per |SB2. (Porb = 126.696d). v*sin(i) = 450km/s. A var (P ~Porb). b Per |SB2. Depths of minima differ by 0.03m. Third body? , P = 701d. b Per |Radio source. In the region of the open cluster NGC 1545. R Phe |P var. Max = 2405121 + 271.0d*E(JD2405000 - 11500); Max = 2414570 + R Phe |266.26d*E(JD2414500 - 25500); since JD2425500 - see Table. T Phe |P var. Max = 2411252 + 281.00d*E(JD2410000 - 30000); since T Phe |JD2430000 - see Table. W Phe |P var. Max = 2414960 + 328.65d*E(JD2414500 - 19500); Max = 2424530 W Phe |+ 332.87d*E(JD2424500 - 30200); since JD2436000 - see Table. RS Phe |P var? RT Phe |P = 208d? RV Phe |P var?; (k-b)2 = 0.06; {Delta}(S) = 8: SX Phe |{mu} = 0.894", ro = 163.1{deg}. P var. Max = 2433923.9618 + SX Phe |0.054964519d*E1 - 0.00337d*sin(2{pi}*(0.28503379*E1 + 0.074)) SX Phe |(JD2433900 - 36900); since JD2436900 - see Table. There is a SX Phe |periodic term in the elements given in the Table: SX Phe |-0.00325*sin(2{pi}*(0.28503575*E2 - 0.107)). According to [09614] SX Phe |for epoch 1950.0 P0 = 0.054964509, P1 = 0.042772831, Pb = SX Phe |0.1928355; dP0/dt = -87*10**(-13), dP1/dt = -174*10**(-13), dPb/dt SX Phe |= 2.46*10**(-10). P1/P0 = 0.778; 0.8m <= A <= 0.3m; 0.2p <= M-m <= SX Phe |0.4p. [Fe/H] = -0.6. WW Phe |Min II 12.7. YZ Phe |Min II 13.0. AD Phe |Min II 10.80. P var. Min I = 2436847.375 + 0.3799277*E (JD2428650 - AD Phe |36850); since JD2436850 - see Table. AE Phe |Min II 8.19; 0.033p <= dI <= 0.05p; dII = 0.00. The shape of the AE Phe |light curve varies with periods 55.9d and 95.3d [09615]. P var. Min AE Phe |I = 2440857.8140 + 0.36237459*E (JD2438250 - 40870) [07388]; Min I AE Phe |= 2441969.57074 + 0.36237186d*E (JD2440870 - 42000) [09616]; Min I AE Phe |= 2442654.8201 + 0.3623741d*E (JD2441950 - 42660) [09533]; since AE Phe |JD2443700 - see Table. AG Phe |Min II 8.95. P var. Min I = 2440415.231 + 0.7553429d*E (JD243800 - AG Phe |40850); since JD2443750 - see Table. AI Phe |Min II 8.89; dI = 0.0035; Min II - Min I = 0.46p. AU Phe |Min II 13.0. According to [09517] the P value given in the Table is AU Phe |wrong. AX Phe |{mu} = 0.234", p = 70{deg}. Multiperiodical: P i = 606.8s, 682.7s, AX Phe |744.7s, 840.2s (Ai ~0.01m). CG Phe |Type RRC: is also possible. CZ Phe |The first-overtone period is tabulated. P0 = 0.56680d, CZ Phe |{Delta}(m)1/{Delta}(m)0 = 1.9. DN Phe |Blazhko effect? DP Phe |P probably varies. DR Phe |Blazhko effect, P=40.17d [81056]. gam Phe |SB1 (P orb = 193.85d). zet Phe |VB A (B 7.0m, A7:, 0.46", 51.4{deg}, 1965.9; C 8.0m, F7V, 6.4"). zet Phe |Total light range of A and B components is given in the Table. Min zet Phe |II 4.22, MinII - MinI = 0.507p; dII = 0.02p. iot Phe |VB A (B 12.7m, 7.7", 270{deg}). ksi Phe |VB A (B 12.1m, 13.2", 253{deg}). Epoch of MinI(v) is given in the ksi Phe |Table. A(v) = 0.13m. rho Phe |Frequency analysis results see also in [09619,09620, 9621]. psi Phe |SB. R Pic |P var. Max = 2413413 + 165.8d*E (JD2413000 - 23600); since R Pic |JD2423600 - see Table. Light curve (1923 - 1953) [01054]. S Pic |P var. Max = 2413595 + 424.7d*E (JD2405500 - 23000); since S Pic |JD2423000 - see Table. OH emission. U Pic |P var. Max = 2428103.565 + 0.44036450*E (JD2414000 - 29000) U Pic |[00353]; since JD2438400 - see Table. (k - b)2 = 0.17; {Delta}(S) = U Pic |3. X Pic |Min II 10.8 RR Pic |Since 1965 periodic light variations were detected with A(B) = RR Pic |0.33m and elements Max = 2438815.380 + 0.14502545d*E. These RR Pic |variations are superimposed by others with A(B) = 0.036m and period RR Pic |~15.6 min or 15.4 min [09612]. There are also rapid oscillations RR Pic |with periods in the range 20 - 40s [09613]. RT Pic |Not seen only on one plate; defect? RV Pic |Min II 9.79. SU Pic |Min II 10.4. VW Pic |Variability may be due to component B. VZ Pic |Kapteyn's star. AL Pic |Blazhko effect, P = 34.0d. AM Pic |VB A (A 9.6m; B = HD 273920, 10.3m, Sp K7, 27", 123{deg}, 2000). AM Pic |The tabulated range is for the combined brightness. AO Pic |VB (A 9.7m; B 11.1m, 2.1", 39{deg}, 1929). AS Pic |Min II = 11.10. dP/dt = +0.38 x 10^(-5)d/yr. AU Pic |Min II = 14.3. AW Pic |Blazhko effect. P(Bl) = 756d [81001]. AX Pic |P varies. AY Pic |SB2. del Pic |Min II 4.83. R Psc |P var. Max = 2418070 + 344.14d*E (JD2397070 - 27700); Max = 2432866 R Psc |+ 347.1d*E(JD2427300 - 33000) - see Table. S Psc |P var. Max = 2406665 + 405.6d*E (JD2398944 - 2407100); Max = S Psc |2415930 + 402.6d*E (JD2407100 - 16500); Max = 2421295 + 413.7d*E S Psc |(JD2416500 - 21500) - see Table. U Psc |P var. Max = 2417230 + 172.71d*E (JD2407720 - 18000); Max = 2423840 U Psc |+ 174.3d*E (JD2418000 - 24000) [00001]; Max = 2424527 + 170.3d*E U Psc |(JD2423000 - 26100) [00960]; Max = 2432514 + 174.05d*E (JD2425000 - U Psc |33000) [00001]; since JD2433000 - see Table. W Psc |P var. Max = 2412690 + 189.08d*E (JD2412692 - 27100) [01193]; since W Psc |JD2435000 - see Table. X Psc |P var. Max = 2433474 + 357.3*E (JD24295000 - 38000); since X Psc |JD2438000 - see Table. Y Psc |P var. Min = 2410002.844 + 3.76582d*E (JD2410000 - 19700) [09707]; Y Psc |Min = 2425495.522 + 3.765903d*E (JD2423200 - 6300) [01072]; Min = Y Psc |2430613.384 + 3.7658895d*E (JD2427300 - 30620); Min = 2432865.357 + Y Psc |3.7658405d*E (JD2430620 - 32900); Min = 2435693.452 + 3.7657765d*E Y Psc |(JD2432860 - 36600) [00001]; Min = 2441225.473 + 3.765859d*E Y Psc |(JD2439000 - 42500) [06956]; Min = 2443142.29056 + 3.7658491d*E Y Psc |(JD2442500 - 44000) [08593]; since JD2444000 - see Table. RS Psc |In the region of the galaxy NGC 251. RT Psc |Mean brightness varies with P2 = 533d. According to [08643] 30d <= RT Psc |P1 <= 70d. RU Psc |[Fe/H] = -1.65. P var. [00752,09714] Max = 2415407.609 + RU Psc |0.3903008d*E (JD2414400 - 15700); Max = 2416022.660 + 0.3902139d*E RU Psc |(JD2415700 - 16600); Max = 2417244.537 + 0.3902878d*E (JD2416600 - RU Psc |19200); Max = 2419936.853 + 0.3903520d*E (JD2419200 - 22000); Max = RU Psc |2425894.778 + 0.3903016d*E (JD2422000 - 26200); Max = 2426214.829 + RU Psc |0.3903546d*E (JD2426200 - 27300); Max = 2427397.519: + 0.3902216d*E RU Psc |(JD2427300 - 28000); Max = 2428165.524 + 0.3903535d*E (JD2428000 - RU Psc |29300); Max = 2429488.868: + 0.3904577d*E (JD2429300 - 600) RU Psc |[00752]. Max = 2430053.353 + 0.390202d*E (JD2430000 - 650); Max = RU Psc |2430935.366 + 0.390354d*E (JD2430600 - 940); Max = 2431331.307 + RU Psc |0.390457d*E (JD2430940 - 31350); Max = 2432119.417 + 0.390346d*E RU Psc |(JD2431350 - 32120); Max = 2433162.250 + 0.390283d*E (JD2432100 - RU Psc |33200); Max = 2433905.311 + 0.390261d*E (JD2433200 - 33910); Max = RU Psc |2433905.311 + 0.390321d*E (JD2433900 - 35430); Max = 2435429.502 + RU Psc |0.390412d*E (JD2435420 - 35800); Max = 2435781.265 + 0.39027d*E RU Psc |(JD2435780 - 36130); Max = 2436501.361 + 0.39032d*E (JD2436130 - RU Psc |36510); Max = 2436534.190 + 0.39043d*E (JD2436500 - 36850); Max = RU Psc |2436845.351 + 0.39025d*E (JD2436840 - 37200); Max = 2437181.358 + RU Psc |0.39031d*E (JD2437180 - 37610); Max = 2437994.329 + 0.39026d*E RU Psc |(JD2437610 - 38000); [00001]. Max = 2438303.950 + 0.39040d*E RU Psc |(JD2438000 - 38400) [03879]. Max = 2438375.409 + 0.39027d*E RU Psc |(JD2438370 - 38650) [00001]. Max = 2439435.2421 + 0.390385d*E RU Psc |(JD2438650 - 39500) [09713]. Max = 2439435.242 + 0.390313d*E RU Psc |(JD2439430 - 39800); Max = 2439771.3049 + 0.39046d*E (JD2439770 - RU Psc |40140) [00001]. Since JD2440140 - see Table. According to [03569] A RU Psc |var with P = 28.8d. RV Psc |Min II 12.0. RY Psc |(k-b)2 = 0.03, {Delta}(S) = 7. P var. Max = 2419677.268 + RY Psc |0.52971027d*E (JD2414000 - 22000); Max = 2425148.192 + RY Psc |0.52972643d*E (JD2422000 - 25500) [01337]; Max = 2425508.390 + RY Psc |0.5297291d*E (JD2425500 - 40000); Max = 2441538.476 + 0.52972911d*E RY Psc |(JD2441000 - 41650) [07984]; since JD2442660 - see Table. RZ Psc |Algol-like. SS Psc |(k-b)2 = 0.19; {Delta}(S) = 2. Blazhko effect: -0.04d <= O-C <= SS Psc |+0.04d; Min(O-C) = 2437520 + 136d*E [09731]. SU Psc |Min II 11.3. SW Psc |P var. Max = 2425177.298 + 0.5212844d*E (JD2419670 - 25200) SW Psc |[04191]; Max = 2425177.256 + 0.5212642d*E (JD2425170 - 38000) SW Psc |[03506]. Since JD2438600 - see Table. There is a periodic term in SW Psc |the elements given in the Table: + 0.0132d*sin(5.440{deg}*(E + 2)). SW Psc |Blazhko effect (Pi = 34.5d). SX Psc |P var. Min = 2427811.357 + 0.825882d*E (JD2425580 - 36000) [01218]; SX Psc |Min = 2437202.453 + 0.825877d*E (JD2436000 - 39900) [00001]; since SX Psc |JD2439800 - see Table. SZ Psc |Min II 7.38. P var. There is a square term in the elements given in SZ Psc |the Table: -0.113d*10**(-6)*E**2. TY Psc |Porb = 0.080d [09735]. The cycle of supermaxima is 370d [09675]. UU Psc |VB A (B 7.60m, F4V, 11.5", 148{deg}, 1966.9). Min II 6.04; Min II - UU Psc |Min I = 0.55P. Elliptical orbit and rotation of the line of apsides UU Psc |are possible. UV Psc |Min II 9.54. P var. Min I = 2424134.574 + 0.8610475d*E (JD2414600 - UV Psc |24150) [00001]; Min I = 2428038.555 + 0.861046d*E (JD2424150 - UV Psc |36700) [02924]; since JD2436700 - see Table. The shape of the light UV Psc |curve varies. UW Psc |Min II 11.0:. UZ Psc |SB1 (Porb > 1 yr [05751]). VZ Psc |Mu = 0.43", P = 65{deg}. Min II 10.43. WW Psc |VB A (B 13.1m, 31"). WX Psc |OH, H2O, SiO maser. ZZ Psc |P1 = 612s, P2 = 816s [07476]. Nonradial modes [08467]. AG Psc |P (Vr) = 0.055d. AH Psc |The star was seen in 1854 - 60; since 1862 it was not observed. AO Psc |Epoch of Max brightness is given. Light variations with Porb = AO Psc |0.1496263d are superimposed by variations with P = 858.6861s and AO Psc |twice smaller amplitude (Max = 2444815.00276 + 0.009938496d*E; M-m AO Psc |= 0.54P), and also by still smaller oscillations with P = 805.2059s AO Psc |(Max = 2444815.00294 + 0.009319513d*E). The last period is the AO Psc |X-ray impulse period which is equal to the period of rotation of AO Psc |the compact object (probably a white dwarf). EM Psc |The depth of MinII is 0.35. EQ Psc |Multi-mode pulsations at a time scale of hours. ET Psc |VB (A 9.1m; B 11.8m, 2".9, 198{deg}, 1830). EU Psc |VB (A 9.1m; B 9.8m, 0.1", 111{deg}, 1991). EW Psc |Min II = 10.37. EX Psc |Min II = 14.27. EY Psc |Min II = 9.35 :. EZ Psc |VB A (B 13.6m, 25", 59{deg}, 2000; C 12.1m, 33", 131{deg}, 1969). FM Psc |Multiperiodic. FR Psc |Blazhko effect, P=51d:. FT Psc |VB AB (A 12.5mHp; B 13.6mHp, 2", 316{deg}, 1991). FU Psc |Min II = 11.98 :. FY Psc |Min II = 13.3. GG Psc |Min II = 13.85. GK Psc |Min II = 13.9. GO Psc |Min II = 13.35. GR Psc |Min II = 11.75. GS Psc |VB A (B 15.8mV, 10", 62{deg}, 1997). GT Psc |Min II = 12.47. GW Psc |Min II = 12.0. GX Psc |Min II = 13.65. GY Psc |Min II = 12.6. HL Psc |Min II = 10.97. Strong O'Connell effect in [80021] but not in HL Psc |[80057]. HN Psc |Min II = 10.93. HO Psc |Min II = 11.6. IN Psc |VB A (B 8", 48{deg}, 1999). Combined magnitudes are tabulated. KV Psc |Multiperiodic. P2 = 0.289120d. P2/P1 = 0.9779. LL Psc |Double-mode pulsation. The period in the Table is for the first LL Psc |overtone. P0 = 0.468938d. P1/P0 = 0.7434. LM Psc |VB A (B 4", 305{deg}, 1997). LO Psc |VB A (B 12.2m, 5", 299{deg}, 2012). LQ Psc |VB A (B 10.5m, 5", 314{deg}; C 10.5m, 9", 57{deg}, 2015). R PsA |P var. Max = 2417385 + 293.00d*E (JD2405000 - 26000); Max = 2432896 R PsA |+ 291.50d*E (JD2426000 - 38000); since JD2438000 - see Table. S PsA |P var. Max = 2417853 + 271.0d*E (JD2411000 - 18000); Max = 2426880 S PsA |+ 273.6d (JD2418000 - 27000); Max = 2434714 + 270.3d (JD2427000 - S PsA |35000); since JD2434000 - see Table. X PsA |Min II 14.2. RW PsA |Min II 11.63. TX PsA |VB B (A 13.0m pg; B 37", 131{deg}); {mu} = 0.22", p = 117{deg}. XZ PsA |MinII 8.04. AE PsA |Blazhko effect, P = 5.78d. AG PsA |The first-overtone period is tabulated. P0 = 0.49785d. A1/A0 = 1.6. AO PsA |Period varies? AR PsA |P1 is presented in the Table. P0 = 0.569776d, P1/P0 = 0.7457. pi. PsA |SB (Porb = 178.3177d [05769]). R Pup |In the region of the open cluster NGC 2439. U Pup |P var. Max = 2415090 + 314.26d*E (JD2408000 - 22800); since U Pup |JD2422800 - see Table. V Pup |VB A (B 10.0m, 7", 0, 70{deg}; C 11.0m, 19.0", 48{deg}). Min II V Pup |4.82. P var. IO - CI < 0.02d. W Pup |P var. Max = 2420990 + 120.68d*E (JD2412500 - 23600); Max = 2424725 W Pup |+ 119.9d*E (JD2423600 - 26300); Max = 2432200 + 120.68d*E W Pup |(JD2426300 - 40800); since JD2440800 - see Table. X Pup |P var. Max = 2414889.8 + 25.939d*E (JD2408800 - 16000); Max = X Pup |2435188.76 + 25.9610d*E (JD2419000 - 35190) [02392]; Max = X Pup |2436279.50 + 25.97d*E (2435190 - 38000) [00001]; since JD2438000 - X Pup |see Table. Z Pup |OH, H2O, SiO emission. P var. Max = 2424256 + 513.90d*E (JD2413900 Z Pup |- 24500); since JD2424500 - see Table. RS Pup |Surrounded by the reflecting nebulosity with a radius of 1.4' RS Pup |[09634]. P var. Max = 2419186.3 + 41.337d*E (JD2414000 - 24000) RS Pup |[02049]; Max = 2427083.613 + 41.414d*E (JD2425800 - 28300) [02440]; RS Pup |Max = 2434823.23 + 41.38535d*E (JD2433750 - 34900) [09636]; since RS Pup |JD2435700 - see Table. RW Pup |P var. Max = 2430175 + 332.5d*E (JD2424500 - 30200) [00001]; since RW Pup |JD2435800 - see Table. RX Pup |Light curve (1890 - 1925) [01265]. Mira type component light RX Pup |variations are observed in the infrared region of spectrum: Max = RX Pup |2444530 + 580d*E, 3.99m - 6.00m J, M - m = 0.50P [09518]. ST Pup |[A/H] = -0.9. The light curve shape and the period vary strongly: ST Pup |0.10P < M - m < 0.30P; 17.4d < P < 19.19d. P = 19.188d (JD2415000 - ST Pup |17000); 18.949d (JD2417000 - 18000), 18.8065d (JD2418000 - 19000), ST Pup |18.721d (JD2419000 - 20000), 18.714d (JD2420000 - 21000), 18.717d ST Pup |(JD2421000 - 22000), 18.6175d (JD2422000 - 23000), 18.678d ST Pup |(JD2423000 - 24000), 18.735d (JD2424000 - 25000), 18.796d ST Pup |(JD2425000 - 26000), 18.817d (JD2426000 - 27000) [01266]. Max = ST Pup |2427779.6 + 18.846d*E (JD2427000 - 28000) [01266]; Max = 2428893.9 ST Pup |+ 18.885d*E (JD2428000 - 29000) [00016]; Max = 2429697.51 + ST Pup |19.188d*E (JD2429000 - 30000) [01266]. P = 19.142d (JD2430000 - ST Pup |31000), 19.145d (JD2431000 - 32000) [01266]. Max = 2435395.430 + ST Pup |18.559d*E (JD2435160 - 500) [06006]; Max = 2435617.45 + 18.8864d*E ST Pup |(JD2435500 - 5620) [02309]; Max = 243957.3 + 17.4d*E (JD2438700 - ST Pup |39600) [06611]; since JD2444000 - see Table. SV Pup |P var. Max = 2419010 + 166.6d*E (JD2413660 - 18000); Max = 2423090 SV Pup |+ 169.8d*E (JD2418000 - 23100); Max = 2426782 + 167.8d*E (JD2423100 SV Pup |- 27500); since JD2427500 - see Table. SW Pup |Min II 9.1; d = 0.029P. TT Pup |Min II 13.6. TY Pup |Min II 8.87. UZ Pup |Min II 10.0. VV Pup |{mu} = 0.100", P = 165.0{deg}. The epoch of light maximum is given. VV Pup |The mean brightness varies by 2 - 3m. Intervals of active light VV Pup |variation with amplitude up to 2m during maximal mean brightness VV Pup |are observed. During low activity intervals when amplitude is about VV Pup |0.3m mean brightness is minimal; during this time the ellipsoidal VV Pup |light variations of the system are observed in the range 15.1m - VV Pup |15.3m J with the elements Min = 2427889.6509 + 0.0697468256d*E VV Pup |[09644]. The white dwarf rotation period is equal to the orbital VV Pup |period. There are flickerings. Spectrum description [09472,09645]. VW Pup |P var. Max = 2425184.67 + 4.28405d*E (JD2422660 - 25600) [00973]; VW Pup |Max = 2435554.86 + 4.28519d*E (JD2425600 - 35600) [02309]; since VW Pup |JD2435500 - see Table. VX Pup |P1 = 2.1389d (A1 = 0.29m); A0 = 0.31m; P1/P0 = 0.71042. VY Pup |The depth of Min II 0.04m. VZ Pup |[A/H] = -0.3. P var. Max = 2434864.90 + 23.1640d*E (JD2426700 - VZ Pup |35300) [02309]; since JD2435300 - see Table. WW Pup |P var. Max = 2424497.73 + 5.5159d*E (JD2423520 - 26000) [00973]; WW Pup |since JD2426000 - see Table. WX Pup |P var. Max = 2435042.184 + 8.93825d*E (JD2422000 - 35100) [02431]; WX Pup |since JD2435000 - see Table. WZ Pup |P var. Max = 2427861.33 + 5.02657d*E (JD2421100 - 29400) [02392]; WZ Pup |since JD2429400 - see Table. XX Pup |P var. Max = 2426338.503 + 0.51719805d*E (JD2426300 - 39500) XX Pup |[03572]; since JD2441700 - see Table. (k - b)2 = 0.07. The spectral XX Pup |type according to CA II is given. XY Pup |Min II 9.4; d = 0.042P. XZ Pup |Min II 7.90. P var. Min I = 2440629.7969 + 2.192383d*E (JD2425850 - XZ Pup |41700) [00099]; since JD2441700 - see Table. YY Pup |The depth of Min II 0.05m. AE Pup |In the region of the open cluster Cr 173. AF Pup |Min II 13.5. AG Pup |Min II 10.9. AH Pup |The depth of Min II 0.05m. AN Pup |Min II 10.7. AQ Pup |VB A (B 11.13m, < 15"; C 12.83m, < 15"). [A/H] = -0.1. The range of AQ Pup |the variation of combined light is given. P var. Max = 2429734.59 + AQ Pup |29.931d*E (JD2427500 - 33000) [03474]; Max = 2433296.2 + 30.018d*E AQ Pup |(JD2433000 - 35850) [02474]; Max = 2436625.9 + 29.8568d*E AQ Pup |(JD2435850 - 36700) [03601]; Max = 2441760.63 + 30.032d*E AQ Pup |(JD2436600 - 42700) [09671]; since JD2443400 - see Table. AR Pup |The mean brightness varies with P = 1200d. AS Pup |In the region of the open cluster NGC 2546. P var. Max = 2416110 + AS Pup |331.4d*E (JD2415460 - 26000); since JD2426000 - see Table. AT Pup |In the region of the open cluster NGC 2546. P var. Max = AT Pup |2426758.205 + 6.6648d*E (JD2426700 - 35600) [02202]; since AT Pup |JD2435600 - see Table. AU Pup |Min II 9.28. P var. Min I = 2428111.304 + 1.126418d*E (JD2414700 - AU Pup |28200) [00007]; since JD2439000 - see Table. AV Pup |Min II 11.0. AW Pup |VB A (B 11.7m, 3.7", 258{deg}). Period probably must be doubled. AY Pup |Min II 12.5. AZ Pup |Min II 10.1. BB Pup |(k - b)2 = 0.24; {Delta}(S) = 3. BH Pup |In the region of the open cluster Cr 173. BI Pup |In the region of the open cluster Cr 173. BK Pup |In the region of the open cluster Cr 173. BL Pup |Min II 14.2. BN Pup |In the region of the open cluster NGC 2533. BP Pup |Min II 12.3. BQ Pup |The shape of the light curve possibly varies. BR Pup |Min II 12.9. BT Pup |Min II 14.5. In the region of the open cluster NGC 2482. BU Pup |Min II 13.9. In the region of the open cluster NGC 2447. BW Pup |The depth of Min II 0.15m. BX Pup |In the region of the open cluster NGC 2482. CE Pup |P var? [07934]. CH Pup |P var. Max = 2428465 + 491.0d*E (JD2428400 - 37300); since CH Pup |JD2437300 - see Table. CO Pup |P var? The epoch of light minimum is given. CP Pup |In 1981 the radius of the shell expanding with Vexp = 710 km/s was CP Pup |equal to 7" [09689,09559]. CX Pup |d = 0.05P. CY Pup |d = 0.01P:; Min II 13.0. CZ Pup |Min II 13.1. DD Pup |Min II 14.6; Min II - Min I = 0.572P. DE Pup |Min II 12.9. DF Pup |Min II 12.8. DK Pup |Min II 13.0. DM Pup |Min II 13.7; Min II - Min I = 0.62P. DN Pup |Min II 13.5. DO Pup |Min II 13.3. DR Pup |Min II 13.3:. DS Pup |Min II 13.4. DT Pup |Min II 14.3. EK Pup |VB A (B 15", 270{deg}). P var? Max = 2427747.89 + 2.62587d*E EK Pup |(JD2425500 - 29500) [01343]; since JD2434500 - see Table. EL Pup |P > 1.3d? In the region of the open cluster NGC 2437. EN Pup |Min II 11.4. EQ Pup |Min II 10.9. ES Pup |According to [00412], Max = 2430377 + 187d*E. The elements given in ES Pup |the Table are valid in the interval JD2425600 - 29700. EU Pup |Min II 14.8. FK Pup |A var (P2 = 3000d). Strong SiC2 bands in the spectrum. FM Pup |Min II 14.2. GG Pup |S5/5. GH Pup |VB A (B 10", 195{deg}; C 16", 280{deg}; D 14", 315{deg}). P var. GH Pup |Max = 2425450 + 800d*E (JD2425300 - 28000); since JD2428700 - see GH Pup |Table. Very red. GI Pup |In the region of the open cluster NGC 2437. GK Pup |IN the region of the open cluster NGC 2437. GN Pup |VB A (B 16.5m, 10", 80{deg}). GP Pup |Min II 13.5. GU Pup |Min II 12.2. GX Pup |Min II 13.9. In the region of the open cluster Cr 173. GY Pup |Min II 12.3. GZ Pup |Min II 12.1. HH Pup |(k - b)2 = 0.14, {Delta}(S) = 1. HI Pup |Min II 11.0. In the region of the open cluster Cr 173. HK Pup |P var. Max = 2425925.732 + 0.7342532d*E (JD2425300 - 36600) HK Pup |[04127]; since JD2436600 - see Table. HM Pup |There is a shallow Min II. HP Pup |P var? HW Pup |P var? Max = 2429756.28 + 13.4532d*E (JD2427100 - 33000) [03551]; HW Pup |since JD2433000 - see Table. KQ Pup |In the open cluster NGC2422. SB2 (Porb = 9752d [03985]). KT Pup |Min II 13.4. KW Pup |Min II 11.8. KX Pup |Min II 13.04; 0.435P (1930) < Min II - Min I < 0.56P (1973) KX Pup |[03474,08094]; e = 0.15. Apsidal motion. KY Pup |Min II 11.1. LN Pup |Min II 12.9; Min II - Min I = 0.533P. LO Pup |Min II 13.9. LP Pup |d = 0.03P:. LT Pup |Min II 12.6. MN Pup |Min II 13.2. MQ Pup |Min II 9.39. MT Pup |RCB? MW Pup |Min II 9.2. NO Pup |VB A [BC7.19m V, 8.1". 124{deg} ({delta}(M) = 0.0m, 0.20", NO Pup |275{deg}, 1976)]. Min II 6.66; Min II - Min I = 0.582P; e = 0.123. NQ Pup |S 4.5/2-. NW Pup |Porb = 1d. NX Pup |Connected with a cometary nebula. OR Pup |In the region of the open cluster NGC 2467. OS Pup |VB A (B 6.10m, 67.4"). In the region of the open cluster C OS Pup |0812-362. OU Pup |In the region of the open cluster IC 2391. OX Pup |In the region of the open cluster NGC 2451. PS Pup |The depth of Min II 0.028m. PT Pup |P2 = 0.168377d. A ({lambda} 1550) = 0.043m; 0.015m < A(B) < 0.035m. PU Pup |VB (5.2m, 5.6m; 0.11", 43.6{deg}, 1927). Min II 4.74. PV Pup |VB B (A 6.1m; B 16.9", 340{deg}; C 10.5m, 100.4", 228{deg}). Min II PV Pup |7.31; DII 0.10P; Min II - Min I = 0.47P. The light curve shape in PV Pup |Max and Min II varies. The deviations DB from the mean curve vary PV Pup |from -0.06m to +0.03m with the elements: Max (I{Delta}(B)I) = PV Pup |2440000.027458 + 1.92207d*E or Max (I{Delta}(B)I) = 2440000.219470 PV Pup |+ 0.48003d*E. PW Pup |Min II 9.54; d = 0.095P. In the region of the open cluster NGC PW Pup |2439. QS Pup |0.008m <= A(u) <= 0.015m. QT Pup |Probably a member of the open cluster NGC 2477. QU Pup |P2 = 0.1680d or 0.2019d; 0.010m <= A(u) <= 0.040m. QV Pup |May be a member of the open cluster NGC 2489. V0360 Pup |Type ACV: is also possible. V0364 Pup |The preceding component of the northern star in the system of two V0364 Pup |CoD-CPD objects, COD-36 3425 and CoD-36 3426 (CPD-36 1171 and V0364 Pup |CPD-36 1172). The cross-identifications of these CoD and CPD V0364 Pup |objects differ from one source to another; our adopted V0364 Pup |identification is based on the paper editions of the catalogs. V0376 Pup |Type ACV: is also possible. V0378 Pup |Type BE is also possible. V0393 Pup |SB, Porb = 2.5248d. V0419 Pup |Not a nearby star (despite having a Gl number). V0575 Pup |VB, {rho}=2". Component A: SB. V0579 Pup |MinII 13.52. V0581 Pup |MinII 12.43. V0582 Pup |MinII 7.94:. V0587 Pup |MinII 9.25. Erroneously marked in the chart in [78321]. V0588 Pup |The chart in [78107] is assumed to be wrong. V0589 Pup |MinII 8.97. V0596 Pup |VB A (B 8.58m, 0.3"). Range of the variation of combined light is V0596 Pup |given. Min II 7.03; DII = 0.08P; Min II - Min I = 0.48P. Min II = V0596 Pup |2444622.86709 + 4.5961766d*E. Apsidal motion (P = 3200 yr). V0605 Pup |A twice shorter period is not excluded. V0611 Pup |MinII - MinI = 0.40P. VB (A 8.6m; B 9.1m, 0.3", 130{deg}, 1990). V0620 Pup |VB B (A 11.7mV; B 12.0mV, 28", 358{deg}, 1999; C 12.5mV, 16", V0620 Pup |78{deg}, 1999). V0624 Pup |A much longer cycle superposed. V0626 Pup |VB (A 9.65m; B 10.0m, 9", 55{deg}, 1991). V0628 Pup |VB A (B 15.8mpg, 9", 84{deg}, 1995). V0634 Pup |A twice longer period is not excluded. V0642 Pup |MinII - MinI = 0.6P. V0651 Pup |Min II = 12.4. V0652 Pup |Min II = 9.83. VB AB (A 10.44m; B 10.55m, 0.80", 170{deg}, 1991). P V0652 Pup |varies. dP/dt = -0.28 x 10^(-5) d/yr. V0653 Pup |Min II = 10.53. V0654 Pup |Min II = 14.8. V0656 Pup |Min II = 18.25. V0658 Pup |Min II = 16.76. V0660 Pup |Min II = 16.4 :. V0661 Pup |Min II = 20.7. V0662 Pup |Min II = 20.5. V0663 Pup |Min II = 17.32:. V0664 Pup |Min II = 12.25. P varies. dP/dt = +0.24 x 10^(-5) d/yr. V0667 Pup |VB (1.8"), the NE star of the pair varies. The tabulated period is V0667 Pup |probably orbital. Stable pulses with Pspin = 0.00593d and amplitude V0667 Pup |of 0.03m. V0668 Pup |Min II = 13.3. V0670 Pup |Min II = 9.00. Eclipse amplitude is about 0.06m , out-of-eclipse V0670 Pup |variations [80015] with an amplitude about 0.12m. V0674 Pup |Min II = 10.95. P varies. dP/dt = -0.77 x 10^(-5) d/yr. V0675 Pup |Min II = 10.9. V0683 Pup |Multiperiodic. P2 = 1.40294d, P3 = 1.17811d. V0687 Pup |Blazhko effect? V0690 Pup |Min II = 8.96. V0691 Pup |Min II = 12.53. V0692 Pup |Min II = 14.70. V0695 Pup |Min II = 15.85. V0696 Pup |Min II = 14.39. V0697 Pup |Min II = 11.06. Cluster non-member. V0698 Pup |Min II = 12.6. V0701 Pup |Two modes with similar amplitudes. For the second mode, Max = V0701 Pup |2453015.749 + 0.296111d x E. V0707 Pup |P varies strongly. V0711 Pup |VB A (B 5", 128{deg}, 1999). V0714 Pup |Blazhko effect, P=116.96d. V0716 Pup |P varies strongly. V0719 Pup |Pulsates in the first (see Table) and second (Max = 2453455.40 + V0719 Pup |0.593216d x E) overtone modes. P2/P1 = 0.8057. VB B (A 9.96m, B V0719 Pup |11.0m, 6", 42{deg}, 1999); the range in the Table is for the V0719 Pup |combined brightness. V0722 Pup |SB2. V0725 Pup |VB A (B 10.3m, 1", 47{deg}, 1991). V0732 Pup |Pulsates in the first (see Table) and second (Max = 2453456.065 + V0732 Pup |0.333105d x E) overtone modes. P2/P1 = 0.8007. V0733 Pup |Pulsates in the fundamental mode (see Table) and in the first V0733 Pup |overtone (Max = 2453600.055 + 0.1742342d x E). P1/P0 = 0.7618. V0743 Pup |VB A (B 10", 211{deg}, 1999); magnitudes in the Table are for V0743 Pup |combined brightness. P1 is presented in the Table. P2 = 0.328118d; V0743 Pup |P2/P1 = 0.8000. V0751 Pup |VB A (B 12.8m, 0.6", 166{deg}, 2015). omi Pup |Type EA: is also possible. rho Pup |VB A (B 13.7m, 29.6", 15{deg}). [Fe/H] = +0.13. P var. Max = rho Pup |2435552.807 + 0.14088141d*E (JD2413900 - 37500) [09756]; Max = rho Pup |2439887.843 + 0.14088141d*E (JD2439800 - 43700); since JD2444000 - rho Pup |see Table. L 2 Pup |VB A (B 11.5m, 62", 214{deg}); {mu} = 0.34", P=18{deg}. H2O, SiO L 2 Pup |maser. S Pyx |P var. Max = 2411770 + 206.60d*E (JD2405500 - 23700); Max = 2423765 S Pyx |+ 207.0d*E (JD2423700 - 29600); since JD2429600 - see Table. T Pyx |Previous outbursts were observed in 1890, 1902, 1920, 1944. RR Pyx |A close companion 14.5m. RZ Pyx |Min II 9.69. SU Pyx |d = 0.016P. TT Pyx |P = 3.031556d? TV Pyx |Depth of Min II 0.05m. TX Pyx |Min II 9.8. TY Pyx |Min II 7.48. TZ Pyx |Min II 11.1. UZ Pyx |VB A (B 7.61m, 110", 180{deg}). VW Pyx |The nucleus of the planetary nebula K1-2. The range of the VW Pyx |variations of combined light: 15.7 - 17.4 pg. The value of P close VW Pyx |to that found by bond [09767] and the epoch of Max brightness are VW Pyx |given in the Table. CR Pyx |MinII 11.37. CU Pyx |MinII 12.36. CY Pyx |SB1. CZ Pyx |P = 635d [78130] superimposed. DK Pyx |MinII - MinI = 0.29P. DN Pyx |A twice shorter period is not excluded. DQ Pyx |Min II = 9.31. R Ret |P var. Max = 2403013 + 280.0d*E (JD2403000 - 13900); Max = 2423317 R Ret |+ 276.68d*E (JD2413900 - 25300); Max = 2430008 + 279.7d*E R Ret |(JD2425200 - 30020); since JD2430000 - see Table. T Ret |Mean brightness varies with P = 200d. X Ret |(k - b)2 = 0.09. P var. Max = 2427425.47 + 0.4920d*E [00357]; Max = X Ret |2434334.611 + 0.492011d*E (JD2434300 - 600) [00080]; since X Ret |JD2434600 - see Table. The shape of the light curve varies. Blazhko X Ret |effect: Pi >= 45d; 0.13P <= M - m <= 0.23P [00080]. VY Ret |MinII - MinI = 0.75P. WY Ret |Min II = 14.0. R Sge |P var (70.07d <= P <= 71.24d [09769]. Period variation study R Sge |[00767]. The elements given in the Table are valid since JD2434000. R Sge |The mean brightness varies: Min = 2414402 + 1112.d*E [01357]. S Sge |SB1 (Porb = 675d [01358]). P var. Max = 2409863.32 + 8.381968d*E S Sge |(JD2406600 - 18000); since JD2418000 - see Table. U Sge |VB A (B 9.6m, 92.0", 318{deg}). Min II 6.71; 0.014P <= dI <= U Sge |0.024P. In the region of the open cluster Col 399. Not a member of U Sge |the cluster. P var [06224,08608]. Mean elements are given in the U Sge |Table representing epochs of Min within +-0.008P. The shape of the U Sge |light curve varies. V Sge |VB A (B 13.9m, 9.7", 267{deg}); SB2 (K1 = 320 km/s, K2 = 85 km/s). V Sge |P var? The depth of eclipses varies from 0.6m to 1.3m. The mean V Sge |brightness outside eclipses varies. There are also flares with V Sge |amplitudes up to 3m and small light variations with a time scale of V Sge |minutes, dozens of minutes and a few days. spectrum description V Sge |[03593,09472]. X Sge |VB A (B 13.18m, 6", 248{deg}). Z Sge |V1 (NGC 6838, M71). Globular cluster member. P var. Max = 2437870 + Z Sge |175.3d*E (JD2437000 - 38700); since JD2438700 - see Table. RS Sge |The mean brightnese varies: Max = 2435999 + 1124d*E [08104]. Two RS Sge |Algol-like light weakenings were also observed: JD2444837.22, RS Sge |2444865.17 [09727]. RW Sge |P var. according to [01363] Max = 2424289 + 429d*E. Since JD2434000 RW Sge |- see Table. RZ Sge |Porb ~97m [09771]. Mean cycle is given according to [09785]. RZ Sge |Supermaxima are repeated with the cycle 266d. The period of RZ Sge |superhumps decreases from 101.3m till 100.8m. SY Sge |Min II 10.7. P var. Elements given in the Table are valid in the SY Sge |interval JD2425800 - 38300. TU Sge |d = 0.035P. TX Sge |P var. Max = 2425002 + 155.0d*E (JD2414900 - 25100); since TX Sge |JD2425000 - see Table. UU Sge |VB A (B 16.5m B, 4", 90{deg}). The nucleus of the planetary nebula UU Sge |Abell 63. Min II 14.41; d = 0.019P. The range of the combined light UU Sge |variation is given. The actual depth of Min I is about 4.3m. Large UU Sge |reflection effect. UZ Sge |Min II 11.6:. P var. Min I = 2429961.231 + 2.215750d*E (JD2429000 - UZ Sge |41600); since JD2441600 - see Table. VZ Sge |VB A (B 12m, 28.2", 206{deg}). WY Sge |Nova Sge 1783 (Max JD2372494:). Min I = 2445137.8993 + WY Sge |0.1536342d*E; D = 0.16P. Brightness outside eclipses is usually WY Sge |~18.7m, the depth of the eclipses is ~ 1.5 - 2m. At present WY Sge |outbursts by 1.6m are sometimes observed similar to the UG type WY Sge |variable outbursts, as well as rapid flickering of light [09708]. WZ Sge |Nova Sge 1913, 1946, 1978. VB A (B 15.76m B, 7", 280{deg}). Really WZ Sge |it is not a nova. Three outbursts were registered up to day: WZ Sge |JD2420094, 32001, 43844 [09710,09711]. There are superhumps on the WZ Sge |light curve during the outburst with 0.057250d >= P >= 0.05714d WZ Sge |(A=0.3m V) [09710,09776]. There are light variations between the WZ Sge |outbursts (A = 0.14m - 0.3m). During some of light weakenings WZ Sge |Algol-like eclipses are observed (A = 0.2m) with the elements: Min WZ Sge |I = 2437547.72845 + 0.0566878455d*E [09774]; D = 0.04P. d = 0.02P. WZ Sge |There are also rapid light oscillations (A <= 0.01m). The periods WZ Sge |of these oscillations before the 1978 outburst were 28.98s and WZ Sge |27.87s [09774], but after this outburst - 28.95963s [09775]. WZ Sge |According to [09777], in 1976 - 78 these oscillations were WZ Sge |represented by the elements: Max = 2443311.790250 + WZ Sge |0.00032254826d*E + 9.8d*10**(-16)*E**2. XY Sge |According to [03705] the spectrum is earlier than M0. AG Sge |P = 117d? BR Sge |d = 0.030P. CP Sge |Min II 13.3. CT Sge |Multiple. The tabulated range is for combined magnitudes. CU Sge |Min II 11.3. CW Sge |Min II 11.7. P var? The shape of the light curve varies. CZ Sge |Min II 15.2. DH Sge |The shape of the light curve varies (1.1m <= A <= 1.7m). P var. Max DH Sge |= 2427612.509 + 0.4695844D*E (JD2427600 - 38800) [04027]; since DH Sge |JD2438800 - see Table. Blazhko effect disappeared after the period DH Sge |change (A = 1.1m). DI Sge |P var. Max = 2427929 + 203.0d*E (JD2427500 - 30200) [02641]; since DI Sge |JD2437100 - see Table. DK Sge |Min II 13.0. DL Sge |Min II 11.5. DM Sge |Min II 11.6. DP Sge |P var. Max = 2427985.464 + 0.4883395d*E (JD2427985 - 33000); Max = DP Sge |2432855.191 + 0.4883339d*E (JD2433000 - 40775); since JD2440775 - DP Sge |see Table. DQ Sge |Min II 14.8. DS Sge |Min II 16.0:. DT Sge |d = 0.05P:. EH Sge |VB A (B 15.6m). EI Sge |Min II 14.6. ER Sge |P var. Max = 2430515.460 + 0.4184209d*E (JD2427000 - 38400); Max = ER Sge |2438443.388 + 0.4184356d*E (JD2438400 - 41800); since JD2441800 - ER Sge |see Table. FF Sge |d = 0.03P; Min II 13.0. FG Sge |VB A (B 14.2m, 8", 100{deg}). The central star of the planetry FG Sge |nebula PK 60{deg} (diameter 36", the age about 6000 years). The FG Sge |brightness of the star steadily increased from 13.6 pg in 1894 to FG Sge |the maximum in 1967, and then is steadily decreasing. In 1982 it FG Sge |was 11.0 B. In 1967 the strong absorption lines of rare earth FG Sge |elements appeared in the spectrum. The spectral class steadily FG Sge |becomes later. The signes of new planetary nebula ejection were FG Sge |observed. In 1962 the star entered the instability strip in the Mv, FG Sge |B-V diagram and began to pulsate with a small amplitude and FG Sge |increasing period: Min(V) = 2442629 + 59.83d*E + 1.126d*E**2 FG Sge |(JD2442600 - 44530). In twenty years the period increased from 50d FG Sge |to 134d, the amplitude of pulsations changed from 0.2mV to 0.5mV; FG Sge |now it decreased again to 0.2mV, and the period is only 90d FG Sge |[09780]. FH Sge |Min II 13.5. FL Sge |There is a close companion 14m. In the minimum probably fainter FL Sge |than 15.9m. FO Sge |P var. Max = 2427578.0 + 67.8d*E (JD2427570 - 28120); Max = FO Sge |2428134.4 + 72.7d*E (JD2428120 - 30150); since JD2430150 - see FO Sge |Table. FP Sge |Min II 14.9. P = 0.32100275d? FT Sge |P.K.55-1 {deg} 2. Not a planetary nebula. FU Sge |Min II 15.8. FX Sge |In the region of the globular cluster M71 (NGC 6838). GI Sge |Red. GN Sge |Min II 10.6. GP Sge |Red. GY Sge |P var. Max = 2431264.49 + 51.497d*E (JD2429490 - 34900) [07199]; GY Sge |Max = 2433787.42 + 51.5991d*E (JD2433600 - 37280), Max = 437911.04 GY Sge |+ 51.2524d*E (JD2437280 - 40510) [06172]; since JD2444450 - see GY Sge |Table. HH Sge |The cycles 23 - 26d and 300d are observed. HM Sge |VB A (B 14.20m, 10", 182{deg}). The brightness increased from 17.2m HM Sge |up to 11.3m pg in the interval JD2442280 - 42650. Then the light HM Sge |variations in the infrared region appeared with P = 550d HM Sge |[09721,09783] and A(K) = 1.5m. Radio and X-ray source. IR Sge |SF star in a close pair. LN Sge |SF star in a close pair. MV Sge |Possible member of the globular cluster Palomar 10. MZ Sge |Possible member of the globular cluster Palomar 10. PT Sge |P component of a close pair. V0339 Sge |Extremely metal-weak. V0366 Sge |O'Connell effect. V0370 Sge |MinII - MinI = 0.38P. V0378 Sge |VB A (B 13.7m, 20", 322{deg}, 2000). V0380 Sge |VB AB (10.7m, 10.9m, 0.57", 74{deg}, 1990). V0404 Sge |The light curve shape, including the depth of minima, varies. V0407 Sge |P = 0.086636d is also possible. V0443 Sge |VB A (14.8mG; B 15.35mG, 17", 85{deg}, 2000; C 15.4mG, 18", V0443 Sge |88{deg}, 2000). del Sge |VB A (B, A = 0.04", P = 7 yr); SB2 (Porb = 3725d [09789]). The last del Sge |superior conjunction of the B-star and its atmospheric eclipse was del Sge |in March - April 1980 [09726]. R Sgr |P var. Max = 2405776 + 271.0d*E (JD2399500 - 2407500); Max = R Sgr |2407115 + 264.2d*E (JD2407100 - 9500); Max = 2418125 + 269.65d*E R Sgr |(JD2409500 - 19500); Max = 2433137 + 267.90d*E (JD2419500 - 36000); R Sgr |since JD2436000 - see Table. S Sgr |P var. Max = 2401029 + 230.6d*E (JD2401000 - 10000); Max = 2411638 S Sgr |+ 229.2d*E (JD2410000 - 19500); Max = 2422222 + 232.81d*E S Sgr |(JD2419500 - 27000); since JD2427000 - see Table. T Sgr |Companion F3IV (ro < 0.8"). P var. Max = 2409013 + 385.1d*E T Sgr |(JD2401500 - 10500); Max = 2414582 + 399.0d*E (JD2413000 - 17500); T Sgr |Max = 2424363 + 387.9d*E (JD2417500 - 25500); since JD2425500 - see T Sgr |Table. S 5/6-e. There are Te lines and a very strong Li {lambda} T Sgr |6708 line in the spectrum. U Sgr |The member of the open cluster M25 (IC 4725). P var. Max = U Sgr |2416628.046 + 6.744925d*E (JD2404480 - 30115) [00765]; since U Sgr |JD2430115 - see Table. [A/H] = 0.1. W Sgr |VB A (A 9.2m, 0.116", 153.3{deg}, 1976.477; B 13.5m, 33.4", W Sgr |233{deg}; C 13.5m, 47.9", 101{deg}). P var. Max = 2403198.39 + W Sgr |7.594695d*E (JD2403100 - 34500); since JD2434500 - see Table. X Sgr |P var. Max = 2410006.22 + 7.01206d*E (JD2403000 - 17000); Max = X Sgr |2424248.11 + 7.01245d*E (JD2417000 - 34500); since JD2434500 - see X Sgr |Table. Y Sgr |In the region of the open cluster M25 (IC 4725). RR Sgr |P var. Max = 2410008 + 336.0d*E (JD2410000 - 17100) [09794]; Max = RR Sgr |2422755 + 332.73d*E (JD2422700 - 32100) [00960]; since JD2432100 - RR Sgr |see Table. OH, H2O emission. RS Sgr |VB A (B 9.65m V, 39.0", 86{deg}). Min II 6.28. RT Sgr |P var. Max = 2412759 + 303.1d*E (JD2412700 - 8300) [00960]; Max = RT Sgr |2425588 + 308.8d*E (JD2422800 - 26700); Max = 2428034 + 303.8d*E RT Sgr |(JD2426700 - 33500); since JD2433500 - see Table. RU Sgr |P var. Max = 2413062 + 242.3d*E (JD2410150 - 16700) [00960]; Max = RU Sgr |2423670 + 242.3d*E (JD2422500 - 24500); Max = 2428200 + 237.6d*E RU Sgr |(JD2424500 - 28800); since JD2428800 - see Table. RV Sgr |P var. Max = 2411206 + 319.3d*E (JD2410200 - 17000) [00960]; Max = RV Sgr |2429032 + 321.3d*E (JD2422600 - 29500); since JD2429500 - see RV Sgr |Table. RW Sgr |P var. Max = 2413798 + 189.0d*E (JD2413700 - 23000); Max = 2431998 RW Sgr |+ 190.87d*E (JD2423000 - 33500); since JD2433500 - see Table. RX Sgr |P var. Max = 2417730 + 330.3d*E (JD2413000 - 18500); Max = 2420122 RX Sgr |+ 346d*E (JD2418500 - 20150); Max = 2420122 + 323d*E (JD2420100 - RX Sgr |22200); Max = 2424120 + 345d*E (JD2422200 - 24200); Max = 2428785 + RX Sgr |332.2d*E (JD2424000 - 31500); since JD2431500 - see Table. RY Sgr |VB A (B 15.69m, 12"). There are pulsational light variations (0.1m RY Sgr |< A < 1.5m) with the elements: Max = 2433670 + 38.6056d*E - RY Sgr |78d*10**(-5)*E**2. light curve [09798,09799]; spectrum description RY Sgr |[06261]. ST Sgr |S 6/3-e. SU Sgr |VB A (B 13.5m, 1.0", 240{deg}, 1932.45). earlier P = 88d was SU Sgr |observed [00017]. SV Sgr |In the nebula M8 (NGC 6523). SW Sgr |P var. Max = 2416338 + 290.3d*E (JD2414000 - 16500); Max = 2428507 SW Sgr |+ 288.5d*E (JD2422500 - 29000); Max = 2429088 + 293.5d*E (JD2429000 SW Sgr |- 33000); since JD2433000 - see Table. SX Sgr |Min II 9.62; d = 0.05P. P var. Min I = 2429114.249 + 4.15395762d*E SX Sgr |(JD2410000 - 29150) [00007]; since JD2429000 - see Table. SY Sgr |In the region of the nebula S188. SZ Sgr |VB A (B 12.5m V, 2.0", 212{deg}.) VV Sgr |In the region of the open cluster NGC 6494. OH, H2O emission. VX Sgr |P var; 1m <= A <= 6m. SIO, H2O, OH maser. Light curve (1935-1969) VX Sgr |[06615]. VY Sgr |[A/H] = 0.5. WX Sgr |VB A (B 12.5m, 0.4", 88{deg}). P var. Min = 2419317.259 + WX Sgr |2.129095d*E (JD2419300 - 24700) [00457]; Min = 2424729.418 + WX Sgr |2.129113d*E (JD2424700 - 39700) [00279]; since JD2440000 - see WX Sgr |Table. WY Sgr |Min II 10.3. WZ Sgr |The member of the open cluster C 1814-190. [A/H] = 0.4. XX Sgr |P var. Max = 2419189.730 + 6.424264d*E (JD2419100 - 30100) [00637]; XX Sgr |since JD2435000 - see Table. XZ Sgr |Min II 8.95; d = 0.022P. P var. Min I = 2420311.519 + 3.275537d*E XZ Sgr |(JD2420300 - 28000) [01604]; Min I = 2436440.137 + 3.27549d*E XZ Sgr |(JD2428000 - 37500) [02516]; Min I = 2441150.348 + 3.2755357d*E XZ Sgr |(JD2437500 - 41500) [07084]; since JD2441500 - see Table. YY Sgr |Min II 10.64; Min II = 2433075.8296 + 2.628463d*E [02302]. Apsidal YY Sgr |motion period is about 300 years. AL Sgr |P var. Max = 2425792 + 79.07d*E (JD2421000 - 26000); since AL Sgr |JD2426000 - see Table. AN Sgr |P var. Max = 2425720 + 339.62d*E (JD2415000 - 26000); Max = 2428360 AN Sgr |+ 330.0d*E (JD2426000 - 28500); since JD2428500 - see Table. AP Sgr |SB? [09004]. AR Sgr |There is a square term in the elements: -[0.0031d (E-30)**2 + AR Sgr |8.8d]. AS Sgr |Planetary nebula HB6 = 7 + 1{deg} 1. AU Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 AU Sgr |(M20). AV Sgr |In the region of the open cluster NGC 6546. Not a member of the AV Sgr |cluster. [A/H] = 0.4. P var. Max = 2429083.30 + 15.4093d*E AV Sgr |(JD2421400 - 39100); since JD2439100 - see Table. AW Sgr |VB A (B 16m, 15", 97{deg}). In the region of the open cluster NGC AW Sgr |6546. AY Sgr |[A/H] = 0.2. BB Sgr |VB A (B = V4088 Sgr, 7.49m - 7.87m, 93.5", 102{deg}). In the region BB Sgr |of the open cluster Cr394. BE Sgr |A var (0.6m <= A <= 1.1m). BM Sgr |P var. BN Sgr |Min II 9.37; d = 0.04P:. Soft X-ray source. P var [01600]. BQ Sgr |d = 0.017P. P var. Min = 2412592.7905 + 8.01964d*E (JD2412590 - BQ Sgr |22220) [01696]; since JD2422220 - see Table. CC Sgr |In the region of the globular cluster NGC 6723. CD Sgr |In the region of the globular cluster NGC 6723. P var. Max = CD Sgr |2416247 + 266.62d*E (JD2411000 - 23000); since JD2423000 - see CD Sgr |Table. CE Sgr |In the region of the globular cluster NGC 6723. SF component of a CE Sgr |close double. CF Sgr |In the region of the globular cluster NGC 6723. P var. Max = CF Sgr |2415632.81 + 0.570026d*E (JD2411000 - 23800) [01616]; since CF Sgr |JD2423900 - see Table. CG Sgr |In the region of the globular cluster NGC 6723. DH Sgr |In the region of the globular cluster NGC 6809 (M55). DI Sgr |In the region of the globular cluster NGC 6809 (M55). DK Sgr |In the region of the globular cluster NGC 6809 (M55). DM Sgr |In the region of the globular cluster NGC 6809 (M55). DO Sgr |In the region of the globular cluster NGC 6809 (M55). DP Sgr |In the region of the globular cluster NGC 6809 (M55). DR Sgr |In the region of the globular cluster NGC 6809 (M55). DS Sgr |In the region of the globular cluster NGC 6809 (M55). DV Sgr |d = 0.044P. EG Sgr |d = 0.010P. FV Sgr |P var. Max = 2424010 + 269.5d*E (JD2424000 - 27500) [00251]; since FV Sgr |JD2427500 - see Table. GG Sgr |P var. Max = 2413840 + 286.5d*E (JD2413800 - 24000); since GG Sgr |JD2424000 - see Table. GK Sgr |According to [05869] - eclipsing. GU Sgr |There are also light variations with P = 37.5d, 0.4m <= A(V) <= GU Sgr |1.5m [06273]. HH Sgr |VB (ro = 0.1'). IR Sgr |VB B (A 13.6m; B 10", 220{deg}). KO Sgr |Similar to UG. It is possible that the observations in Min KO Sgr |brightness refer to a companion. LN Sgr |P = 227.0d? LZ Sgr |VB A (B 16m, 7", 30{deg}). MV Sgr |Very hot hydrogen deficient extreme helium carbon star. MW Sgr |P var. Max = 2418940 + 202.3d*E (JD2418900 - 23900); Max = 2428753 MW Sgr |+ 206.5d*E (JD2423900 - 28950); since JD2428950 - see Table. NP Sgr |The cycles 100 - 300d are possible. OW Sgr |In the region of the open cluster NGC 6716. V0348 Sgr |VB A (B 15m pg, 16", 73{deg}). Very hot hydrogen deficient helium V0348 Sgr |carbon star. By the character of light variation and the spectrum V0348 Sgr |the star is unique. The light curve resembling those of RCB type V0348 Sgr |stars is superimposed by conspicuons irregular and semiregular V0348 Sgr |variations with the mean cycle about 200d [02449,09824]. The star V0348 Sgr |is surrounded by a nebula the radius of which equals 1". A fainter V0348 Sgr |nebulous envelope is observed up to 7" from the star. Large V0348 Sgr |infrared excess. Spectrum description [02451,09825]. Probably the V0348 Sgr |star is intermediate between the RCB variables And planetary nebula V0348 Sgr |Wolf-Rayet central stars. V0350 Sgr |SB [09004]. V0354 Sgr |d = 0.02P. V0356 Sgr |Min II 7.24; DII = 0.20P:; d = 0.05P; 0.490P (1928) <= Min II - Min V0356 Sgr |I <= 0.505P (1951). Apsidal motion is possible. V0366 Sgr |P var. Max = 2425479.448 + 0.4779616d*E (JD2423990 - 28780) V0366 Sgr |[00705]; since JD2435600 - see Table. [Ca/H] = -0.73. V0367 Sgr |[Ca/H] = -1.21. V0377 Sgr |The epoch of light min is given in the Table. P var. Min = V0377 Sgr |2426071.24 + 16.17076d*E (JD2425300 - 26600) [00048]; Min = V0377 Sgr |2427350.25 + 16.19326d*E (JD2426600 - 28700) [01400]; Min = V0377 Sgr |2436358.98 + 16.1575d*E (JD2436200 - 37300); Min = 2437863.09 + V0377 Sgr |16.1925d*E (JD2437660 - 39100); Min = 2440114.81 + 16.2407d*E V0377 Sgr |(JD2440200 - 560); since JD2440950 - see Table. V0397 Sgr |There is a square term in the elements: -0.009d*10**(-6)*E**2 V0401 Sgr |Min II 14.1. V0403 Sgr |There is a nonlinear term in the elements: -0.013d*10**(-6)*E**2. V0410 Sgr |VB A (B 13.6m, 270{deg}). V0426 Sgr |Min II 13.3. V0427 Sgr |There is a nonlinear term in the elements: -131d*10**(-10)*E**2. V0427 Sgr |The shape of the light curve varies: 0.17P <= M - m <= 0.22P. V0431 Sgr |Min II 14.9. V0437 Sgr |Min II 14.0. V0440 Sgr |{Delta}(S) = 9. P var. P = 0.4774659d (JD2416000 - 23000) [00752]; V0440 Sgr |P < 0.4774659d (JD2422000 - 26000) [00235]; Max = 2426581.203 + V0440 Sgr |0.477474d*E (JD2426000 - 29460) [01000]; since JD2437100 - see V0440 Sgr |Table. V0453 Sgr |There is a nonlinear term in the elements: +0.003d*10**(-6)*E**2. V0457 Sgr |There is a nonlinear term in the elements: -0.005d*10**(-6)*E**2. V0466 Sgr |There is a nonlinear term in the elements: +0.03d*10**(-6)*E**2. V0496 Sgr |Min II 14.3. V0497 Sgr |Min II 16.0. V0505 Sgr |Min II 6.63. P var. Min I = 2433515.3295 + 1.18287141d*E (JD2425500 V0505 Sgr |- 35800) [01642]; Min I = 2437494.4964 + 1.1828622d*E (JD2435800 - V0505 Sgr |37500); Min I = 2440055.3991 + 1.1828650d*E (JD2437500 - 40100); V0505 Sgr |Min I = 2442656.5283 + 1.18286917d*E (JD2440100 - 42670); since V0505 Sgr |JD2442670 - see Table. The shape of the light curve varies. V0505 Sgr |Deviations from the mean light curve vary with P = 310d. The V0505 Sgr |difference of Min I and Min II depths varies by 0.05m [09830]. V0511 Sgr |P var. Max = 2423950 + 158.8d*E (JD2411300 - 23950); since V0511 Sgr |JD2423950 - see Table. V0515 Sgr |There is a nonlinear term in the elements: +0.015d*E**2. V0519 Sgr |There is a nonlinear term in the elements: +0.0046d*E**2. V0520 Sgr |There is a nonlinear term in the elements: +0.051d*E**2. V0523 Sgr |Min II 9.88. Apsidal motion is observed. In the Table the epoch of V0523 Sgr |Min I is given corresponding to the moment of line of apsides V0523 Sgr |coinciding with the line of sight, when Min II - Min I = 0.50P. The V0523 Sgr |mean period according to [02453] is given; with this period O - C V0523 Sgr |deviations do not exceed +-0.06P for both minima. The period of V0523 Sgr |apsidal motion is 248 years [02453]. Min II - Min I = 0.39P in V0523 Sgr |1953. V0524 Sgr |Min II 11.2. V0525 Sgr |Min II 8.51. V0526 Sgr |VB A (B 12.40m, 8.6", 7.3{deg}). Min II 10.20, DII = 0.17P; dI = V0526 Sgr |0.006P, dII = 0.013P. There are periodic terms in the elements: V0526 Sgr |+0.1369d*sin(0.01295{deg}*E) - 0.0115d*sin(0.0259{deg}*E) + V0526 Sgr |0.0011d*sin(0.0388{deg}*E). Min II = 2422055.0453 + 1.919411d*E - V0526 Sgr |0.1369d*sin(0.01295{deg}*E) - 0.0115d*sin(0.0259{deg}*E) - V0526 Sgr |0.0011d*sin(0.0388{deg}*E). The period of apsidal motion is 146 V0526 Sgr |years. e = 0.224. V0527 Sgr |P var. Max = 2426904.95 + 1.258956d*E (JD2425790 - 7650) [01648]; V0527 Sgr |since JD2438200 - see Table. V0551 Sgr |VB B (A 16.5m; B 12", 135{deg}). V0552 Sgr |P var. The elements given in the Table are valid since JD2418400. V0554 Sgr |Min II 14.5. V0557 Sgr |P var. Max = 2415110.5 + 16.233d*E (JD2415100 - 22000); Max = V0557 Sgr |2426100.0 + 16.260d*E (JD2423900 - 27700) [00251]; Max = 2428097.70 V0557 Sgr |+ 16.171d*E (JD2427700 - 28800) [00296]; since JD2428800 - see V0557 Sgr |Table. V0558 Sgr |Min II 14.3. V0564 Sgr |P var. Max = 2424056 + 27.8d*E (JD2423780 - 26000) [00251]; Max = V0564 Sgr |2428403.3 + 27.99d*E (JD2427870 - 29160) [00296]; Max = 2429158.2 + V0564 Sgr |27.2d (JD2429150 - 515); since JD2429515 - see Table. V0567 Sgr |The central star of the planetary nebula P.K.355 -6{deg} 1 (M3-21). V0573 Sgr |Min II 12.7. V0574 Sgr |Min II 14.7. V0578 Sgr |According to [02448], Max = 2428710 + 253d*E. V0593 Sgr |P var. Max = 2414150 + 230d*E (JD2414100 - 22900); since JD2423900 V0593 Sgr |- see Table. V0598 Sgr |d = 0.05P. V0611 Sgr |P var. Max = 2414150 + 123d*E (JD2414150 - 19000); since JD2420250 V0611 Sgr |- see Table. The period must probably be doubled because the star V0611 Sgr |resembles RV Tau (Min II 16.2). V0612 Sgr |P var. Max = 2413750 + 107.9d*E (JD2413700 - 17900); since V0612 Sgr |JD2418800 - see Table. V0615 Sgr |P.K.356 -7{deg} 1 = He 2-349. V0626 Sgr |P var? Max = 2427715.4 + 26.745d*E (JD2425380 - 28800) [00046]; V0626 Sgr |since JD2434500 - see Table. V0631 Sgr |Min II 14.2. V0632 Sgr |P var. Max = 2413350 + 263d*E (JD2413300 - 19000); since JD2420200 V0632 Sgr |- see Table. V0633 Sgr |P var. Max = 2415110 + 224d:*E (JD2415000 - 18800); since JD2420000 V0633 Sgr |- see Table. V0638 Sgr |P var? Max = 2412670 + 73.1d*E (JD2412600 - 14540); since JD2414800 V0638 Sgr |- see Table. V0646 Sgr |P var. Max = 2413350 + 95d*E (JD2413300 - 15900); since JD2423900 - V0646 Sgr |see Table. V0655 Sgr |P = 213.0d? The coordinates given in [05869] are erroneous. V0660 Sgr |P var. Max = 2426460 + 235.6d*E (JD2426400 - 35700) [00251]; since V0660 Sgr |JD2435600 - see Table. V0663 Sgr |P var. Max = 2426160 + 305d*E [00251]; since JD2435600 - see Table. V0671 Sgr |P = 292.5d? V0672 Sgr |P var? Max = 2424680 + 228d*E [00251]; since JD2435600 - see Table. V0674 Sgr |P var. Max = 2425830 + 249d*E [00251]; since JD2435600 - see Table. V0675 Sgr |(k - b)2 = -0.01; {Delta}(S) = 11. V0676 Sgr |P var. Max = 2414140 + 181d*E (JD2414100 - 22600) [00251]; since V0676 Sgr |JD2423900 - see Table. V0679 Sgr |P var. Max = 2415900 + 225d*E (JD2415900 - 22200) [00251]; Max = V0679 Sgr |2425440 + 223.1d*E (JD2425000 - 29000); since JD2429000 - see V0679 Sgr |Table. V0683 Sgr |Min II 12.5. V0686 Sgr |P var? Max = 2425390 + 225.3d*E [00251]; since JD2435600 - see V0686 Sgr |Table. V0687 Sgr |Min II 12.2. V0691 Sgr |P var? Max = 2426095.550 + 0.46911d*E [00251]; since JD2435630 - V0691 Sgr |see Table. V0703 Sgr |Var 4. According to [02951] the range of light variation, the type V0703 Sgr |of variability and the elements of light variation are erroneously V0703 Sgr |assigned in [01640] to the star Var 3. V0705 Sgr |Min II 12.9. V0710 Sgr |P var. Min = 2426101.550 + 2.3817d*E [00251]; Min = 2431286.425 + V0710 Sgr |2.381633d*E (JD2428390 - 35700) [03513]. V0713 Sgr |P var? Max = 2424680 + 253.4d*E [00251]; since JD2435600 - see V0713 Sgr |Table. V0716 Sgr |P var? Max = 2424670 + 277d*E [00251]; since JD2435600 - see Table. V0718 Sgr |P var? Max = 2425850 + 153.2d*E [00251]; since JD2435600 - see V0718 Sgr |Table. V0721 Sgr |P = 71:d? V0725 Sgr |Unique star. The mean brightness increased from 13.0m to 12.4m V0725 Sgr |since 1889 to 1915, and fell to 12.8m in 1926. From 1895 to 1926 V0725 Sgr |real shortperiodic oscillations with the amplitude about 0.4m. In V0725 Sgr |1928 the amplitude suddenly increased by almost 2m, but the V0725 Sgr |magnitude in maximum remained unchanged. From 1928 to 1935 the V0725 Sgr |light variations became periodic, the period increasing every year V0725 Sgr |by 1d in accordance with the formula: Min = 2426087 + 15.933d*E + V0725 Sgr |0.0233d*E**2. In 1935 P = 21d. Since 1936 only small oscillations V0725 Sgr |of brightness with a gradual increase of the mean magnitude from V0725 Sgr |14.3m to 13.9m B (1969). Photoelectric observations in 1968 - 69 V0725 Sgr |reveal the light variations 12.33m - 12.72m V with possible periods V0725 Sgr |15.4d in 1968 and 45.3d in 1969. In 1973 12.28m - 12.58m V, B-V = V0725 Sgr |+1.37, P = 50d [07101]. V0727 Sgr |VB A (B = V728 Sgr, 14.7m - 15.9m, 25", 108{deg}). V0728 Sgr |VB B (A = V727 Sgr, B 25", 108{deg}). V0734 Sgr |Min II 13.1. V0735 Sgr |VB A (B 15.5m, 6", 315{deg}). According to B-V, U-B values and V0735 Sgr |spectrum the star is not a UG type variable [09840]. V0738 Sgr |In the region of the globular cluster NGC 6558. According to V0738 Sgr |[05403], RV? P = 86.78d? V0743 Sgr |Min II 14.2. V0745 Sgr |P var. Max = 2416560 + 385.1d*E (JD2411000 - 19260); since V0745 Sgr |JD2419260 - see Table. V0748 Sgr |Min II 14.7; d = 0.04P. V0750 Sgr |d = 0.02P:. V0752 Sgr |Min II 12.7. V0755 Sgr |d = 0.01P. V0757 Sgr |Min II 13.8; d = 0.06P. V0760 Sgr |Min II 13.4. P var. Min = 2414059.5 + 45.10d*E (JD2412800 - 19000); V0760 Sgr |since JD2419000 - see Table. V0761 Sgr |Min II 12.8; d = 0.05P. V0762 Sgr |P var. Max = 2414100 + 461d*E (JD2411000 - 22860); since JD2422860 V0762 Sgr |- see Table. V0763 Sgr |P var. The observations are satisfied by the given elements since V0763 Sgr |JD2415000. V0766 Sgr |d = 0.05P. V0768 Sgr |Min II 13.0. V0770 Sgr |Min II 13.1. V0773 Sgr |[A/H] = 0.1. V0777 Sgr |d = 0.055P. V0778 Sgr |Min II 12.1. V0779 Sgr |Min II 12.0. V0780 Sgr |Min II 12.9; d = 0.08P. V0782 Sgr |d = 0.045P. V0784 Sgr |Min II 12.8. V0786 Sgr |d = 0.025P. V0789 Sgr |In the region of the open cluster Tr 31. P = 5.10470d (Min II V0789 Sgr |12.7)? [00478]. V0791 Sgr |d = 0.03P:. V0792 Sgr |Min II 12.2. In the region of the open cluster and the diffuse V0792 Sgr |nebula NGC 6514 (M 20). V0793 Sgr |P var. Max = 2412610 + 195d*E (JD2412600 - 19400); since JD2423400 V0793 Sgr |- see Table. V0794 Sgr |P var. Min I = 2413723 + 173.48d*E (JD2413700 - 23750); since V0794 Sgr |JD2423750 - see Table. V0801 Sgr |Min II 14.9. V0802 Sgr |[A/H] = -0.4. V0803 Sgr |P = 3.771748d? V0818 Sgr |The shape of the light curve varies. V0819 Sgr |P var? V0824 Sgr |Min II 15.2. V0828 Sgr |There is a close companion. V0838 Sgr |P var? V0839 Sgr |P var? Max = 2426170.126 + 1.835347d*E (JD2425700 - 26600) [01598]; V0839 Sgr |since JD2441500 - see Table. V0841 Sgr |The shape of the light curve varies. V0844 Sgr |P var? V0845 Sgr |Min II 14.6. V0859 Sgr |The shape of the light curve varies. V0879 Sgr |There is a close companion. V0882 Sgr |Min II 14.6. V0884 Sgr |0.20P <= M - m <= 0.40P. Blazhko effect. V0889 Sgr |0.14P <= M - m <= 0.24P. Blazhko effect. V0902 Sgr |Min II 14.8. V0903 Sgr |Min II 13.0. V0919 Sgr |Spectrum description [09845]. V0935 Sgr |P var. Max = 2420040 + 232.0d*E (JD2419500 - 28650); since V0935 Sgr |JD2428600 - see Table. V0938 Sgr |P = 138.27d? V0960 Sgr |nP = 1734d. V0966 Sgr |Min II 14.0. V0977 Sgr |d = 0.03P. V0981 Sgr |Min II 14.8. V0985 Sgr |Min II 14.3. V0986 Sgr |d = 0.015P. V0993 Sgr |dI = 0.05P:; Min II 13.7, DII = 0.09P, dII = 0.00P. V0994 Sgr |Min II 12.8:. V0998 Sgr |The depth of Min II 0.04m:. V1000 Sgr |Min II 13.9. V1002 Sgr |Min II 13.7. V1004 Sgr |[A/H] = -0.2. V1005 Sgr |Min II 13.9. V1013 Sgr |Min II 15.0. V1017 Sgr |VB B (A 10.6m V; B 15", 270{deg}). For a long time the star was V1017 Sgr |considered to be a recurrent nova. Three considerable flares were V1017 Sgr |observed: in 1901 (10.8m), 1919 (6.2m), and 1973 (10.5m). Composite V1017 Sgr |spectrum with a trace of a hot component [03872]. V1023 Sgr |In the region of the open cluster Cr 394. Min II 13.0:. V1026 Sgr |Min II 13.4. V1028 Sgr |Min II 14.4. V1032 Sgr |Min II 15.0. V1033 Sgr |The shape of the light curve varies. Blazhko effect? V1034 Sgr |d = 0.025P:. V1056 Sgr |Min II 14.1. V1063 Sgr |The shape of the light curve strongly varies. Blazhko effect? V1068 Sgr |Min II 15.4. V1069 Sgr |The shape of the light curve strongly varies. Blazhko effect? V1071 Sgr |P = 1.3560996d? V1072 Sgr |The shape of the light curve strongly varies. Blazhko effect? V1080 Sgr |P var. The shape of the light curve varies. V1081 Sgr |P var? V1089 Sgr |Cycle <= 30d. V1100 Sgr |d = 0.02P:. V1108 Sgr |Min II 11.9; Min II - Min I = 0.516P. V1109 Sgr |Min II 14.5. V1127 Sgr |There is a nonlinear term in the elements: +78.10d**(-10)*E**2. V1136 Sgr |d = 0.020P. V1148 Sgr |In the region of the globular cluster NGC 6553. V1153 Sgr |P var? Max = 2428391.266 + 1.332624d*E (JD2427680 - 30910); since V1153 Sgr |JD2435630 - see Table. V1177 Sgr |Min II 11.4. V1178 Sgr |d = 0.03P:. V1180 Sgr |[A/H] = -0.4. V1181 Sgr |[A/H] = 0.6. P var. Max = 2428452.25 + 21.341d*E (JD2427400 - V1181 Sgr |31000) [01638]; since JD2433000 - see Table. V1185 Sgr |[A/H] = -0.5. P var. Max = 2428778.86 + 13.9123d*E (JD2427500 - V1185 Sgr |32750) [01638]; Max = 2437485.4 + 13.901345d*E (JD2437100 - 43760) V1185 Sgr |[08519]; since JD2444000 - see Table. V1187 Sgr |[A/H] = -0.8. V1188 Sgr |[CA/H] = -0.37. V1189 Sgr |[A/H] = -1.1. V1190 Sgr |P = 3.000078d? V1191 Sgr |Min II 14.4. V1205 Sgr |The alternative period is possible: 0.659820d [01638]. V1209 Sgr |A var. V1211 Sgr |{Delta}(S) = 3:. V1214 Sgr |There is a nonlinear term in the elements: -0.25d*10**(-7)*E**2. V1216 Sgr |{mu} = 0.720", P = 106.7{deg}. V1223 Sgr |As a rule has a persistent high state; five drops by two to more V1223 Sgr |than three magnitudes have been registered and a twelve year V1223 Sgr |interval of irregular variations at intermediate magnitudes. V1223 Sgr |According to [09850] there are slow variations in brightness by V1223 Sgr |0.15m on a time scale of ~1 day. They are superimposed by V1223 Sgr |variations with the orbital period P orb (Max = 2444749.9866 + V1223 Sgr |0.140239d*E) and with amplitude up to 0.15m. These variations in V1223 Sgr |their turn are superimposed by the others: with P = 794.38s and the V1223 Sgr |amplitude from 0.03m up to 0.15m (Max = 2444750.00404 + V1223 Sgr |0.009194215d*E and (sometimes) with P = 849.8s and a twice smaller V1223 Sgr |amplitude (Max = 2444750.00350 + 0.00983588d*E). Besides there are V1223 Sgr |rapid brightness variations on time scales 10 - 100s by 0.10m - V1223 Sgr |0.20m, and high frequency flickering by 0.05m. According to V1223 Sgr |[09851], the period of X-ray pulses associated with the rotation of V1223 Sgr |the compact object is 12.5 minutes. V1276 Sgr |Min II 14.3. V1280 Sgr |Brightness of Max varies by 2m with the period 5230d. V1281 Sgr |The light variation is not strictly periodic. V1282 Sgr |P var. Min = 2427651.297 + 1.754574d*E (JD2427650 - 30560) [00705]; V1282 Sgr |since JD2435600 - see Table. V1284 Sgr |Min II 13.5. EB? V1287 Sgr |Var 3. According to [02951] the range of light variation of Var 4 V1287 Sgr |(V703 Sgr), the type of variability and the elements of light V1287 Sgr |variation of Var 4 (V703) are erroneously assigned in [01640] to V1287 Sgr |the star Var 3. According to [02951] the range of light variation, V1287 Sgr |the type of variability and the elements of light variation are V1287 Sgr |erroneously assigned in [01640] to the star Var 4. Min II 14.8. V1290 Sgr |[A/H] = -1.2. V1303 Sgr |[A/H] = -0.8. P var? Max = 2438241.176 + 18.46812d*E (JD2427700 - V1303 Sgr |38250) [00001]; since JD2444000 - see Table. V1304 Sgr |[A/H] = 0.3. P var. Max = 2428758.10 + 12.9287d*E (JD2427590 - V1304 Sgr |28820) [01640]; since JD2435600 - see Table. V1309 Sgr |Not far from V4032 Sgr. V1311 Sgr |V 14 in the globular cluster NGC 6656 (M22). Not a member of the V1311 Sgr |cluster. V1312 Sgr |P var? Max = 2428815.600 + 0.6011427d*E (JD2427590 - 28820) V1312 Sgr |[01640]; since JD2435630 - see Table. V1314 Sgr |P var? Max = 2428346.536 + 0.657489d*E (JD2427600 - 28820) [01640]; V1314 Sgr |since JD2435630 - see Table. V1317 Sgr |P var? V1327 Sgr |SR?, L? [08424]. V1328 Sgr |P = 0.39937d? V1329 Sgr |VB B (A 17.2m; B 1.4", 120{deg}). P var. Max = 2432388.777 + V1329 Sgr |0.48306d*E (JD2431670 - 32740) [03524]; since JD2443300 - see V1329 Sgr |Table. V1331 Sgr |Min II 16.5. V1352 Sgr |P var. Max = 2431998.851 + 0.49505d*E (JD2431670 - 33150) [01680]; V1352 Sgr |Max = 2443341.844 + 0.49493d*E (JD2443300 - 350); Max = 2444087.558 V1352 Sgr |+ 0.49516d*E (JD2444050 - 110); in the interval JD2444400 - 410 - V1352 Sgr |see Table. V1356 Sgr |Min II 18.0:. V1357 Sgr |Min II 19.0. V1359 Sgr |P var? V1369 Sgr |P var. Max = 2432736.821 + 0.52956d*E (JD2431670 - 33150) [03524]; V1369 Sgr |since JD2440700 - see Table. V1374 Sgr |{Delta}(S) = 1. V1378 Sgr |{Delta}(S) = -3:. V1387 Sgr |{Delta}(S) = 3. V1389 Sgr |The epoch of Min brightness is given. V1390 Sgr |Min II 17.6. V1392 Sgr |P var. Max = 2432739.791 + 0.55032d*E (JD2431670 - 33150) [03524]; V1392 Sgr |since JD2440700 - see Table. V1393 Sgr |{Delta}(S) = 3. V1394 Sgr |Min II 18.0. V1401 Sgr |The epoch of Min brightness is given. V1405 Sgr |P var. Max = 2432031.778 + 0.46511d*E (JD2431670 - 33150) [06094]; V1405 Sgr |since JD2443300 - see Table. V1408 Sgr |A var (0.5m <= A <= 1.4m). V1409 Sgr |P var. Max = 2432739.822 + 0.65159d*E (JD2431670 - 33150) [03524]; V1409 Sgr |since JD2443300 - see Table. V1412 Sgr |The epoch of Min brightness is given. V1415 Sgr |P var? V1416 Sgr |{Delta}(S) = 3. P var? Max = 2432002.875 + 0.42767d*E (JD2431670 - V1416 Sgr |33150) [06094]; since JD2440700 - see Table. V1418 Sgr |P var. Max = 2432740.818 + 0.45423d*E (JD2431670 - 33150) [03524]; V1418 Sgr |since JD2440700 - see Table. V1419 Sgr |P var. Max = 2432061.669 + 0.57144d*E (JD2431670 - 33150) [01680]; V1419 Sgr |since JD2440700 - see Table. V1425 Sgr |Min II 18.8. V1426 Sgr |{Delta}(S) = 1.5. V1429 Sgr |The epoch of Min brightness is given. V1435 Sgr |Min II 18.0; Min II - Min I = 0.53P. V1437 Sgr |V8 (NGC 6522); not a member of the globular cluster. V1438 Sgr |V9 (NGC 6522); not a member of the globular cluster. V1439 Sgr |P = 0.53711d? [06094]. V1443 Sgr |Min II 18.6. V1446 Sgr |Min II 18.0. V1447 Sgr |Min II 18.2. V1454 Sgr |Min II 15.4. V1457 Sgr |Min II 19.0. V1459 Sgr |The depth of Min II is 0.04m. V1460 Sgr |P var. Max = 2432067 + 162.0d*E (JD2431670 - 33150) [01680]; since V1460 Sgr |JD2440340 - see Table. V1464 Sgr |{Delta}(S) = 1. V1465 Sgr |P var. Max = 2431702.660 + 0.45757d*E (JD2431700 - 940); Max = V1465 Sgr |2432706.945 + 0.45757d*E (JD2431940 - 32740) [03524]; since V1465 Sgr |JD2440740 - see Table. V1466 Sgr |The epoch of Min brightness is given. V1473 Sgr |According to [08424] P = 340d. V1487 Sgr |Min II 18.8. V1491 Sgr |Min II 18.5. V1498 Sgr |SP component of a close pair. P var. Max = 2432739.728 + 0.47467d*E V1498 Sgr |(JD2431670 - 33150) [06094]; since JD2443300 - see Table. V1508 Sgr |VB. V1509 Sgr |Min II 18.1:. V1510 Sgr |According to [06094], P = 0.48546d. V1516 Sgr |P var? Max = 2432740.753 + 0.49709d*E (JD2431670 - 33150) [03524]; V1516 Sgr |since JD2440700 - see Table. V1517 Sgr |P < 2.0d. V1523 Sgr |P var? Max = 2432417.702 + 0.36202d*E (JD2431670 - 33150) [03524]; V1523 Sgr |since JD2443300 - see Table. V1526 Sgr |Min II 18.3. V1537 Sgr |Min II 17.4; Min II - Min I = 0.54P. V1540 Sgr |According to [08424], P = 465d. V1546 Sgr |The epoch of Min brightness is given. V1550 Sgr |P = 0.37432d? [06094]. V1554 Sgr |Min II 17.5. V1557 Sgr |{Delta}(S) = 8. V1558 Sgr |{Delta}(S) = 1. V1559 Sgr |The depth of MinII is 0.04m. V1561 Sgr |Min II 17.7. V1567 Sgr |Min II 18.0. V1569 Sgr |Min II 18.6. V1576 Sgr |[Ca/H] = -1.23. V1577 Sgr |P var. Max = 2426200 + 290d*E (JD2426000 - 30560) [02449]; since V1577 Sgr |JD2430560 - see Table. V1580 Sgr |P var (310d <= P <= 365d). V1589 Sgr |[Ca/H] = -0.91. V1602 Sgr |d = 0.03P. V1610 Sgr |P < 0.5d. V1639 Sgr |The shape of the light curve varies. V1640 Sgr |(k -b)2 = 0.24. P var? V1642 Sgr |250d <= P <= 350d. V1643 Sgr |Min II 12.1. According to [05771], RR?, P = 0.34d. V1644 Sgr |The shape of the light curve varies. V1647 Sgr |VB A (B 9.13m, 8", 104{deg}). Min II 7.43, DII = 0.059P, Min II - V1647 Sgr |Min I = 0.262P (JD2441830); Min II = 2441830.55561 + 3.28282227d*E. V1647 Sgr |The apsidal motion period is 592.5 +- 6.5 years. V1648 Sgr |Close VB. Flat Min. V1652 Sgr |Close VB. Flat Min. V1653 Sgr |Close VB. Flat Min. V1656 Sgr |Close VB. Flat Min. V1658 Sgr |P var.Max = 2426560 + 105d*E (JD2417000 - 28000) [00842]; since V1658 Sgr |JD2428000 - see Table. V1660 Sgr |Close VB. Flat Min. V1661 Sgr |Close VB. Flat Min. P var. Max = 2426850 + 275d*E (JD2424000 - V1661 Sgr |26850); since JD2436700 - see Table. V1667 Sgr |P var. Max = 2426560 + 158d*E (JD2417000 - 36000) [00842]; since V1667 Sgr |JD2436000 - see Table. V1668 Sgr |Close VB. Flat Min. V1670 Sgr |A var. P var. The shape of the light curve varies (probably with a V1670 Sgr |period of about 11 years). V1675 Sgr |A possible companion of 16m. V1679 Sgr |Close VB. Flat Min. V1681 Sgr |A possible companion of 16m. V1690 Sgr |A possible companion of 16m. V1691 Sgr |Close VB. Flat Min. P var. Max = 2426520 + 235d*E (JD2417000 - V1691 Sgr |28000) [00842]; since JD2436000 - see Table. V1697 Sgr |A possible companion of 16m. V1698 Sgr |A possible companion of 16m. V1699 Sgr |P var. Max = 2425410 + 203.6d*E (JD2417000 - 27600) [00842]; since V1699 Sgr |JD2436000 - see Table. V1703 Sgr |A possible companion of 16m. V1705 Sgr |P var. Max = 2425860 + 142d*E (JD2417000 - 27000) [00842]; since V1705 Sgr |JD2435800 - see Table. V1711 Sgr |[A/H] = -1.1. P var. Max = 2435365.19 + 30.46d*E (JD2432700 - V1711 Sgr |35400) [02570]; since JD2442200 - see Table. V1714 Sgr |In the region of the open cluster Ruprecht 134. V1721 Sgr |d = 0.03P:. V1723 Sgr |Min II 13.8. V1730 Sgr |Min II 14.8:; d = 0.03P:. V1741 Sgr |In the nebula and the cluster NGC 6530 (M8). Var1. V1743 Sgr |In the nebula and the cluster NGC 6530 (M8). Var2. V1747 Sgr |In the nebula and the cluster NGC 6530 (M8). Var3. V1748 Sgr |In the nebula and the cluster NGC 6530 (M8). Var4. V1749 Sgr |In the nebula and the cluster NGC 6530 (M8). Var6. V1750 Sgr |In the nebula and the cluster NGC 6530 (M8). Var8. V1751 Sgr |In the nebula and the cluster NGC 6530 (M8). Var7. V1752 Sgr |In the nebula and the cluster NGC 6530 (M8). Var13. V1753 Sgr |In the nebula and the cluster NGC 6530 (M8). Var14. V1755 Sgr |In the nebula and the cluster NGC 6530 (M8). Var15. V1758 Sgr |In the nebula and the cluster NGC 6530 (M8). Var16. V1761 Sgr |In the nebula and the cluster NGC 6530 (M8). Var19. V1762 Sgr |In the nebula and the cluster NGC 6530 (M8). Var20. V1764 Sgr |In the nebula and the cluster NGC 6530 (M8). Var23. V1765 Sgr |In the nebula and the cluster NGC 6530 (M8). Var24. V1768 Sgr |In the nebula and the cluster NGC 6530 (M8). Var26. V1769 Sgr |In the nebula and the cluster NGC 6530 (M8). Var27. V1771 Sgr |In the nebula and the cluster NGC 6530 (M8). Var29. V1772 Sgr |In the nebula and the cluster NGC 6530 (M8). Var28. V1773 Sgr |In the nebula and the cluster NGC 6530 (M8). Var31. V1774 Sgr |In the nebula and the cluster NGC 6530 (M8). Var30. V1775 Sgr |In the nebula and the cluster NGC 6530 (M8). Var33. V1776 Sgr |In the nebula and the cluster NGC 6530 (M8). Var36. V1777 Sgr |In the nebula and the cluster NGC 6530 (M8). Var37. V1778 Sgr |In the nebula and the cluster NGC 6530 (M8). Var34. V1779 Sgr |In the nebula and the cluster NGC 6530 (M8). Var40. V1780 Sgr |In the nebula and the cluster NGC 6530 (M8). Var39. V1781 Sgr |In the nebula and the cluster NGC 6530 (M8). Var41. V1782 Sgr |In the nebula and the cluster NGC 6530 (M8). Var44. V1784 Sgr |In the nebula and the cluster NGC 6530 (M8). Var45. V1785 Sgr |In the nebula and the cluster NGC 6530 (M8). Var46. V1786 Sgr |In the nebula and the cluster NGC 6530 (M8). Var48. V1787 Sgr |In the nebula and the cluster NGC 6530 (M8). Var47. V1788 Sgr |In the nebula and the cluster NGC 6530 (M8). Var50. V1789 Sgr |In the nebula and the cluster NGC 6530 (M8). Var51. V1790 Sgr |In the nebula and the cluster NGC 6530 (M8). Var49. Western V1790 Sgr |component of a close pair. V1791 Sgr |In the nebula and the cluster NGC 6530 (M8). Var53. V1792 Sgr |In the nebula and the cluster NGC 6530 (M8). Var55. V1793 Sgr |In the nebula and the cluster NGC 6530 (M8). Var54. V1794 Sgr |In the nebula and the cluster NGC 6530 (M8). Var56. V1795 Sgr |In the nebula and the cluster NGC 6530 (M8). Var58. V1797 Sgr |In the nebula and the cluster NGC 6530 (M8). Var59. V1798 Sgr |In the nebula and the cluster NGC 6530 (M8). Var60. V1800 Sgr |In the nebula and the cluster NGC 6530 (M8). Var61. V1801 Sgr |In the nebula and the cluster NGC 6530 (M8). Var62. V1802 Sgr |In the nebula and the cluster NGC 6530 (M8). Var63. V1803 Sgr |In the nebula and the cluster NGC 6530 (M8). Var64. SP component of V1803 Sgr |a close pair. V1805 Sgr |In the nebula and the cluster NGC 6530 (M8). Var66. V1807 Sgr |In the nebula and the cluster NGC 6530 (M8). Var67. V1808 Sgr |In the nebula and the cluster NGC 6530 (M8). Var68. V1828 Sgr |P var. Max = 2424402 + 12.985d*E (JD2423800 - 36000) [02515]; since V1828 Sgr |JD2436000 - see Table. V1831 Sgr |P var. Max = 2428849.4 + 26.58d*E (JD2427500 - 31270) [02447]; V1831 Sgr |since JD2435630 - see Table. V1843 Sgr |P = 163.7d? [05869]. V1845 Sgr |Flat Min. Close companion? V1864 Sgr |Epoch of light maximum is given. V1869 Sgr |P var. Max = 2434178 + 346d*E (JD2427590 - 34220) [02447]; since V1869 Sgr |JD2435630 - see Table. V1882 Sgr |The shape of the light curve varies. V1891 Sgr |A companion of 16m. V1894 Sgr |V4 (NGC 6637). Possible member of the globular cluster NGC 6637 (M V1894 Sgr |69). V1895 Sgr |P var. Max = 2421065 + 156.0d*E (JD2418850 - 21100); since V1895 Sgr |JD2427600 - see Table. V1900 Sgr |A companion of 15m. V1904 Sgr |A companion of 15m. V1911 Sgr |P var. Max = 2428832.4 + 10.0581d*E (JD2427600 - 34220) [02447]; V1911 Sgr |since JD2435630 - see Table. The shape of the light curve varies? V1925 Sgr |P var? V1942 Sgr |In the region of the open cluster Ruprecht 147. V1945 Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 V1945 Sgr |(M20). V1946 Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 V1946 Sgr |(M20). V1947 Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 V1947 Sgr |(M20). All the published charts for this variable are wrong. V1947 Sgr |According to [09861] the star actually lies 1.1 mm south and 0.8 mm V1947 Sgr |east of "D2" in fugure 3 published in [02428]. V1948 Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 V1948 Sgr |(M20). V1949 Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 V1949 Sgr |(M20). V1950 Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 V1950 Sgr |(M20). V1951 Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 V1951 Sgr |(M20). V1954 Sgr |VB(ro = 2"). P var. There is a nonlinear term in the elements: V1954 Sgr |-4.1313d*10**(-8)*E**2. V1958 Sgr |Min II 14.0. V1962 Sgr |In the region of the open cluster and the diffuse nebula NGC 6618 V1962 Sgr |(M 17). V1963 Sgr |In the region of the open cluster and the diffuse nebula NGC 6618 V1963 Sgr |(M 17). V1966 Sgr |In the region of the open cluster and the diffuse nebula NGC 6618 V1966 Sgr |(M 17). V1969 Sgr |There are three close faint companions (15.8m-16.3m). V1970 Sgr |In the region of the open cluster and the diffuse nebula NGC 6618 V1970 Sgr |(M 17). V1971 Sgr |In the region of the open cluster and the diffuse nebula NGC 6618 V1971 Sgr |(M 17). V1973 Sgr |In the region of the open cluster and the diffuse nebula NGC 6618 V1973 Sgr |(M 17). V1975 Sgr |In the region of the open cluster and the diffuse nebula NGC 6618 V1975 Sgr |(M 17). The presence of a blue companion is possible. V1976 Sgr |In the region of the open cluster and the diffuse nebula NGC 6618 V1976 Sgr |(M 17). V1977 Sgr |In the region of the open cluster and the diffuse nebula NGC 6618 V1977 Sgr |(M 17). V1980 Sgr |Min II 11.7; DII = 0.11P; Min II - Min I = 0.52P. V1996 Sgr |VB. V2003 Sgr |S 5.5/5. In the region of the open cluster M 25 (IC 4725). V2007 Sgr |V 26 (NGC 6656 = M 22). V2008 Sgr |P = 120 - 135d. V2028 Sgr |In the region of the globular cluster NGC 6681 (M 70). V2037 Sgr |A close companion is possible. V2054 Sgr |P > 450d? V2062 Sgr |The chart in [4233] is wrong. V2064 Sgr |VB. Combined brightness of the star and the close companion was V2064 Sgr |estimated. It is not clear which star is variable. V2065 Sgr |NP component of a close binary. V2094 Sgr |P < 0.5d. V2106 Sgr |VB. Combined brightness of the components was estimated. V2148 Sgr |VB. Combined brightness of the components was estimated. The V2148 Sgr |variable is the northern component. V2276 Sgr |P < 30d. V2282 Sgr |Star L. In the region of the open cluster and the diffuse nebula V2282 Sgr |NGC 6514 (M20). Late spectrum. V2283 Sgr |Min II 10.59:. Apsidal motion with P = 560 years [07107]: 0.739P V2283 Sgr |(1898) <= Min II - Min I <= 0.797P (1965). There are periodic terms V2283 Sgr |in the elements given in the Table: +0.5414d*sin(0.006{deg}*(E + V2283 Sgr |45019)) - 0.0995d*sin(0.012{deg}* (E + 45019)) + V2283 Sgr |0.0217d*sin(0.018{deg}*(E + 45019)); Min II = 2438946.7619 + V2283 Sgr |3.4714231d*E - 0.5414d*sin(0.006{deg}* (E + 45019)) - V2283 Sgr |0.0995d*sin(0.012{deg}*(E + 45019)) - 0.0217d* sin(0.018{deg}*(E + V2283 Sgr |45019)). V2284 Sgr |P var. V2313 Sgr |Min II 16.8. V2315 Sgr |P = 0.193d? V2323 Sgr |Blue [08424]. V2341 Sgr |The epoch of Min brightness is given. V2342 Sgr |V 17 (NGC 6626 = M28). The member of this globular cluster. Min II V2342 Sgr |13.5. V2343 Sgr |A close companion of 14.5m. V2346 Sgr |Cycles 50 - 100d. V2349 Sgr |Min II 9.2. V2351 Sgr |Min II 10.31. V2352 Sgr |P var. There is a nonlinear term in the elements: 0.0525d*E**2. V2355 Sgr |In the region of the globular cluster NGC 6637 (M 69). V2358 Sgr |In the region of the globular cluster NGC 6642. V2359 Sgr |In the region of the globular cluster NGC 6637 (M 69). V2360 Sgr |In the region of the globular cluster NGC 6637 (M 69). V2361 Sgr |In the region of the globular cluster NGC 6637 (M 69). V2362 Sgr |A close companion of 15m. V2366 Sgr |P var. There is a nonlinear term in the elements: V2366 Sgr |+0.6815d*10**(-9)*E**2. V2367 Sgr |V28 (NGC 6656 = M22). Not a member of this globular cluster. P = V2367 Sgr |323d? V2378 Sgr |Two close companions of 15.3m and 15.8m. V2389 Sgr |P var? V2391 Sgr |P = 189d? V2413 Sgr |P var. The elements are valid in the interval JD2425440 - 30905. V2416 Sgr |P.K. 7 +1G 2. V2425 Sgr |E? V2442 Sgr |P = 0.5d? V2449 Sgr |Min II 17.4. V2468 Sgr |Blue [08424]. V2471 Sgr |VB B (A 14.6m; B 8", 225{deg}). V2493 Sgr |Blue [08424]. V2506 Sgr |P.K. 3 -4{deg} 6. V2507 Sgr |Min II 14.6. V2508 Sgr |Min II 14.1:. V2509 Sgr |Min II 7.50. V2510 Sgr |The epoch of Min brigtness is given. The elements given in the V2510 Sgr |Table are valid since JD2427440. V2520 Sgr |VB. V2526 Sgr |The epoch of Min brightness is given. P var. Min = 2428699.5 + V2526 Sgr |31.3224d*E (JD2424100 - 31400) [05590]. Since JD2431400 - see V2526 Sgr |Table. V2529 Sgr |Min II 14.5. Twice shorter period is given in [05590]. V2540 Sgr |P var. V2544 Sgr |VB? V2552 Sgr |VB A (B 15.7m). V2553 Sgr |There are two close companions. V2562 Sgr |Northern component of a close pair. The companion is of 16m. V2563 Sgr |P var. V2564 Sgr |P var? V2565 Sgr |VB B (A 12.5m; B 90{deg}). V2566 Sgr |P var. [Ca/H] = -0.52. V2567 Sgr |[Ca/H] = -0.57. V2568 Sgr |P var? V2576 Sgr |P var. Max = 2426200 + 149d*E (JD2423500 - 27000); since JD2433000 V2576 Sgr |- see Table. V2577 Sgr |P var? V2578 Sgr |VB. In the region of the globular cluster NGC 6642. V2579 Sgr |P var. Max = 2429926.251 + 0.5911903d*E (JD2427590 - 34200) V2579 Sgr |[05590]; since JD2435600 - see Table. V2584 Sgr |P var. Max = 2426564.347 + 0.534829d*E (JD2423940 - 33860); since V2584 Sgr |JD2437820 - see Table. V2592 Sgr |In the region of the globular cluster NGC 6656 (M22). V2593 Sgr |P var. Max = 2428780.349 + 0.5123825d*E (JD2427680 - 34200) V2593 Sgr |[05590]; since JD2435600 - see Table. V2594 Sgr |P var. V2598 Sgr |A companion 15.8m. Spectrum description [06495]. V2601 Sgr |P.K. 12 -7{deg} 1. The epoch of Min brightness is given. V2616 Sgr |Min II 13.0. V2617 Sgr |Min II 9.63. V2620 Sgr |P = 185.6d? V2625 Sgr |P = 0.75837d? V2628 Sgr |P = 171d:?/205d:?/256d:?. V2645 Sgr |P var? V2649 Sgr |P = 143d:? V2672 Sgr |P = 196.8d? /204.5d, /255.3d? /315.0d? V2682 Sgr |P = 228.5d? V2687 Sgr |P = 174d:? V2703 Sgr |P = 270d:? V2719 Sgr |SR? V2731 Sgr |P = 147d:? V2732 Sgr |P = 188.6d? V2733 Sgr |P = 244d:? V2736 Sgr |[Ca/H] = -1.45. V2738 Sgr |[Ca/H] = -0.67. V2740 Sgr |P = 269.0d? V2745 Sgr |[Ca/H] = -1.15. V2756 Sgr |P.K. 2 -5{deg} 1. The epoch of Min brightness is given. V2763 Sgr |P = 216d:? V2777 Sgr |[Ca/H] = -0.83. V2783 Sgr |P = 265.0d? V2789 Sgr |P = 255.5d? V2798 Sgr |P = 244.5d? V2816 Sgr |P = 250d:? V2828 Sgr |P = 0.39669d? V2830 Sgr |Cepheid? V2833 Sgr |P = 224.0d? V2834 Sgr |P = 275d:? V2846 Sgr |P = 0.39659d? V2868 Sgr |P = 235.5d? V2876 Sgr |Min II 15.7:. V2877 Sgr |P = 254.5d? V2893 Sgr |P = 250d:? V2900 Sgr |P = 0.49835d? V2905 Sgr |Spectrum description [04452,06495]. V2918 Sgr |P = 197d:? V2937 Sgr |[Ca/H] = -0.75. V2947 Sgr |RV Tau? Cepheid? V2959 Sgr |P = 0.37233d? V2962 Sgr |P = 209.5d? V2967 Sgr |P = 0.68750d? V2996 Sgr |RV Tau? Cepheid? V3004 Sgr |[Ca/H] = -0.76. V3005 Sgr |RV Tau? Cepheid? V3016 Sgr |P var? V3032 Sgr |P = 153d:? V3033 Sgr |The coordinates given in [05869] are erroneous. V3034 Sgr |P = 154d:? V3038 Sgr |P = 252d:? V3052 Sgr |RV Tau? Cepheid? V3062 Sgr |EW? P = 0.59610d? V3065 Sgr |P = 179.8d?/215.5d? V3071 Sgr |P = 291d:? V3072 Sgr |P = 194d:? V3088 Sgr |P = 215d:? V3105 Sgr |[Ca/H] = -0.82. V3106 Sgr |P = 261d:? V3111 Sgr |P = 182.8d? V3127 Sgr |UG? Not red. V3128 Sgr |Nova? Only one Max was observed. V3170 Sgr |[Ca/H] = -0.82. V3175 Sgr |P = 179.8d? V3176 Sgr |P = 197d:? V3179 Sgr |P = 297d:? V3186 Sgr |[Ca/H] = -1.28. V3196 Sgr |RV Tau? Cepheid? V3207 Sgr |P = 237d:? V3239 Sgr |P = 226d:? V3249 Sgr |UG? V3285 Sgr |P = 173.8d /196.2d? V3294 Sgr |P = 121d:? /177d:? V3295 Sgr |P = 197d:? V3335 Sgr |RV Tau? Cepheid? V3353 Sgr |P var? V3356 Sgr |P = 239.5d? V3365 Sgr |P = 197d:? /252d:? V3388 Sgr |P = 125d:? /160d:? V3395 Sgr |P = 159d:? V3412 Sgr |Cepheid? V3433 Sgr |P = 287.0d? V3443 Sgr |P = 177.6d? V3444 Sgr |P = 160d:? V3459 Sgr |P var. The shape of the light curve varies. V3467 Sgr |RV Tau? Cepheid? V3473 Sgr |SR? V3500 Sgr |RV Tau? Cepheid? V3501 Sgr |Min II 15.7:. V3508 Sgr |The member of the open cluster M25 (IC 4725). V3511 Sgr |RV Tau? Cepheid? V3536 Sgr |P = 239.5d? V3537 Sgr |P = 318.0d? V3551 Sgr |P = 165.2d? /201.0d? V3560 Sgr |P = 181d:? V3564 Sgr |Cepheid? V3566 Sgr |P = 249.0d? V3583 Sgr |P = 228.0d? V3588 Sgr |[Ca/H] = -0.69. V3625 Sgr |P = 294d:? V3634 Sgr |P = 145d:? V3645 Sgr |In the region of the open cluster M25 (IC 4725). V3709 Sgr |P = 240.0d? V3718 Sgr |P var. There is a nonlinear term in the elements: V3718 Sgr |+0.865d*10**(-10)*E**2. V3748 Sgr |P = 0.305327d? V3765 Sgr |[Ca/H] = -0.78. V3783 Sgr |In the region of the globular cluster NGC 6681 (M70). V3784 Sgr |P = 176.4d? V3788 Sgr |In the region of the globular cluster NGC 6723. Red. V3791 Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 V3791 Sgr |(M20). V3792 Sgr |VB A (B 8.92m, 13.3", 90{deg}). Min II 6.81. The range of the V3792 Sgr |combined light variation is given in the Table. The shape of the V3792 Sgr |light curve varies. V3804 Sgr |Spectrum description [06495,07099]. V3811 Sgr |P2 = 4d? Spectrum description [07099,09845]. V3817 Sgr |VB A (B 16m). V3819 Sgr |P var. There is a nonlinear term in the elements: +10**(-10)*E**2. V3829 Sgr |A close companion. V3832 Sgr |A close companion. V3834 Sgr |Cepheid or eclipsing? V3837 Sgr |P = 0.565d? [06383]. V3838 Sgr |VB A (B 15.8m). V3841 Sgr |P var. Max = 2431970 + 358d*E (JD2423900 - 33000); since JD2433000 V3841 Sgr |- see Table. V3842 Sgr |A close companion with M2? Spectral class possibly exists. V3843 Sgr |In the region of the globular cluster NGC 6642. V3853 Sgr |V22 (NGC 6656 = M22). The member of this globular cluster. V3855 Sgr |V31 (NGC 6656 = M22). Possible member of the cluster. V3857 Sgr |According to [06278] the spectral class is M8. V3867 Sgr |Under the chart S 4903 is printed erroneously instead of CSV 4309. V3868 Sgr |P var. Max = 2426130 + 270d*E (JD2423900 - 33900); since JD2435700 V3868 Sgr |- see Table. V3874 Sgr |P var. Max = 2436035 + 115.3d*E (JD2426000 - 38000); since V3874 Sgr |JD2438000 - see Table. V3875 Sgr |P var. P = 358d (JD2424000 - 33800); since JD2435000 - see Table. V3876 Sgr |P var. Max = 2430090 + 345d*E (JD2423900 - 32000); Max = 2436830 + V3876 Sgr |358d*E (JD2436000 - 41500) [06279]; since JD2441400 - see Table. V3879 Sgr |VB ({Delta}(m) = 2.6m, ro = 0.6"). V3880 Sgr |OH, SiO, H2O maser. V3885 Sgr |Porb = 0.206d [04939]. Besides the irregular variability V3885 Sgr |high-frequency oscillations are sometimes observed with P1 = 29.0s, V3885 Sgr |P2 = 30.15s and with amplitudes of 0.00028m. In the spectrum there V3885 Sgr |are extremely broad absorption lines of HI and HeI. The Balmer V3885 Sgr |lines have emission components. X-ray source. V3886 Sgr |Type EB? V3893 Sgr |Connected with a ring nebula. V3894 Sgr |Min II 6.37. P var? V3899 Sgr |In the region of the open cluster and the diffuse nebula NGC 6514 V3899 Sgr |(M20). V3900 Sgr |V7 (NGC 6522). Not a member of this globular cluster. V3903 Sgr |The member of the open cluster Collinder 367. In the nebula Simeis V3903 Sgr |188. V3907 Sgr |The epoch of Min brightness is given. V3929 Sgr |P.K.5 -5{deg} 2. V3961 Sgr |SB1 (Porb = 690d [09915]). V4024 Sgr |SB. V4032 Sgr |Not far from V1309 Sgr. V4034 Sgr |Flat Min. Close companion? V4046 Sgr |Flares (11.1m - 12.4m U). V4048 Sgr |Min II 12.6; DII = 0.15P. V4051 Sgr |In the region of the globular cluster NGC 6638. Not a member of the V4051 Sgr |cluster. V4052 Sgr |In the region of the globular cluster NGC 6638. Not a member of the V4052 Sgr |cluster. V4054 Sgr |In the region of the globular cluster NGC 6638. Not a member of the V4054 Sgr |cluster. V4055 Sgr |In the region of the globular cluster NGC 6638. Not a member of the V4055 Sgr |cluster. V4058 Sgr |d = 0.02P V4060 Sgr |P var. Max = 2437846 + 283d*E (JD2436030 - 38970); since JD2438970 V4060 Sgr |- see Table. V4066 Sgr |d ~0.07P. V4067 Sgr |V32 (NGC 6656 = M22). Not a member of the globular cluster. V4068 Sgr |V17 (NGC 6656 = M22). Not a member of the globular cluster. V4069 Sgr |V33 (NGC 6656 = M22). Not a member of the globular cluster. V4390 Sgr |SB2 and speckle binary. V4417 Sgr |The variability may be due to the fainter (B) component. V4429 Sgr |A giant, according to HIPPARCOS data, despite the published V4429 Sgr |luminosity class (V). V4620 Sgr |In the region of the globular cluster NGC 6558. V4955 Sgr |Close to the N of V4521 Sgr, the periods differ considerably. V5099 Sgr |SU UMa-type cv. V5112 Sgr |A symmetrical minimum lasted for several months, with variations V5112 Sgr |also outside it. V5129 Sgr |MinII 15.71. V5157 Sgr |The type was confirmed spectroscopically in [78222]. V5164 Sgr |MinII 13.31. V5325 Sgr |The Mira V3978 Sgr is in 12" to the west. V5400 Sgr |The coordinates are given for BMB 21. BMB 20 5" np. It is not clear V5400 Sgr |which component varies. V5431 Sgr |VB A (B 5" np). It is not clear which component varies. V5521 Sgr |MinII 15.8. V5527 Sgr |MinII 16.9. V5528 Sgr |MinII 17.7. V5533 Sgr |The light curve with P = 0.94741 d in [78022] is not convincing, V5533 Sgr |our period is based on ASAS-3 data. V5535 Sgr |MinII 10.96. V5555 Sgr |A protoplanetary object, rapid irregular brightness variations. V5559 Sgr |A twice shorter period is not excluded. V5565 Sgr |MinII - MinI = 0.41P. V5566 Sgr |VB A (B 7.5mKs, 7", 327{deg}, 1999). The A component looks not V5566 Sgr |round on DSS images, the spectral type M6: [79127] probably refers V5566 Sgr |to an unresolved companion and not to component B. V5569 Sgr |Besides eclipses, complex variations of different nature. V5627 Sgr |A decline from 15.1m to 16.9m was observed between JD 2449800 and V5627 Sgr |2451400. The tabulated light elements are for eclipses in V5627 Sgr |quiescence (Max 16.88m). V5631 Sgr |VB A (B 11.2m, 1".9, 98{deg}, 2002). V5632 Sgr |OH maser. V5633 Sgr |Multiperiodic. V5634 Sgr |X-ray pulses with P = 5.539917s. V5639 Sgr |VB A (B 11.6m, 8", 142{deg}, 2000; several fainter companions). V5640 Sgr |Erroneously called V1592 Sgr in [80502]. V5641 Sgr |Multiperiodic, P2 = 0.203290d. V5644 Sgr |The fundamental period is tabulated; for the first overtone, P = V5644 Sgr |0.34247d. V5649 Sgr |Blended, combined magnitudes are tabulated. Type Mira is not V5649 Sgr |excluded. V5659 Sgr |Blazhko effect, P = 45.69d. V5664 Sgr |Type EW with a twice longer period is possible. V5672 Sgr |VB A (B 5", 35{deg}, 2000). The magnitudes in the Table were V5672 Sgr |influenced by the companion. V5675 Sgr |P = 129d is superposed. V5680 Sgr |VB A (B 14.5mV, 6", 148{deg}, 1996). V5695 Sgr |MinII - MinI = 0.56P. V5697 Sgr |MinII - MinI = 0.59P. V5700 Sgr |VB A (B 3.5" f). V5701 Sgr |Several close companions. V5728 Sgr |VB A (B 2.5" f). V5731 Sgr |VB A (B 2.5" p). V5732 Sgr |VB B (A 2" np). V5743 Sgr |Several close companions. V5745 Sgr |VB A (B 2" np). V5759 Sgr |SB, Porb = 671d. V5760 Sgr |VB B (A 2.5" nf). Eclipses: 16.9m - 17.2m, MinII 17.1m. A V5760 Sgr |brightening to 15.0m, of unclear nature, was observed on JD2453050 V5760 Sgr |- 2453170. V5779 Sgr |Main wave: amplitude about 1.2m; long wave: P = 1566d, amplitude V5779 Sgr |about 3m. V5815 Sgr |VB A (B 11.9, 8", 235{deg}, 2000). V5824 Sgr |VB A (B 13.0m, 7", 69{deg}, 1999). V5825 Sgr |VB A (B = V2790 Sgr, 13", 271{deg}, 1980; also other companions). V5830 Sgr |The identification with V1615 Sgr [81002] is wrong. V5833 Sgr |Multiperiodic. Other periods: 0.1345604d; 0.0821122d? V5837 Sgr |Multiperiodic, 5 harmonics detected. V5840 Sgr |SB2. V5845 Sgr |Double-mode pulsations. P1 is given in the Table, P0 = 0.45389d. V5845 Sgr |P1/P0 = 0.7416. V5846 Sgr |VB A (9.53m; B 10.9m, 13", 106{deg}, 1999). The magnitudes in the V5846 Sgr |Table are influenced with the companion. V5847 Sgr |The elements in the Table are for the first overtone. P0 = V5847 Sgr |0.474648d. P1/P0 = 0.7439. V5860 Sgr |P0 is presented in the Table. P1 = 3.37986d; P1/P0 = 0.7009. V5864 Sgr |Blended. P0 is presented in the Table. P1 = 0.832980d; P1/P0 = V5864 Sgr |0.7051. V5867 Sgr |P = 215.3d is superposed. V5874 Sgr |P = 161.7d is superposed. V5875 Sgr |The depth of eclipses varies strongly. V5954 Sgr |VB A (B 4", 22{deg}, 2000). The range is for combined brightness. V5960 Sgr |P = 142d is superposed. V5977 Sgr |P = 138d is superposed. V5980 Sgr |Porb = 1.2664d. V5985 Sgr |P = 97d is superposed. V5995 Sgr |P = 131d is superposed. V6099 Sgr |VB B (A 12mV; AB 4.4", 46{deg}, 2015). V6102 Sgr |P = 95.5d is superposed. V6109 Sgr |VB A (B 14m, 5", 138{deg}, 2000). V6125 Sgr |VB B (A 13m; AB 6", 54{deg}, 2000). V6173 Sgr |P = 163d is superposed. V6298 Sgr |P = 333d is superposed. V6318 Sgr |VB (NW); the SE component (NEXT STAR) 10", 123{deg}, 2000. V6319 Sgr |VB (SE); the NW component (PREVIOUS STAR) 10", 303{deg}, 2000. V6335 Sgr |VB A (B 14.36mG, 5", 2{deg}, 2000; C 14.39mG, 10", 258{deg}, 2000). V6361 Sgr |VB A (B 8", 135{deg}, 2000); the range in the Table can be V6361 Sgr |influenced by the companion. V6386 Sgr |VB A (B 4", 326{deg}, 2000); the range in the Table is for combined V6386 Sgr |brightness. Mira type is not excluded. V6434 Sgr |P = 71.7d is superposed. V6467 Sgr |P = 59d is superposed. V6474 Sgr |P = 119d is superposed. V6490 Sgr |VB A (12.8mG; B 14.3mG, 7", 87{deg}, 2000). V6495 Sgr |Long-term variations with a cycle about 750d are superposed. V6499 Sgr |VB A (B = EH Sgr, 12mV - 17mV, 47", 349{deg}, 2000). V6500 Sgr |VB A (9.5mV; B 9.8mV, 5", 161{deg}, 2000). The range in the Table V6500 Sgr |is for combined brightness. V6501 Sgr |P = 64.7d is superposed. V6502 Sgr |P = 83.0d is also possible. V6508 Sgr |VB C (A 13.3mG; B 13.7mG, 29", 255{deg}, 2000; C 14.99mG, 11", V6508 Sgr |294{deg}, 2000; other companions). V6509 Sgr |Type EW with a twice longer period is also possible. V6515 Sgr |Blazhko effect? V6525 Sgr |Blazhko effect? V6554 Sgr |P1 is presented in the Table. P0 = 0.546995d; P1/P0 = 0.7457. V6560 Sgr |Period varies. V6573 Sgr |Period strongly varies. V6574 Sgr |Period varies. eta Sgr |VB A (B 8.0m, 3.5",105{deg}). mu. Sgr |VB A (B 10.48m, 16.9", 285{deg}; C 13.0m, 25.2", 119{deg}; D 9.69m, mu. Sgr |48.5", 312{deg}; E 9.25m, 50.0", 115{deg}). SB2 (e = 0.4). The mu. Sgr |variability type is EA/GS + ACYG. According to [09922] there are mu. Sgr |also quasiperiodical light variations with the amplitudes 0.08m - mu. Sgr |0.15m and cycles from 16d to 40d. ups Sgr |Min II 4.59. R Sco |V7 (NGC 6093 = M80). Probable field star. P var. Max = 2400518 + R Sco |220.2d*E (JD2400500 - 04000) [00960]; Max = 2404493 + 225.86d*E R Sco |(JD2404000 - 08600); Max = 2409003 + 222.29d*E (JD2408600 - 33300); R Sco |since JD2433300 - see Table. S Sco |V6 (NGC 6093 = M80). Cluster non-member. P var. Max = 2400986 + S Sco |177.00d*E (JD2400900 - 17500); since JD2417500 - see Table. T Sco |4.0" N, 2.7" E from the center of the globular cluster NGC 6093 = T Sco |M80. U Sco |Previous outbursts: 2401646: (1863), 2417343 (1906), 2428342 U Sco |(1936). Y Sco |Since 1972 varies its brightness in the range 12.3m-15.0m Y Sco |irregularly, maxima are unpredictable [08080]. Z Sco |P var. Max = 2425546 + 357.17d*E (JD2412500 - 25600); since Z Sco |JD2430000 - see Table. RR Sco |SiO maser. P var. Max = 2416944 + 284.31d*E (JD2411000 - 18000); RR Sco |Max = 2422828 + 278.09d*E (JD2422800 - 40000); since JD2440000 - RR Sco |see Table. RU Sco |P var. During JD2425000 - 40000 - see Table. RV Sco |VB A (B 13.0m, 5.9", 325{deg}). RW Sco |OH, H2O, SiO maser. RY Sco |P var, nonlinear term: +4.10d*10**(-6)*E**2. [A/H] = 0.2. VB A (B RY Sco |10.70m, F8:, 13.8", 220.5{deg}, 1965; C 11.5m, 2.0", 102{deg}, RY Sco |1964; D 11.43m, 24", 80{deg}). Combined brightness of AC is given. RZ Sco |P var. Max = 2413994 + 161.20d*E (JD2413600 - 22700); Max = 2422858 RZ Sco |+ 155.79d*E (JD2422700 - 28000); Max = 2428156 + 160.29d*E RZ Sco |(JD2428000 - 35000); since JD2437500 - see Table. SV Sco |P var. Max = 2418886 + 258.5d:*E (JD2411600 - 19000); Max = 2424233 SV Sco |+ 252.43d*E (JD2420500 - 28600); Max = 2429055 + 255.9d:*E SV Sco |(JD2428600 - 35000); since JD2437000 - see Table. SY Sco |In the region of the open cluster NGC 6475 = M7. TX Sco |In the region of the open cluster NGC 6475 = M7. Probable cluster TX Sco |member. XX Sco |The elements Max = 2413786 + 152d*E [00031] do not represent the XX Sco |observations from [09447]. AC Sco |According to [00266], CST:, 12.2m - 12.6m pg. AH Sco |OH, H2O, SiO maser. AI Sco |P2 = 966.6d. AL Sco |Min II 11.3. AN Sco |EA type is possible. AP Sco |The chart in [09447] is wrong. AR Sco |According to [07104], T Tau type spectrum. AU Sco |It is assumed that the star, called AU Sco in [00121], is actually AU Sco |NSV 20691. AV Sco |The chart and data in [09447] correspond to another star. BI Sco |VB B (A = GW Sco; B 6", 150{deg}). BM Sco |In the region of the open cluster NGC 6405 = M6. BN Sco |In the region of the open cluster NGC 6475 = M7. Resembles R Cen. BS Sco |d <= 0.03P. According to [00021], SP F8. BT Sco |P var. There is periodic term in the elements given in the Table: BT Sco |+0.05d*sin(176{deg} + 0.0857{deg}*E). Blazhko effect? BV Sco |Doubtful identification in [09447]. CF Sco |Min II 13.8. CK Sco |VB A (B 15m, 14"). CL Sco |The brightness in optical and UV range is modulated according to CL Sco |the elements: Min (pg) = 2427020 + 624.7d*E. Outbursts 1892, 1899, CL Sco |1907, 1926. CP Sco |N /= 4. CQ Sco |[A/H] = -1.4. DX Sco |VB A (B p). EZ Sco |VB A (B 15.6m nf). FQ Sco |VB A (B 16m vis). FU Sco |VB A (B np). Min II 12.7, Min II - MiN I = 0.493P. FV Sco |d = 0.015P. Depth of Min II 0.1m pg. FY Sco |VB A (B 15m, 15", 35{deg}). GG Sco |VB A (B 15m, 8", 45{deg}). GM Sco |The nothern one of the two stars noted on the chart for SVS 1677. GW Sco |VB A (B = BI Sco, 6", 150{deg}). IU Sco |VB A (B 16.4m nf). Max = 2413280 + 69.05d*E (1893 - 1906); during IU Sco |1910 - 1928 - see Table. KO Sco |Rapid variations: A = 1.0m. Slow changes: A = 0.5m, P = 2000d +-. KQ Sco |[A/H] = +0.3. P var? LO Sco |P var? Before JD2419150 Max = 2411500 + 450d*E; since JD2423900 - LO Sco |see Table. The spectrum is later than M5. LR Sco |The spectrum resembles RCrB in Max light [08090]. IR excess. RCB LR Sco |type minima were not observed. OO Sco |In the region of the open cluster TR 29. OQ Sco |The chart in [06286] is wrong. QZ Sco |P var. Before JD2420400 Max = 2412640 + 158d*E; since JD2423900 - QZ Sco |see Table. V0347 Sco |P var. Before JD2418700 Max = 2411500 + 198d*E; since JD2423900 - V0347 Sco |see Table. V0350 Sco |VB A (B 15.0m, 3", 233 {deg}). V0381 Sco |d = 0.046P. V0382 Sco |In the region of the open cluster NGC 6475 = M7. V0385 Sco |In the region of the open cluster CR 338. V0387 Sco |Min II 12.2. V0390 Sco |P var. Before JD2422500 Max = 2420330 + 466d*E; since JD2423900 - V0390 Sco |see Table. V0393 Sco |Min II 8.3. V0400 Sco |Min II 15.0. V0402 Sco |In the region of the open cluster NGC 6475 = M7. V0403 Sco |d ~0.02P. The depth of Min II 0.05m. V0407 Sco |In the region of the open cluster NGC 6475 = M7. V0411 Sco |Min II 14.0. V0412 Sco |Min II 14.8. In the region of the open cluster NGC 6475 = M7. V0420 Sco |In the region of the open cluster NGC 6475 = M7. V0421 Sco |P var. Before JD2418000 Max = 2413830 + 293d*E; since JD2423900 - V0421 Sco |see Table. V0423 Sco |Min II 14.2. In the region of the open cluster NGC 6475 = M7. V0425 Sco |In the region of the open cluster NGC 6475 = M7. V0426 Sco |In the region of the open cluster NGC 6475 = M7. V0429 Sco |In the region of the open cluster NGC 6475 = M7. V0430 Sco |In the region of the open cluster Tr 30. V0432 Sco |In the region of the open cluster Tr 30. V0437 Sco |d = 0.02P. Min II 13.9. V0439 Sco |P var. Before JD2418200 Max = 2413350 + 166.5d*E; since JD2419900 - V0439 Sco |see Table. V0440 Sco |In the region of the open cluster Tr 30. V0446 Sco |P var? before JD2435000 Max = 2434980.1 + 28.6195d. [A/H] = -1.0. V0450 Sco |A = 0.9m pg. V0453 Sco |VB A (B 13.51m, F7V, 13.5", 168{deg}). Min II 6.70. The light curve V0453 Sco |shape var? V0455 Sco |P.K.351{deg} + 3{deg}1. Planetary nebula nature is doubtful. V0455 Sco |Nova-like outbursts separated by several years. V0457 Sco |Min II 11.3. V0460 Sco |d = 0.02P. V0464 Sco |d = 0.03P. V0466 Sco |Min II 13.7. V0467 Sco |P var. P = 2.41354d (1889 - 1903); since 1903 - see Table. V0470 Sco |[A/H] = 0.1. V0471 Sco |Min II 15.2, dII = 0.08P(!). V0472 Sco |d = 0.02P. V0474 Sco |Min II 10.6. V0483 Sco |CI = +3.5m. V0485 Sco |Short term variations are superimposed. V0486 Sco |D >= 4d? P = 1d is possible. In the region of the open cluster NGC V0486 Sco |6383. V0487 Sco |[Fe/H] = -1.67, {Delta}(S) = 9.0. V0490 Sco |Min II 12.5. V0491 Sco |Min II 13.2. V0494 Sco |A var (1.27m - 1.66m B). P var? {Delta}(S) = 2. VB A (B 12.72m y, V0494 Sco |23"). V0495 Sco |Short term variation are superimposed. ({Delta}(m)short = 0.5m +-). V0496 Sco |In the region of the open cluster NGC 6414. d = 0.03P. V0497 Sco |Min II 13.6. V0499 Sco |AII = 0.47m V. Min I - Min II = 0.504P. V0502 Sco |In the region of the open cluster C 1712 - 407. V0507 Sco |The epoch of Max from [00300] contradicts the elements. V0540 Sco |VB A (B 15.2m sp). V0547 Sco |VB B (A 14.2m sf). V0549 Sco |[A/H] = -1.1. V0555 Sco |[A/H] = -0.3. V0562 Sco |Min II 12.1. V0566 Sco |d = 0.01P:. V0567 Sco |VB A (B 13.01m, 10"sp, CD 30"nf). P var. V0568 Sco |d = 0.04P. V0569 Sco |Min II 11.4. V0570 Sco |P var? Unusually broad Max. V0573 Sco |d = 0.06P. In the region of the open cluster Tr 24. V0574 Sco |In the region of the open cluster Tr 24. V0575 Sco |Min II 12.4. V0579 Sco |In the region of the open cluster Tr 24. V0581 Sco |Min II 11.9. V0584 Sco |Min II 13.1. V0585 Sco |d = 0.03P:. V0586 Sco |d = 0.04P. In the region of the open cluster Tr 24. V0588 Sco |d = 0.02P. In the region of the open cluster Tr 24. V0589 Sco |d = 0.05P. In the region of the open cluster Tr 24. V0590 Sco |In the region of the open cluster NGC 6231. V0592 Sco |Min II 13.3. V0593 Sco |d = 0.05P:. V0594 Sco |d = 0.01P. V0603 Sco |d = 0.04P. V0606 Sco |d = 0.07P. V0607 Sco |Min II 10.3. V0609 Sco |Min II 13.7. V0611 Sco |d = 0.04P. Min II 13.7. V0612 Sco |d = 0.05P. V0613 Sco |d = 0.04P. V0616 Sco |Min II 12.4. V0619 Sco |Min II 12.1. V0620 Sco |d = 0.02P. V0621 Sco |d = 0.04P. V0622 Sco |Min II 14.2. V0623 Sco |Long intervals in Max without changes, sometimes becomes faint. V0625 Sco |VB A (B 13.2m sf). Min II 13.5. V0627 Sco |Min II 14.1. V0628 Sco |Min II 12.4. V0629 Sco |Apsidal motion. V0631 Sco |Min II 13.2. V0632 Sco |d = 0.06P. V0633 Sco |Min II 12.2. V0634 Sco |Min II 12.2. V0636 Sco |SB1 (Porb = 1318d). V0638 Sco |d = 0.07P. V0640 Sco |Min II 13.5. V0656 Sco |The chart in [06286] is wrong. V0660 Sco |VB A (B 16.0m s). V0672 Sco |P = 180d is possible. V0674 Sco |VB A (B 15.0m s). V0677 Sco |The chart in [06286] is wrong. V0679 Sco |P = 364d is possible. V0690 Sco |VB A (B 14.40m y, 6", 0{deg}). The range of the combined light is V0690 Sco |given. {Delta}(S) = 4. V0698 Sco |D <= 0.20d, d = 0.043d. V0700 Sco |Min II 10.3. V0701 Sco |Min II 9.05. P var. Min I = 2439329.6657 + 0.76187133d*E (JD2428000 V0701 Sco |- 39400) [07177]; since JD2439400 - see Table. Probable member of V0701 Sco |the open cluster NGC 6383. V0702 Sco |Probable member of the open cluster NGC 6383. V0703 Sco |P0 = 0.1499615d [03521]; P1 - see Table (P var?). Also noted P = V0703 Sco |0.04162025d [03521]. A var (0.23m - 0.46m). Beat phenomenon: Max = V0703 Sco |2436760.249 + 0.497306d*E [03521]. {Delta}(S) = 1. In the region of V0703 Sco |the open cluster NGC 6405 = M6. V0705 Sco |Min II 14.1:. V0706 Sco |Moments of Max from [00046] contradict the tabulated elements. V0706 Sco |According to [04678], A <= 0.05m V during 6 nights. V0708 Sco |In the region of the open cluster NGC 6475 = M7. V0709 Sco |IN the region of the open cluster NGC 6475 = M7. [A/H] = -0.6. V0710 Sco |Min II 14.2. V0711 Sco |In the region of the open cluster NGC 6475 = M7. V0712 Sco |Min II 14.0. V0714 Sco |d = 0.05P:. P may be twice longer. V0717 Sco |[A/H] = 0.9. V0718 Sco |D ~4d. Another Min 2429847 - 849 [00270]. V0720 Sco |In the region of the open cluster NGC 6475 = M7. V0723 Sco |In the region of the open cluster NGC 6475 = M7. At the edge of a V0723 Sco |dark cloud. V0725 Sco |It is assumed that the southern neighbou of the star, called AU Sco V0725 Sco |in [00121], is actually NSV 20691. V0729 Sco |Possibly a Nova. V0732 Sco |P may be twice longer. V0733 Sco |Possibly a Nova. V0734 Sco |Possibly a Nova. V0735 Sco |The light curve shape var. V0738 Sco |d = 0.04P:; Min II 13.4:. In the region of the open cluster NGC V0738 Sco |6475 = M7. V0740 Sco |In the region of the open cluster NGC 6475 = M7. V0741 Sco |There is a red variable close to the coordinates in the discovery V0741 Sco |announcement [02448], but a different star is marked in the chart V0741 Sco |in [02448]. V0749 Sco |P = 410d is possible. V0751 Sco |Erroneously named HV 9160 and CSV 3584 in [02448]. V0756 Sco |Min II 10.7. V0760 Sco |dI = 0.02P; Min II 7.4; DII = 0.2P:, dII = 0.03P. V0761 Sco |IN type is not excluded. V0764 Sco |Min II 9.0. V0805 Sco |Possibly P is twice shorter. V0818 Sco |Sco X-1. SB. Var X-ray and multi-component radio source. Lx/Lbol = V0818 Sco |300 - 1000. The epoch of Min is given for the periodic component of V0818 Sco |the light variation (A ~0.25m). Flickering and flares up to 1m with V0818 Sco |time scale from dozens of seconds to minutes. The mean brightness V0818 Sco |level decreased in the middle of 1960-es by 0.3m-0.4m. The spectrum V0818 Sco |with blue continuum and H, HeI, HeII, CIII, NIII emissions. V0819 Sco |Min II 13.2. V0821 Sco |Min II 14.5. V0822 Sco |VB? Combined brightness. V0827 Sco |Min II 14.1. V0833 Sco |Min II 11.2. V0837 Sco |d ~0.03P:; Min II 14.3. V0838 Sco |Min II 13.4. V0842 Sco |Min II 12.3. V0843 Sco |Min II 10.5. V0848 Sco |Min II 13.1. RRC type with twice shorter period is possible. V0849 Sco |Min II 14.1. V0853 Sco |d = 0.05P; Min II 14.1. V0856 Sco |VB C (A = BS 6000, 6.65m, AO-3III; B 12.55m, 16", 298{deg}; C 44", V0856 Sco |185{deg}; D 11.7m, CD 1.3", 105{deg}, 1945). V0857 Sco |Erroneously labelled "10" (instead of "11") in the chart. V0858 Sco |Erroneously labelled "11" (instead of "10") in the chart. V0861 Sco |SB1. Min II 6.28. Depths of minima var. In the region of the open V0861 Sco |cluster NGC 6231, Cr 316, Tr 24. V0862 Sco |Usually 6.67m - 6.76m. A flare of 40m duration on July 3, 1965. In V0862 Sco |the region of the open cluster NGC 6405 = M6. V0866 Sco |VB ({Delta}(m) ~0.5m, ~1", 200{deg}). m (6370 A) = 11.14m - 12.37m. V0866 Sco |IR excess. V0870 Sco |B-V = +3.38m - +3.52m. In the region of the open cluster NGC 6231. V0877 Sco |Min II 13.1. V0883 Sco |VB A (B 12.60m, 9", 130{deg}). P var? Min = 2438228.315 + V0883 Sco |1.294745d*E (JD2438200 - 40500) [06871]; since JD2440500 - see V0883 Sco |Table. Deep Min II. V0884 Sco |4U 1700-37. LX/Lbol = 0.00007. Eclipsing X-ray source. Eclipse V0884 Sco |duration is variable in the ranges 0.61d <= dx <= 1.10d. The epoch V0884 Sco |of the middle of the X-ray eclipse coinciding with Min II is given. V0884 Sco |X-ray flux var in the scale from seconds till hours. Sometimes a V0884 Sco |periodic modulation with P ~97 Min is present, its amplitude in the V0884 Sco |optical band reaches {Delta}(V) ~0.01m. Min II 6.57; Min I - Min II V0884 Sco |= 0.63P, dI=0.2P. Surrounded by the ring nebula Sh 2. in the region V0884 Sco |of the open cluster NGC 6281. Field star. V0885 Sco |Noticeable Min II. V0889 Sco |The northern component of a triple. V0890 Sco |VB A (B 11.5m, 0.5' n). V0894 Sco |A = 0.6m pg. V0896 Sco |Co-ordinates or the chart may be erroneous. V0900 Sco |In the region of the open cluster NGC 6231. The light curve is a V0900 Sco |sinusoidal wave. Possibly P = 6.20d; 6.85d. V0903 Sco |N96 [02448]. Erroneously identified with V479 Sco. V0906 Sco |In the region of the open cluster NGC 6475 = M7. Probable cluster V0906 Sco |member. VB ({delta}(mV) = 0.8m, 0.1", 111{deg}, 1957). The range of V0906 Sco |the combined light variation is given. Min II 6.21. V0907 Sco |In the region of the open cluster NGC 6475 = M7. Min II 9.2. V0911 Sco |Alternative P = 4.2d. V0913 Sco |Alternative P = 0.976d. IR excess. V0914 Sco |VB ({delta}(mV) = 2m, 3", 200{deg}). Sine wave with P = 2.69d, V0914 Sco |{Delta}(B) = 0.15m (B = 12.91m) [09753]. V0915 Sco |VB A (B 10.43m, WN6, 14", 330{deg}; C 11.40m, 20", 202{deg}; D V0915 Sco |13.96m, 22", 80{deg}, 1973). The brightness decreased from 6.32m to V0915 Sco |6.50m during JD2443680 - 44115. V0917 Sco |VB A (B 17m: sp). The outburst: rise 1930-1936, Max 1936-1938, V0917 Sco |decline 1938-1952. V0919 Sco |In the region of the open cluster NGC 6231. V0920 Sco |In the region of the open cluster NGC 6231. Multiple periodicity: V0920 Sco |P1 - see Table, semiamplitude A1 = 0.0051m; P2 = 0.10765d. A2 = V0920 Sco |0.0046m; P3 = 0.10388d, A3 = 0.00485m; P4 = 0.12137d, A4 = 0.0036m; V0920 Sco |P5 = 0.6929d?, A5 = 0.0028m. V0921 Sco |The star illuminates a nebula. V0922 Sco |Multiple periodicity, superposition of frequencies with amplitudes V0922 Sco |0.0010m - 0.0352m. V0923 Sco |D = 0.32d:. The elements need confirmation. In the region of the V0923 Sco |open cluster NGC 6281. V0924 Sco |B-V var: +1.90, +2.50, Light fluctuations by 0.1m - 0.2m (u, b) in V0924 Sco |several minutes. V0925 Sco |VB A (B ~10", faint, blue). Probable member of the open cluster TR V0925 Sco |27. In Vr possible values of P: 105.3d, 73.0d, 188.7d, 312.5d V0925 Sco |[09950]. V0926 Sco |3U 1735-44 = Sco XR-3. Bursts superimpose small light variations V0926 Sco |with P = 0.18d which is apparently the orbital period [04394]. V0927 Sco |The epoch of Min in U light is given. IR excess. V1195 Sco |MinII 9.01 at phase 0.4. V1196 Sco |Symbiotic spectrum. V1212 Sco |The magnitude in [78189] refers to a different star but the period V1212 Sco |is correct [78040]. V1216 Sco |MinII 10.35. V1225 Sco |MinII 10.25. V1229 Sco |MinII 8.96. V1230 Sco |Erroneously called V719 Sco in [78218]. V1270 Sco |MinII 9.70. V1279 Sco |B - V: +1.23, +1.46. V1286 Sco |Very red, J - K = 1.35 (2MASS). V1292 Sco |MinII - MinI = 0.44P. V1296 Sco |MinII - MinI = 0.56P. V1299 Sco |MinII - MinI = 0.55P. V1300 Sco |A twice shorter period is not excluded. V1301 Sco |MinII - MinI = 0.53P. V1302 Sco |A twice shorter period is not excluded. V1303 Sco |MinII - MinI = 0.34P:. V1305 Sco |VB (9.0m, 11.8m, 1.0", 153{deg}, 1927). V1308 Sco |MinII - MinI = 0.48P. V1317 Sco |One deep fading has been detected. After JD 2454100, a cycle of V1317 Sco |58.4d (amplitude 0.7m) was observed. V1319 Sco |P varies. Before JD 2452258, Max = 2452053.713 + 0.2541756d x E. V1319 Sco |The tabulated light elements are valid after JD 2452258. V1327 Sco |VB (0.3", 5{deg}, 1995). V1331 Sco |In the region of the globular cluster M4. Cluster non-member. V1364 Sco |Multiperiodic. V1414 Sco |OH maser. V1452 Sco |Multiperiodic. V1485 Sco |VB A (B 15.6m, 7", 244{deg}, 1999). V1488 Sco |VB A (9.56mJ; B 9.74mJ, 6", 245{deg}, 1999). V1504 Sco |The long period is about 735d. V1506 Sco |VB A (B 14.04m, 10", 333{deg}, 2000; several other components. V1506 Sco |Second periodicity: P = 0.423350d or twice shorter. V1512 Sco |P2 = 0.058920d. VB AB (10.6, 11.0, 0".5, 204{deg}, 1991). V1517 Sco |Foreground star, globular cluster non-member. V1520 Sco |Foreground star, globular cluster non-member. V1537 Sco |Multiperiodic. VB A (8.1mV; B 12.6mV, 1.9", 231{deg}, 1939). V1544 Sco |It is assumed that there is a typo in the star's declination in V1544 Sco |[81021]. V1547 Sco |Simultaneous presence of two periods. P1 is given in the Table. P2 V1547 Sco |= 2.27816d. V1552 Sco |VB A (B 16.0m, 11", 111{deg}, 2000). V1553 Sco |Double-mode pulsations. The period for the fundamental mode is V1553 Sco |given in the Table. P1 = 0.1470447d. P1/P0 = 0.7978. V1560 Sco |VB A (B 15.0m, 6", 147{deg}, 1999). V1611 Sco |MinII - MinI = 0.65P. V1614 Sco |Several close companions. V1628 Sco |VB B (A 11.2m; AB 15", 220{deg}, 1999). The tabulated magnitude in V1628 Sco |maximum was influenced by component A. V1644 Sco |VB A (B 5", 114{deg}, 1999). V1646 Sco |VB A (B 12.2m, 17", 355{deg}, 1999). V1653 Sco |VB B (A 12.6m; AB 9", 21{deg}, 1998). The magnitude at maximum in V1653 Sco |the Table is for the combined brightness. V1679 Sco |P = 38.8d is superposed. V1695 Sco |VB A (15.5mV; B 15.6mV, 9", 204{deg}, 1999). V1708 Sco |According to [240], the star showed semiregular variations before V1708 Sco |its outburst with a peak-to-peak amptitude about 1m and P = 140.5d. V1712 Sco |Cluster non-member. V1713 Sco |Cluster non-member? alf Sco |ADS 10074 A(B 5.1m, B4Ve, A = 2.9", Porb = 878 yr.). Connected with alf Sco |a nebula. zet 1 Sco |In the region of the open cluster NGC 6231. kap Sco |SB. P2 = 0.205430d. P1 var. Beat phenomenon: Pi = 7.3316d. lam Sco |SB1. Porb = 5.6d? Apuls = 0.02m. Long period light changes: Max = lam Sco |2440376.15 + 10.1605d*E [09761]. One eclipse was found (JD2440690, lam Sco |A ~0.04m) [06388]. mu. 1 Sco |Min II 3.12. sig Sco |VB AA (A 5.5m, 0.37", 96{deg}, 1981, orbital motion?; B 8.45m, sig Sco |B9.5V, 20.1", 273{deg}, 1961); SB1, Porb = 33.06d. P0 var. Max Vr = sig Sco |2420000.1465 + 0.24682815d*E (1918 - 1924) [09953]; Max = sig Sco |2432306.918 + 0.246846d*E (JD2432000 - 37800) [09764]; since sig Sco |JD2437800 - see Table. A0 = 0.036m y. P1 = 0.2396674d, A1 = 0.013m sig Sco |y [09762]. Pbeat = 8.256d = Porb/4 [09957]. Connected with a sig Sco |nebula. R Scl |VB A (B 19.9m, 10", 234{deg}). CO emission. S Scl |P var. Max = 412774 + 367.9d*E (JD2405400 - 20500); Max = 2423035 + S Scl |360.6d*E (JD2421250 - 27740); Max = 2427738 + 370.4d*E (JD2427700 - S Scl |34000) [00960]; Since JD2434000 - see Table. H2O emission. T Scl |P var. Max = 2417400 + 202.26d*E (JD2411300 - 19000); Max = 2420390 T Scl |+ 197.85d*E (JD2419000 - 23600); since JD2423600 - see Table. V Scl |P var. Max = 2414006 + 294.8d*E (JD2411600 - 18200); Max = 2422866 V Scl |+ 297.2d*E (JD2420400 - 35100); since JD2435100 - see Table. X Scl |P var. Max = 2413796 + 258.7d*E (JD2413500 - 22800); since X Scl |JD2422800 - see Table. Y Scl |The cycles 100d: and 300d: are sometimes observed. RT Scl |Min II 10.47. [Fe/H] = -0.75. P var. There is a nonlinear term in RT Scl |the elements given in the Table: -9.04d*10**(-11)*E**2. RU Scl |(k - b)2 = 0.09. A var [03429]. P var. Max = 2425094.4175 + RU Scl |0.4933257d*E (JD2416750 - 25100) [00183]; Max = 2427403.177 + RU Scl |0.4933239d*E (JD2425100 - 30650) [01381]; since JD2430650 - see RU Scl |Table. RW Scl |P var? SV Scl |[Fe/H] = -1.82. P var? Max = 2439468.364 + 0.3773636d*E (JD2427300 SV Scl |- 39500) [05233]; since JD2439850 - see Table. SY Scl |H2O maser. P var? Max = 2426160 + 411d*E [00193]; since JD2440400 - SY Scl |see Table. SZ Scl |Min II 13.68. UY Scl |Near the galaxy NGC 55. UZ Scl |VB A (B 15.81m, 23", 135{deg}); (k - b)2 = 0.14. The shape of the UZ Scl |light curve varies. VV Scl |Min II 8.50. ACV? [08083]. VY Scl |Porb = 0.1662d? [09932]. High and low states of the system are VY Scl |observed. VZ Scl |High and low states of the system are observed [09933]. WZ Scl |There are two oscillations with the periods P1 and P2: P1 = WZ Scl |0.06576d, P2 = 0.095944d, P1/P2 = 0.6854. XX Scl |There are two oscillations with the periods P1 and P2: P1 = XX Scl |0.048898d, P2 = 0.051350d, P1/P2 = 0.95225. AI Scl |There are two oscillations with the periods P1 and P2: P1 = 0.044d, AI Scl |P2 = 0.0931d, P1/P2 = 0.47. AL Scl |Min II 6.20; Min II - Min I = 0.475P; DII = 0.08P. AO Scl |{mu} = 0.46", P = 187{deg}. BC Scl |May be eclipsing. BI Scl |Type E: is also possible. CE Scl |Min II 9.75. CI Scl |MinII - MinI = 0.39P. VB (A 9.50mHp; B 9.82mHp, 0.8", 240{deg}, CI Scl |1991). CM Scl |MinII - MinI = 0.40P. VB (9.0m, 10.8m, 1.0", 111{deg}, 1991). CP Scl |Min II = 13.01. P varies. dP/dt = -0.23x10^(-5) d/yr. CQ Scl |Min II = 12.40. P varies. dP/dt = -0.23x10^(-5) d/yr. CR Scl |Min II = 9.68. P varies. dP/dt = 0.26x10^(-5) d/yr. VB AB (A 9.8m; CR Scl |B 12.7m, 4", 231{deg}, 1975). CT Scl |Min II = 12.08. CX Scl |Light elements for eclipses are tabulated. DSCTC pulsations: P = CX Scl |0.183038d, {Delta} m = 0.11m. CY Scl |Blazhko effect. DE Scl |P1 is presented in the Table; P1/P0 = 0.7448. DI Scl |SB2. R Sct |[Fe/H] = -1. P var. Min I = 2377165 + 142.8d*E (JD2377160 - 9820); R Sct |Min I = 2384885 + 142.6d*E (JD2384890 - 8170); Min I = 2394451 + R Sct |141.4d*E (JD2394450 - 8500); Min I = 2398777 + 142.4d*E (JD2398770 R Sct |- 2404320); Min I = 2404627 + 137.4d*E (JD2404600 - 6410); Min I = R Sct |2406561 + 142.7d*E (JD2406560 - 9065); Min I = 2409742 + 143.6d*E R Sct |(JD2409730 - 12700); Min I = 2412755 + 141.5d*E (JD2412750 - R Sct |16720); Min I = 2417161 + 139.5d*E (JD2417150 - 20790); Min I = R Sct |2421083 + 143.4d*E (JD2421050 - 25170) [09935]; Min I = 2429478 + R Sct |142.8d*E (JD2429000 - 30650) [09938]; Min I = 2432078 + 140.05d*E R Sct |(JD2432000 - 42240) [07596]; Min I = 2442737 + 152.5d*E (JD2442550 R Sct |- 43050); Min I = 2443315 + 138.5d*E (JD2443050 - 44150) [00001]; R Sct |since JD2444150 - see Table. Light curve drawings [09935,09936, R Sct |9937]. Spectrum description [09939,09954]. S Sct |VB A (B 11.9M V, 14.5", 238{deg}; C 12.5m V, 44", 105{deg}). U Sct |Min II 10.31. W Sct |Min II 10.1. X Sct |[A/H] = -0.1. In the region of the open cluster NGC 6639. Y Sct |In the region of the open cluster NGC 6664. Z Sct |[A/H] = 0.3. RS Sct |Min II 10.08. RU Sct |[A/H] = -0.7. P var. There is a nonlinear term in the elements RU Sct |given in the Table: +3.15d*10**(-6)*E**2. RX Sct |Connected with the bright hydrogen nebula YM 13. RY Sct |Min II 9.56. P var? Min I = 2427979.340 + 11.124939d*E (JD2414800 - RY Sct |36100) [00007]; since JD2431200 - see Table. The shape of the light RY Sct |curve varies. RZ Sct |Min II 7.47. P var. There is nonlinear term in the elements given RZ Sct |in the Table: +0.78d*10**(-7)*E**2. SU Sct |P var. Max = 2424324.48 + 1.467713d*E (JD2420700 - 34310); Max = SU Sct |2439678.428 + 1.468753d*E (JD2437100 - 41100) [07806]; since SU Sct |JD2441100 - see Table. TX Sct |CWA? red. TY Sct |[A/H] = -0.3. In the region of the open cluster Tr 35. UZ Sct |[Fe/H] = 0.35. P var. Max = 2435629.5 + 14.7468d*E (JD2423900 - UZ Sct |35700) [02309]; since JD2436000 - see Table. VV Sct |SF component of a pair. VW Sct |P var. Max = 2415887 + 234d*E (JD2411900 - 22210); Max = 2423588 + VW Sct |235d*E (JD2422880 - 27600); Max = 2429468 + 235.1d*E (JD2428750 - VW Sct |34200); since JD2434600 - see Table. VX Sct |d = 0.064P. VZ Sct |Min II 12.0. WY Sct |P var. XY Sct |Min II 14.5. AC Sct |d = 0.024P; Min II 10.2. AE Sct |d = 0.04P. AI Sct |In the region of the open cluster NGC 6705. AN Sct |P var? AP Sct |V2 (NGC 6712). AU Sct |d ~0.03P. BC Sct |Following component of a close double system. The companion - NSV BC Sct |11551. BH Sct |Min II 14.9. BI Sct |VB A (B 16.3m:, 3", 280{deg}; C 16.7m:, 12", 190{deg}; D 16.8m:, BI Sct |18", 45{deg}; E 17.0m:, 6", 350{deg}). BK Sct |Close companion 16.5m sf. BN Sct |d = 0.02P. BP Sct |S 5.5/5.5. BS Sct |Min II 11.07. In the region of the open cluster M11 (NGC 6705). BU Sct |A var. P var. Max = 2425804.625 + 0.42022d*E [01401]; Max = BU Sct |2427928.041 + 0.4202188d*E (JD2427900 - 9440) [01404]; Max = BU Sct |2432770.464 + 0.4201944d*E (JD2432740 - 38290); Max = 2438589.357 + BU Sct |0.4202171d*E (JD2438580 - 40510) [07806]; since JD2440770 - see BU Sct |Table. BX Sct |[A/H] = -0.9. CD Sct |Min II 13.7. CF Sct |d = 0.035P. CH Sct |V7 (NGC 6712). The member of this globular cluster. CK Sct |[Fe/H] = 0.23. CL Sct |May be the period should be doubled? CM Sct |[A/H] = 0.1. CN Sct |[A/H] = -1.5. CO Sct |P var? Resembles RV Tau type variables: if the period is doubled, CO Sct |the neight of max I and the depth of Min II vary. CR Sct |Min II 12.1; DII = 0.071P; Min II - Min I = 0.53P. CT Sct |Min II 11.1. CW Sct |Min II 10.1. DD Sct |One of the components probably varies. DE Sct |Min II 16.3. DG Sct |d = 0.03P:. DL Sct |Min II 15.9. DT Sct |Min II 16.5. DV Sct |Min II 17.8. DW Sct |Min II 16.4. EE Sct |Min II 15.3. EH Sct |Min II 15.0. EK Sct |Min II 16.0. EL Sct |The shape of the light curve varies? EN Sct |Min II 17.2. The different elements are also possible: Min I = EN Sct |2428008.85 + 1.06446d*E. EP Sct |d = 0.04P:; Min II 15.6. EQ Sct |In the region of the open cluster NGC 6631. Min II 12.6:. ER Sct |Min II 9.3; Min II - Min I = 0.506P; DII = 0.14P. EU Sct |VB A (B 17.5m, 6", 45{deg}). EV Sct |[A/H] = -0.4. The member of the open cluster NGC 6664. EW Sct |P0 = 5.8195d (A/2 = 0.27m), P1 = 4.0646d (A/2 = 0.22m); P1/P0 = EW Sct |0.6984. EX Sct |d = 0.025P:. EY Sct |Min II 12.4. In the region of the open cluster NGC 6683. EZ Sct |Min II 12.5. FF Sct |Min II 14.2. FG Sct |Min II 14.70. P var? Min I = 2429017.557 + 0.2705728d*E (JD2427975 FG Sct |- 29520) [01397]; since JD2444700 - see Table. FH Sct |In the region of the open cluster NGC 6694. FK Sct |Min II 14.4:. FL Sct |Min II 13.8. FM Sct |Min II 12.9. FN Sct |In the open cluster NGC 6704. FO Sct |D = 0.22d. FR Sct |Spectrum description [01410]. GI Sct |Min II 14.5. GM Sct |Min II 13.8:. HI Sct |D = 0.29d. HL Sct |Min II 13.4. IS Sct |P < 200d. IT Sct |In the region of the open cluster NGC 6705. LL Sct |sf component of a close pair. LR Sct |V14 (NGC 6712). LU Sct |P2 = 30d. LZ Sct |In the region of the globular cluster NGC 6712. MM Sct |Min II 15.8. MP Sct |V1 (NGC 6712). The member of this globular cluster. [Fe/H] = -0.69. MR Sct |V8 (NGC 6712). P var. Max = 2430885 + 117d*E (JD2427900 - 32400) MR Sct |[04231]; since JD2434900 - see Table. NU Sct |VB A (B 16.6m, 12", 180{deg}). NV Sct |P = 200d? OU Sct |P var. Max = 2427620 + 152d*E (JD2426200 - 32800); since JD2433100 OU Sct |- see Table. PT Sct |There is a close companion, 16.4m. PW Sct |The range of the combined light of the variable and a close PW Sct |companion, which follows, is given in the Table. QU Sct |The variable is also eclipsing one with P = 0.2d and A = 0.7m. V0337 Sct |A close companion (16.2m, <7", 90{deg}). V0340 Sct |Min II 15.6. V0356 Sct |Min II 12.3; DII = 0.10P. V0360 Sct |A close fn companion, 16.4m. V0362 Sct |P = 170d? V0367 Sct |In the open cluster NGC 6649. The light elements with fundamental V0367 Sct |mode period P0 (A0 = 0.54m B) are given in the Table. For the V0367 Sct |first-overtone period P1 (A1 = 0.41m B) Max = 2437435.12 + V0367 Sct |4.38466d*E; P1/P0 = 0.696744. M - m var (0.15 <= M - m <= 0.45). V0369 Sct |In the region of the open cluster NGC 6705 (M 11). There is a V0369 Sct |superposition of the four light oscillations: P1 = 0.240d (A1 = V0369 Sct |0.044m), P2 = 0.220d (A2 = 0.020m), P3 = 0.182d (A3 = 0.068m), P4 = V0369 Sct |0.114d (A4 = 0.028m) [09745]. V0370 Sct |d = 0.016P. V0372 Sct |d = 0.012P. V0414 Sct |Blue companion? V0479 Sct |Porb = 4.4267 d. V0484 Sct |MinII 9.22. V0490 Sct |Min II 13.6; Min II - Min I = 0.326P; DII = 0.025P. V0491 Sct |Min II 14.1. V0493 Sct |MinII - MinI = 0.75P. V0498 Sct |Multiperiodic. V0509 Sct |Several close companions. V0514 Sct |Several close companions. V0521 Sct |VB B (A 13.7m; AB 4", 359{deg}, 1998). V0530 Sct |VB B (A 3" sp). V0531 Sct |VB (companion of comparable brightness, 4.5", 326{deg}, 1998). V0548 Sct |Crowded. V0556 Sct |Crowded. V0558 Sct |Several companions. V0567 Sct |Crowded. V0571 Sct |Crowded. V0573 Sct |Crowded. V0574 Sct |Crowded. V0575 Sct |Crowded. V0584 Sct |Crowded. V0600 Sct |VB A (B 2" nf). V0646 Sct |OH, H2O, SiO maser. del Sct |VB A (B 10m, 53", 130{deg}); (k - b)2 = 0.37. The basic light del Sct |variation P0 (A0 = 0.125m) given in the Table is superposed by the del Sct |secondary one with P1 = 0.1867756 (A1 = 0.034) [09975]. R Ser |P var. Max = 2372429 + 356.93d*E (JD2372400 - 88900) [00960]; Max = R Ser |2397809 + 353.00d*E (JD2394000 - 2403000); Max = 2403104 + R Ser |357.25d*E (JD2403000 - 24000); Max = 2432387 + 356.10D*E R Ser |(JD2424000-39200); since JD2441000 - see Table. Maser (SiO, H2O). S Ser |P var. Max = 2394360 + 361.01d*E (JD2394000 - 2407000); Max = S Ser |2407024 + 372.70d*E (JD2407000 - 17000) [00960]; Max = 2425875 + S Ser |366.59d*E (JD2417000 - 36000); since JD2437600 - see Table. Maser S Ser |(OH, SiO, H2O). T Ser |In the region of the open cluster NGC 6633. P var. Max = 2400907 + T Ser |342.05d*E (JD2400500 - 15000); Max = 2417912 + 345.73d*E (JD2417900 T Ser |- 26000); Max = 2428524 + 332.21d*E (JD2426000 - 32500); Max = T Ser |2438382 + 345.71d*E (JD2432500 - 39500); since JD2439500 - see T Ser |Table. 0.8' from BN Ser. U Ser |P var. Max = 2421158 + 237.70d*E (JD2414000 - 22000); Max = 2422347 U Ser |+ 236.78d*E (JD2422000 - 26600); Max = 2426609 + 239.21d*E U Ser |(JD2426600 - 32500); since JD2432500 - see Table. V Ser |Min II 9.85. W Ser |P var, nonlinear terms: +(3.140d*10**(-6))*E**2 + W Ser |(1.432d*10**(-9))*E**3. The light curve shape var. Wavelike W Ser |variations in Max light. Changes of emission lines with the orbital W Ser |phase. Active mass exchange, evidence for a common envelope. X Ser |After 1932 variations 14.3m - 18.3m were noted; according to X Ser |[01417], P = 275d. Observations in 1961 - 1964 did not confirm P = X Ser |275d, fluctuations of light with a period of several minutes were X Ser |suspected [03625]. The spectral data are for 1981. Y Ser |Epoch of min is given. According to [08643], variations with P Y Ser |~400d are superimposed by P ~40d. Z Ser |The elements are valid during JD2422000 - 31000. RS Ser |Min II 11.4. RT Ser |Max (1920 - 1923). In the spectrum (1977 - 1979) there are RT Ser |emissions H{alpha} - H{delta}, HeI, HeII, [OI] etc. Absorptions RT Ser |TiO. RV Ser |Maser (H2O). VY Ser |[Fe/H] = -1.77, {Delta}(S) = 9. WW Ser |Maser (H2O). WX Ser |Maser (OH, SiO, H2O). P var? AA Ser |[A/H] = 0.2. AG Ser |P var? since JD2435000 - see Table. AK Ser |P var? before JD2442300 Min = 2431313.266 + 1.9225667d*E [00318]; AK Ser |since JD2442300 - see Table. AN Ser |P var? Max = 2429156.260 + 0.5220703d*E (JD2427000 - 38000) AN Ser |[00001]; since JD2438000 - see Table. According to [02740], Blazhko AN Ser |effect with Pi = 21.94d; the presence of the Blazhko effect is AN Ser |denied in [07258]. {Delta}(S) = 0. AO Ser |Min II 10.8. AP Ser |VB A (B 14.29m, 8" sp). [Fe/H] = -1.37. AQ Ser |Min II 11.1. AR Ser |P var. Before JD2425000 Max = 2415617.698 + 0.5752221d*E; Max = AR Ser |2425313.530 + 0.57508945d*E (JD2425000 - 28500); Max = 2428848.662 AR Ser |+ 0.575214d*E (JD2428500 - 31000) [08081]; Max = 2431436.424 + AR Ser |0.5751134d*E (JD2431000 - 34200); Max = 2436013.279 + 0.5752169d*E AR Ser |(JD2435900 - 37200); Max = 2438138.467 + 0.5750651d*E (JD2437200 - AR Ser |38700) [00001]. Elements working on average since JD2438700 - see AR Ser |Table. Complex Blazhko effect. Pi = 108.4d [08082]. A var (0.23m - AR Ser |0.87m V). Pi var (80d - 120d) [07032]. {Delta}(S) = 4.6. AS Ser |Min II 11.5. The epoch of Min I 2442937.428 (BBSAG) is not in AS Ser |agreement with the elements. AT Ser |P var. Max = 2415353.783 + 0.74655695d*E (JD2415000 - 27000); Max = AT Ser |2428337.260 + 0.7465670d*E (JD2428000 - 39500); since JD2441500 - AT Ser |see Table. {Delta}(S) = 9. AU Ser |Min II 11.61. The light curve shape var. AV Ser |{Delta}(S) = 6. AW Ser |{Delta}(S) = 5.0. BF Ser |[A/H] = -2.5. {Delta}(S) = 6. BH Ser |P var. Max = 2427956.674 + 0.434545d*E (JD2425000 - 30700) [01039]; BH Ser |since JD2437650 - see Table. BI Ser |Min I 2446264.414 [10200] contradicts the elements. P var? BN Ser |In the region of the open cluster NGC 6633. 0.8' from T Ser. BO Ser |P var? Max = 2425681 + 201d (JD2425600 - 30100) 0447]; the Table BO Ser |gives mean elements (JD2425600 - 35400). BQ Ser |P0 - see Table. P1 = 3.012d [08188]. In the region of the open BQ Ser |cluster IC 4756. BR Ser |In the region of the open cluster IC 4756. BS Ser |In the region of the open cluster IC 4756. BT Ser |In the region of the open cluster IC 4756. BU Ser |In the region of the open cluster IC 4756. CC Ser |Min II 11.63. CN Ser |[Fe/H] = -0.77. {Delta}(S) = 3.4. CO Ser |P var? The light curve shape var. [Fe/H] = -1.38. {Delta}(S) = 7.2. CQ Ser |Min II 12.0. CR Ser |[A/H] = -0.2. CS Ser |P var. Max = 2418137.875 + 0.5267904d*E (JD2416000 - 32500) CS Ser |[00001]; since JD2432500 - see Table. {Delta}(S) = (6). In the CS Ser |region of the HII complex S 54 and the open star cluster NGC 6604. CS Ser |Connected with a shell-structure nebula. Sometimes eclipses are CS Ser |observed during the configuration "WR in front of O" (see Table) CS Ser |and sometimes during the configuration "O in front of WR" which CS Ser |coincided with the deepest eclipse ever observed (with the depth CS Ser |0.5m B, V). Sometimes the photometric eclipse at predicted moments CS Ser |does not occur, and only the atmospheric eclipse of the O star with CS Ser |the WR component is observed at {lambda} 4653 A (emission of CII - CS Ser |CIV, NIII), {lambda} < 2000 A. IR excess; possibly an IR eclipse in CS Ser |the configuration "O in front of WR". CX Ser |The light curve (resembling the eclipsing light curve of U Gem) CX Ser |shows a hump of ~0.2m height before the minimum; fluctuations up to CX Ser |~0.3m - 0.4m in Max. DF Ser |VB A (B 13.9m, 0.4', -115{deg}). DG Ser |Min II 16.5:. The alias period is possible (0.3360742d). DH Ser |Another possible P = 450d. DK Ser |Max 2433829 [10008] contradicts the elements. DR Ser |VB A (B 12.54m, 28", 0{deg}). DT Ser |VB A (B ~5"). The spectrum shows emissions of [OIII] {lambda} DT Ser |lambda 4959, 5007 A. Symbiotic? [08676]. DV Ser |In a small star cluster. DY Ser |[Fe/H] = -1.58. {Delta}(S) = 8.4. EE Ser |In the region of the open cluster M 17 = NGC 6618. EF Ser |In the region of the open cluster M 17 = NGC 6618. EG Ser |VB A (ro > 10"). EL Ser |N <= 7. EN Ser |[Fe/H] = -1.07. {Delta}(S) = 5.3. EO Ser |The light curve shows large scatter. RR(B) type is possible. Max = EO Ser |2437433.653 + 0.6309d*E (JD2437433 - 514) [3625]. [Fe/H] = -1.63. EO Ser |{Delta}(S) = 8.8. ER Ser |In the region of the open cluster M 16 = NGC 6611. ES Ser |In the region of the open cluster M 16 = NGC 6611. ET Ser |In the region of the open cluster M 16 = NGC 6611. EU Ser |VB A (B 4" np). A member of the open cluster M 16 = NGC 6611. IR EU Ser |excess. EV Ser |In the region of the open cluster M 16 = NGC 6611. EW Ser |In the region of the open cluster M 16 = NGC 6611. EX Ser |In the region of the open cluster M 16 = NGC 6611. FI Ser |Hints of periodicity in U light. FK Ser |VB ({Delta}(m) ~0.5m, 1.3", 11.5{deg}, 1972). Flares were found in FK Ser |the satellite UV range [10013]. Differences from typical by stars FK Ser |and probable "post-T Tau" nature are noted [07260,03866]. According FK Ser |to [06948], Min = 2441939.200 + 5.20d*E. Soft X-ray source. FL Ser |VB ({Delta}(m) = 1.9m, 0.46", 145{deg}, 1981). FM Ser |In the region of the open cluster M 16 = NGC 6611. VB (var sf?). FN Ser |In the region of the open cluster M 16 = NGC 6611. FR Ser |ADS 11477 A (B 12.5m, 10.5", 330{deg}, 1924; C 9.3m, 30.5", 5{deg}, FR Ser |1930). Possible values of P: 2.1308d, 2.1565d. LN Ser |m pg ~17.5m ~const; blue companion? [07264]. LS Ser |The light curve shows large scatter, the elements need LS Ser |confirmation. Possible identification with an X-ray source 2ASE LS Ser |1822 + 0. LV Ser |The epoch of max in V light is given; in B and U varies in opposite LV Ser |phase. LX Ser |The depth of eclipses ~2.5m. Comparatively frequent outbursts LX Ser |[10023]. MM Ser |Ser X-1 = 4 U 1 837 + 04. LX/Lopt >= 100. VB B (A 19.1m; B 2.2", MM Ser |210{deg}). MO Ser |V1 (NGC 6535). Cluster non-member. MP Ser |V2 (NGC 6535). Cluster non-member. OU Ser |SB2. PS Ser |Both components are SB systems, Porb(A) = 15.888d, Porb(B) = PS Ser |13.561d. PT Ser |SB, Porb = 38.937d. V0381 Ser |SB2. V0383 Ser |SB2. V0384 Ser |MinII 12.35. V0391 Ser |The coordinates in [78230] are wrong. V0393 Ser |VB A (B 15" np). V0399 Ser |MinII 11.9. V0413 Ser |Apsidal motion, P(MinII) = 2.259735d. VB(9.1m, 9.1m, 0.3", V0413 Ser |215{deg}, 1991). V0425 Ser |Min II = 12.1. V0437 Ser |Superposed variations with an amplitude about 0.3m and a period of V0437 Ser |44d. V0462 Ser |P = 0.274277d is also possible. V0466 Ser |P = 0.177978d is also possible. V0493 Ser |Porb = 0.07408d, superhumps: P = 0.082866d. V0497 Ser |P = 0.302612d is also possible. V0499 Ser |Multiperiodic. V0501 Ser |P = 0.266086d is also possible. V0539 Ser |Multiperiodic. V0562 Ser |d = 0.07P. V0575 Ser |Double-mode pulsations. The Table contains light elements for the V0575 Ser |first overtone. Fundamental mode: Max = 2454700.867 + 0.475615d x V0575 Ser |E. P1/P0 = 0.7446. V0579 Ser |Double-mode pulsations. The Table contains light elements for the V0579 Ser |first overtone. Fundamental mode: Max = 2454800.609 + 0.479144d x V0579 Ser |E. P1/P0 = 0.7444. V0585 Ser |SiO maser. V0592 Ser |VB A (B 14.0mpg, 13", 80{deg}, 1998). V0595 Ser |VB A (B 5" p). V0609 Ser |VB A (B 4", 186{deg}, 1998; several fainter companions). The V0609 Ser |magnitudes in the Table were influenced by the companions. V0627 Ser |A twice shorter period is also possible. VB A (B 7", 183{deg}; C V0627 Ser |5", 159{deg}, 2000). V0628 Ser |VB A (B 14.0mV, 7.5", 207{deg}, 2000). V0637 Ser |P1 is presented in the Table. P0 = 0.541556d; P1/P0 = 0.7460. V0638 Ser |Double-mode pulsations. P = 0.04191053d is superposed. V0640 Ser |The data for 1SWASP J151652.90+004835.8 in [82030] are combined V0640 Ser |measurements for a non-variable star (V = 14.3m) near the SuperWASP V0640 Ser |position and the real variable. V0641 Ser |Type EB with a twice longer period is not excluded. V0646 Ser |P1 is presented in the Table. P0 = 0.596277d; P1/P0 = 0.7450. V0647 Ser |Double-mode pulsations. P = 0.042667 is superposed. V0649 Ser |P1 is presented in the Table. P0 = 0.481733d; P1/P0 = 0.7438. V0654 Ser |P1 is presented in the Table. P0 = 0.491922d; P1/P0 = 0.7456. V0661 Ser |H2O, OH maser. V0664 Ser |SiO, H2O maser. V0667 Ser |VB AB (10.2mV, 11.2mV, 3", 127{deg}, 2000). V0677 Ser |Cluster non-member? V0679 Ser |Cluster non-member? del Ser |ADS 9701A (B 5.16m, dF0, a = 5.843", Porb = 3168 yr; 4", 175G, del Ser |1980). omi Ser |SB? d Ser |ADS 11353 A (B 7.44m, SB?, F5V, 3.9", 320{deg}, 1983). VB d Ser |(speckle-interferometric; 0.25", 157{deg}, 1976). SB (P1orb = 385d, d Ser |P2orb = 1.8505205d). S Sex |P var. Max = 2422029 + 257.2d*E (JD2417650 - 22050); Max = 2428968 S Sex |+ 266.65d*E (JD2422050 - 30300); Max = 2434739 + 260.86d*E S Sex |(JD2430300 - 34750); Max = 2438796 + 254.3d*E (JD2434750 - 38800); S Sex |since JD2440600 - see Table. T Sex |[Fe/H] = -1.20. P var. Max = 2416146.675 + 0.32465971d*E (JD2414000 T Sex |- 18300), Max = 2424561.398 + 0.32467107d*E (JD2418300 - 24570) T Sex |[00752]; Max = 2424561.430 + 0.3246702d*E (JD2424560 - 28280), Max T Sex |= 2429350.320 + 0.3247113d*E (JD2429350 - 34370), Max = 2434795.409 T Sex |+ 0.3246978d*E (JD2434795 - 36630) [09978]; since JD2441380 - see T Sex |Table. U Sex |P var. Max = 2419823.355 + 0.53402622d*E (JD2419470 - 36670) U Sex |[03697]; since JD2443980 - see Table. Y Sex |Min II 10.17; dII = 0.05P. P var. Min I = 2428122.700 + Y Sex |0.41982341d*E (JD < 2429000) [00007]; Min I = 2434445.989 + Y Sex |0.419818d*E (JD2428100 - 35000) [00001], Min I = 2439521.964 + Y Sex |0.41981543d*E (JD2431150 - 43250) [09981]; since JD2440300 - see Y Sex |Table. RU Sex |Min II 11.4. According to [09923], RR? (P = 0.5398d?), CEP? (P = RU Sex |6.792d?). RW Sex |Porb = 0.247d [09925]; LX/Lopt = 10**(-4) [09926]; Px = 254s RW Sex |[09927]. RX Sex |VB A (B 9.1m, 116.3", 191{deg}). RY Sex |Mu = 0.67", P = 281{deg}. WW Sex |MinII 10.46. WX Sex |MinII 12.8. WY Sex |The depth of MinII is 0.29. WZ Sex |MinII 10.0. AI Sex |Min II = 11.0. AO Sex |P = 0.234675d is also possible. AY Sex |A millisecond radio pulsar showing optical variations with the AY Sex |tabulated orbital period. Dramatic shanges in the spectrum were AY Sex |recorded. BG Sex |P = 0.415502d is also possible. BP Sex |VB A (B 10.96mV, 1.3", 342{deg}, 1991). BY Sex |Pulsates in the first overtone (see Table) and fundamental (Max = BY Sex |2454801.000 + 0.581288d x E) modes. P1/P0 = 0.7473. CF Sex |P strongly varies. The elements in the Table are for JD 2455900 - CF Sex |2456500. CW Sex |P1 is presented in the Table. P0 = 0.475673d; P1/P0 = 0.7443. CX Sex |P1 is presented in the Table. P0 = 0.563212d; P1/P0 = 0.7459. CY Sex |P1 is presented in the Table. P0 = 0.488334d; P1/P0 = 0.7446. R Tau |OH, H2O, Sio maser. P var. Max = 2411012 + 325.0d*E (JD2398654 - R Tau |2414000); Max = 2424243 + 322.1d*E (JD2414000 - 24300); Max = R Tau |2434005 + 325.4d*E (JD2424300 - 35500); since JD2435500 - see R Tau |Table. S Tau |P var. Max = 2404646 + 380.1d*E (JD2399326 - 2405000); Max = S Tau |2425085 + 371.40d*E (JD2405000 - 26000); since JD2426000 - see S Tau |Table. T Tau |VB A (B 15m, 0.27", 358{deg}; C - infrared companion, 0.590", T Tau |180{deg}). Near the variable nebula NGC 1555. OH, H2O maser. In the T Tau |interval JD2402140 - 21000 the light range 9.3m - 13.5m, since T Tau |JD2421000 - only 9.5m - 10.8m. U Tau |VB (A 10.9m; B 12.0m, 3", 77{deg}). V Tau |P var. Max = 2417978 + 170.0d*E (JD2404550 - 18000); Max = 2424580 V Tau |+ 169.3d*E (JD2418000 - 24600); Max = 2432746 + 170.1d*E (JD2424600 V Tau |- 33500); Max = 2436970 + 168.7d*E (JD2433500 - 37300); Max = V Tau |2442442 + 171.1d*E (JD2437300 - 43000); since JD2443000 - see V Tau |Table. W Tau |P value is given in the Table. P var. Max = 2415320 + 274.1d*E W Tau |(JD2410360 - 15500), Max = 2421995 + 266.1d*E (JD2415500 - 22500), W Tau |Max = 2425135 + 260.5d*E (JD2422500 - 28800), Max = 2438837 + W Tau |245.4d*E (JD2428800 - 39100) [00001]. Z Tau |VB A (B 13.6m, 4", 45{deg}). P var. Max = 2425115 + 499.90d*E Z Tau |(JD2415100 - 26500) Max = 2438768 + 486.20d*E (JD2426500 - 39000); Z Tau |since JD2439000 - see Table. RR Tau |Spectrum description and the photographs of the nebula [04002]. RU Tau |VB A (B 4"). P var. Max = 2426004 + 545.3d*E (JD2415009 - 27500). RU Tau |Max = 2434309 + 604.0d*E (JD2427500 - 34500); since JD2437500 - see RU Tau |Table. RV Tau |OH maser. Mean brightness varies: Min = 2417553 + 1224d*E [00580]. RW Tau |VB A (12.5m, 1.3", 172{deg}, 1959). dI = 0.020P; Min II 8.09. P RW Tau |var. Min I = 2417198.410 + 2.7688665d*E + 0.038d*sin(0.0818{deg}*(E RW Tau |- 100)) (JD2409913 - 24150), Min I = 2434423.3571 + 2.7688209d*E RW Tau |(JD2424150 - 37000) [05460]; Min I = 2437164.4860 + 2.7688480d*E RW Tau |(JD2437000 - 39900) [07531]; Min I = 2442776.93772 + 2.76884463d*E RW Tau |(JD2439855 - 42780) [08593]; Min I = 2442776.9313 + 2.7688396d*E RW Tau |(JD2442780 - 45750) [09084]; since JD2445750 - see Table. The shape RW Tau |of the light curve varies. RX Tau |OH, H2O maser. P var. Max = 2423561 + 338.4d*E (JD2417155 - 24000); RX Tau |Max = 2430505 + 330.2d*E (JD2424000 - 30700); Max = 2437963 + RX Tau |339.3d*E (JD2430700 - 38000); since JD2438000 - see Table. RY Tau |SB1. The photographs of the nebula and spectrum description RY Tau |[05064]. Long period light variations are possible with cycles RY Tau |70.25, 15.9, 9.4 and 5.84 years [09993]. RZ Tau |Min II 10.66. P var. Min I = 2424032.1426 + 0.41567109d*E RZ Tau |(JD2424000 - 34100) [00312]; since JD2436000 - see Table. SS Tau |P var [03506]. Max = 2420894.2339 + 0.3699665d*E (JD2420890 - SS Tau |21300) [09995]; Max = 2426669.080 + 0.3699687d*E (JD2426400 - SS Tau |26700) [00320]; Max = 2428843.856 + 0.3699231d*E (JD2426700 - SS Tau |30300), Max = 2431392.603 + 0.369912d*E (JD2430300 - 31400), Max = SS Tau |2432118.794 + 0.369937d*E (JD2431400 - 32150), Max = 2432857.884 + SS Tau |0.3699146d*E (JD2432150 - 35000), Max = 2435055.528 + 0.3699066d*E SS Tau |(JD2435000 - 36400), Max = 2437313.503 + 0.3699266d*E (JD2436400 - SS Tau |37320), Max = 2437960.419 + 0.369878d*E (JD2437300 - 37960), Max = SS Tau |2437960.419 + 0.369938d*E (JD2437960 - 38740); since JD2438740 - SS Tau |see Table. SV Tau |Min II 9.8. SW Tau |P var. Max = 2432049.856 + 1.583623d*E (JD2418240 - 36000); since SW Tau |JD2436000 - see Table. SX Tau |In the region of the Pleiades cluster. Not a member of the cluster. SY Tau |In the region of the Pleiades cluster. Not a member of the cluster. SZ Tau |The member of the halo of the open cluster NGC 1647. P var. Max = SZ Tau |2410000.60 + 3.1487d*E (JD2412000 - 20200) [09996]; Max = SZ Tau |2419267.519 + 3.149046d*E (JD2419260 - 34650); since JD2434650 - SZ Tau |see Table. TT Tau |P = 364d? [00589]. TY Tau |In the region of the hyades cluster. Not a member of the cluster. TY Tau |According to [09997], Min = 2422291.303 + 0.539250d*E. UU Tau |In the region of the Pleiades cluster. Not a member of the cluster. UX Tau |VB A (B 13.67m V, M2.5 VE, 5.74", 270.1{deg}, 1944). UZ Tau |VB A (B 15.16m B, M4VE (Li), 3.7", 271.5{deg}, 1944). The range of UZ Tau |the combined light variation is given in the Table. VW Tau |The chart in [06286] is wrong. WW Tau |P var. P = 114.8d (JD2414800 - 20800). P = 124.4d (JD2420800 - WW Tau |23700) [00634]; P = 114d (JD2424800 - 26300), P = 139d (JD2426300 - WW Tau |27700) [00310]; P = 114d (JD2427900 - 30800), P = 131d (JD2430800 - WW Tau |31500), P = 109d (JD2431500 - 33400) [00364]; since JD2433400 - see WW Tau |Table. WY Tau |Min II 11.73. P var? [10048]. WZ Tau |VB. XZ Tau |VB A (B = HL Tau, 23", 273{deg}). YZ Tau |[Fe/H] = -1.53. In the region of the Pleiades cluster. Not a member YZ Tau |of the cluster. There is a square term in the elements: YZ Tau |-6d*10**(-11)*E**2. AA Tau |Cyclic light variation with P = 4.5d and 2d [10003] and also 8.2d AA Tau |[10004] is possible. AC Tau |d = 0.025P. P var? AH Tau |Min II 11.85. P var? In the region of the Pleiades cluster. Not a AH Tau |member of the cluster. AL Tau |P var. The depth of Min II 0.15m. AM Tau |d = 0.012P:. P var. Min I = 2427534.444 + 2.044018d*E (JD2425580 - AM Tau |27540), Min I = 2435019.436 + 2.043935d*E (JD2433320 - 37020); AM Tau |since JD2442365 - see Table. AN Tau |Min II 10.5; Min II - Min I = 0.53P. P var. AP Tau |Min II 14.7; Min II - Min I = 0.48P. AS Tau |P var. Min I = 2439390.595 + 3.4835542d*E (JD2419440 - 44300) AS Tau |[07806]; since JD2444300 - see Table. AU Tau |P var. Max = 2426642 + 71.0d*E (JD2426290 - 30400) [00310]; since AU Tau |JD2438000 - see Table. AW Tau |OH, H2O maser. P var. Max = 2426278 + 690d*E (JD2416100 - 33850) AW Tau |[00609]; since JD2433850 - see Table. BB Tau |SC 7/7 e. BK Tau |In the region of the Pleiades cluster. Not a member of the cluster. BN Tau |P var. Min I = 2435460.370 + 4.2542044d*E (JD2419000-39100) BN Tau |[05466]; since JD2443000 - see Table. BP Tau |There are quasisinusoidal light variations with P = 7.6d [10011]. BU Tau |Pleione. The member of the Pleiades cluster. BV Tau |Min II 11.9. BW Tau |3C 120. Seyfert galaxy; Z = 0.033. Spectrum description [10012]. CD Tau |VB A (B 9.88m, 9.9", 148.8{deg}). Min II 7.31. In the region of the CD Tau |open cluster CR 65. CF Tau |d = 0.02P; Min II 10.2; CH Tau |The epoch of Min brightness is given. CM Tau |SN 1054 in the Crab nebula (NGC 1952 = M1); pulsar NP 0532. The CM Tau |outburst epoch is JD2106210:. The pulsed radiation varies precisely CM Tau |in phase over the whole spectrum, from radio waves to {gamma} rays CM Tau |with P = 0.033S in the range 13.9m - 17.7m V. P var [10017,10018]: CM Tau |0.033095563927s (JD2440297.5094) <= P <= 0.033242051159s CM Tau |(JD2444312.750). CR Tau |P = 1.362692d? CT Tau |Min II 11.12. P var. Min I = 2437312.369 + 0.6668274d*E (JD2432700 CT Tau |- 38790) [10010]; since JD2441400 - see Table. CU Tau |In the region of the Pleiades cluster. Not a member of the cluster. CU Tau |Min II 11.90. P var. Min I = 2431822.5193 + 0.4126022d*E (JD2431060 CU Tau |- 2890) [00604]; since JD2440960 - see Table. CZ Tau |VB B (A = DD Tau; B 31", 13{deg}). DD Tau |VB A (B = CZ Tau; 31", 13{deg}. DE Tau |VB A (B 26", 10{deg}). DG Tau |Connected with a small bright arc-shaped nebula. DH Tau |VB A (B = DI Tau, 16", 125{deg}). According to [10004] there is DH Tau |periodical light variability with P = 7.0d and A = 0.4m V. DI Tau |VB B (A = DH Tau; B 16", 125{deg}). According to [10004] there is DI Tau |periodical light variability with P ~7.0d and A < 0.4m V. DL Tau |VB A (B 17m V, 12", 333{deg}). Cyclic light variation with P = 2.7d DL Tau |is present [10003]. DN Tau |There are sinusoidal light variations with P = 6.6d [10011]. DO Tau |Connected with a small bright arc-shaped nebula. DS Tau |VB A (B 13.7m, 4", 288{deg}). Range of Combined light variation of DS Tau |the pair is given in the Table. EI Tau |VB? EQ Tau |Min II 10.97. In the region of the Pleiades cluster. Not a member EQ Tau |of the cluster. ET Tau |Min II 9.3. EY Tau |The member of the Hyades cluster. EZ Tau |The member of the Hyades cluster. FH Tau |The member of the Hyades cluster. FL Tau |The member of the Pleiades cluster. FS Tau |VB A (B 16", 289{deg}). FV Tau |VB A (B 13", 103{deg}). FW Tau |VB A (B 13", 243{deg}). FY Tau |VB B (A = FZ Tau, B 17", 250{deg}.) FZ Tau |VB A (B = FY Tau, 17", 250{deg}). GG Tau |VB A (B 18.5m, 12", 205{deg}). GH Tau |VB B (A = V807 Tau; B 21.4", 193{deg}). GI Tau |VB B (A = GK Tau; B 13", 329{deg}). There are quasisinusoidal light GI Tau |variations with P = 7.2d [10011]. Connected with a small bright GI Tau |arc-shaped nebula. GK Tau |VB A (B = GI Tau, 13", 329{deg}). There are quasisinusoidal light GK Tau |variations with P = 4.6d [10011]. Connected with a small bright GK Tau |arc-shaped nebula. GL Tau |The central star of the planetary nebula PK 174 -14{deg} 1. GP Tau |P2 = 1000d. GR Tau |dI = 0.068P; Min II 10.49; Mim II - Min I = 0.516P. GS Tau |SB1 (Porb = 7.227424d [06568]). The epoch of Min brightness is GS Tau |given. GU Tau |VB A (B 11", 299{deg}). GV Tau |Herbig-haro object. GW Tau |Min II 11.7. P var? GX Tau |VB A (B 11", 310{deg}). HK Tau |VB A (B 21m, 2", 180{deg}). HL Tau |VB B (A = XZ Tau; B 23", 273{deg}). Connected with a small bright HL Tau |arc-shaped nebula. HN Tau |VB A (B 18m, 3.3", 205{deg}). HO Tau |VB A (B 8", 110{deg}). HP Tau |Connected with a small bright arc-shaped nebula. According to HP Tau |[10004] there is periodical variability with P = 1.2d. HR Tau |VB B (A = HS Tau; B 14", 119{deg}). HS Tau |VB A (B = HR Tau; 14", 119{deg}). HU Tau |Min II 5.91. HW Tau |Minor planet (49) Pales. HZ Tau |In the region of the Pleiades cluster. Possible member of the HZ Tau |cluster. II Tau |In the region of the Pleiades cluster. Possible member of the II Tau |hyades cluster IK Tau |OH, H2O, SiO maser. IM Tau |P var. Max = 2439792.398 + 0.144969d*E (JD2439790 - 43130) [10019]; IM Tau |P1 = 0.109016d, P1/P0 = 0.752. Since JD2444230 - see Table. IN Tau |{mu} = 0.121", P = 105{deg}. The member of the Hyades cluster? IO Tau |In the region of the Hyades cluster. IQ Tau |VB A (B 17m, 11", 298{deg}). IS Tau |SVS 1319 [04051]. The star N23 with H{alpha} emission [00596]. In IS Tau |the map given in [00596] erroneously designated as N26 in IS Tau |contradiction with the co-ordinates given in the same paper. It was IS Tau |the reason for different mistakes when the star was identified by IS Tau |some other investigators. IT Tau |SVS 1320 [04051]. The star N26 with H{alpha} emission [00596]. In IT Tau |the map given in [00596] IS Tau erroneously designated as N26 in IT Tau |contradiction with the co-ordinates given in the same paper. It was IT Tau |the reason for different mistakes when IS Tau was identified by IT Tau |some other investigators. KK Tau |In the region of the Pleiades cluster. KL Tau |In the region of the Pleiades cluster. KM Tau |In the region of the Pleiades cluster. KN Tau |In the region of the Pleiades cluster. KO Tau |In the region of the Pleiades cluster. KP Tau |In the region of the Pleiades cluster. Not a member of the cluster. KQ Tau |In the region of the Pleiades cluster. KR Tau |In the region of the Pleiades cluster. Not a member of the cluster. KS Tau |In the region of the Pleiades cluster. KT Tau |In the region of the Pleiades cluster. KU Tau |In the region of the Pleiades cluster. KV Tau |In the region of the Pleiades cluster. KW Tau |In the region of the Pleiades cluster. KX Tau |In the region of the Pleiades cluster. Not a member of the cluster. KY Tau |The member of the Pleiades cluster. KZ Tau |In the region of the Pleiades cluster. LL Tau |In the region of the Pleiades cluster. LM Tau |In the region of the Pleiades cluster. Possible member of the LM Tau |cluster. LN Tau |In the region of the Pleiades cluster. LO Tau |In the region of the Pleiades cluster. Possible member of the LO Tau |cluster. LP Tau |In the region of the Pleiades cluster. Not a member of the cluster. LQ Tau |In the region of the Pleiades cluster. LR Tau |In the region of the Pleiades cluster. Possible member of the LR Tau |Hyades cluster. LS Tau |In the region of the Pleiades cluster. LT Tau |In the region of the Pleiades cluster. Possible member of the LT Tau |cluster. LU Tau |In the region of the Pleiades cluster. Possible member of the LU Tau |cluster. LV Tau |In the region of the Pleiades cluster. Possible member of the LV Tau |cluster. LW Tau |In the region of the Pleiades cluster. Not a member of the cluster. LX Tau |In the region of the Pleiades cluster. LY Tau |In the region of the Pleiades cluster. Possible member of the LY Tau |cluster. LZ Tau |The member of the Pleiades cluster. MM Tau |The member of the Pleiades cluster. MN Tau |In the region of the Pleiades cluster. MO Tau |In the region of the Pleiades cluster. Possible member of the MO Tau |cluster. MP Tau |In the region of the Pleiades cluster. MQ Tau |In the region of the Pleiades cluster. MR Tau |The member of the Pleiades cluster. MS Tau |The member of the Pleiades cluster. MT Tau |In the region of the Pleiades cluster. Not a member of the cluster. MU Tau |In the region of the Pleiades cluster. Possible member of the MU Tau |cluster. MV Tau |In the region of the Pleiades cluster. Possible member of the MV Tau |cluster. MW Tau |In the region of the Pleiades cluster. MX Tau |The member of the Pleiades cluster. MY Tau |The member of the Pleiades cluster. MZ Tau |In the region of the Pleiades cluster. Possible member of the MZ Tau |cluster. NN Tau |In the region of the Pleiades cluster. NO Tau |In the region of the Pleiades cluster. NP Tau |The member of the Pleiades cluster. NQ Tau |In the region of the Pleiades cluster. NR Tau |In the region of the Pleiades cluster. Not a member of the cluster. NS Tau |In the region of the Pleiades cluster. NT Tau |In the region of the Pleiades cluster. Possible member of the NT Tau |cluster. NU Tau |In the region of the Pleiades cluster. NV Tau |In the region of the Pleiades cluster. Not a member of the cluster. NW Tau |In the region of the Pleiades cluster. NX Tau |In the region of the Pleiades cluster. Not a member of the cluster. NY Tau |In the region of the Pleiades cluster. Not a member of the cluster. NZ Tau |In the region of the Pleiades cluster. OO Tau |In the region of the Pleiades cluster. OP Tau |In the region of the Pleiades cluster. Possible member of the OP Tau |cluster. OQ Tau |In the region of the Pleiades cluster. OR Tau |The member of the Pleiades cluster. OS Tau |The member of the Pleiades cluster. OT Tau |The member of the Pleiades cluster. OU Tau |Max = 2444896.758 + 0.39701d*E, M - m = 0.5P, A(V) = 0.13m [10052]. OU Tau |The member of the Pleiades cluster. OW Tau |The member of the Pleiades cluster. OX Tau |In the region of the Pleiades cluster. OY Tau |In the region of the Pleiades cluster. Not a member of the cluster. OZ Tau |In the region of the Pleiades cluster. Possible member of the OZ Tau |cluster. PP Tau |In the region of the Pleiades cluster. Possible member of the PP Tau |cluster. PQ Tau |In the region of the Pleiades cluster. Not a member of the cluster. PR Tau |The member of the Pleiades cluster. PS Tau |In the region of the Pleiades cluster. PT Tau |The member of the Pleiades cluster. PU Tau |In the region of the Pleiades cluster. PV Tau |In the region of the Pleiades cluster. Possible member of the PV Tau |cluster. PW Tau |In the region of the Pleiades cluster. PZ Tau |In the region of the Pleiades cluster. QQ Tau |SB2. The member of the Pleiades cluster. QR Tau |In the region of the Pleiades cluster. QS Tau |In the region of the Pleiades cluster. QT Tau |In the region of the Pleiades cluster. QU Tau |VB A (B 18.0m, 4.0", 135{deg}). In the region of the Pleiades QU Tau |cluster. QV Tau |In the region of the Pleiades cluster. QW Tau |In the region of the Pleiades cluster. QX Tau |The member of the Pleiades cluster. Max = 2444896.79 + 0.483d*E, M QX Tau |- m = 0.5P, A(V) = 0.125m [10052]. QY Tau |In the region of the Pleiades cluster. Not a member of the cluster. QZ Tau |In the region of the Pleiades cluster. V0335 Tau |In the region of the Pleiades cluster. V0336 Tau |In the region of the Pleiades cluster. Possible member of the V0336 Tau |cluster. V0337 Tau |In the region of the Pleiades cluster. V0338 Tau |In the region of the Pleiades cluster. Possible member of the V0338 Tau |cluster. V0339 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0340 Tau |In the region of the Pleiades cluster. V0341 Tau |In the region of the Pleiades cluster. V0342 Tau |In the region of the Pleiades cluster. V0343 Tau |The member of the Pleiades cluster. V0344 Tau |In the region of the Pleiades cluster. V0345 Tau |In the region of the Pleiades cluster. V0346 Tau |The member of the Pleiades cluster. V0347 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0348 Tau |In the region of the Pleiades cluster. V0349 Tau |In the region of the Pleiades cluster. Possible member of the V0349 Tau |cluster. V0350 Tau |In the region of the Pleiades cluster. Possible member of the V0350 Tau |cluster. V0351 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0352 Tau |In the region of the Pleiades cluster. V0353 Tau |In the region of the Pleiades cluster. Possible member of the V0353 Tau |cluster. V0354 Tau |In the region of the Pleiades cluster. Possible member of the V0354 Tau |cluster. V0355 Tau |In the region of the Pleiades cluster. Possible member of the V0355 Tau |cluster. V0356 Tau |In the region of the Pleiades cluster. V0357 Tau |The member of the Pleiades cluster. V0358 Tau |The member of the Pleiades cluster. V0359 Tau |In the region of the Pleiades cluster. V0360 Tau |In the region of the Pleiades cluster. V0361 Tau |In the region of the Pleiades cluster. Possible member of the V0361 Tau |cluster. V0362 Tau |In the region of the Pleiades cluster. V0363 Tau |In the region of the Pleiades cluster. Possible member V0364 Tau |In the region of the Pleiades cluster. Possible member of the V0364 Tau |cluster. V0365 Tau |In the region of the Pleiades cluster. V0366 Tau |The member of the Pleiades cluster. V0367 Tau |In the region of the Pleiades cluster. V0368 Tau |In the region of the Pleiades cluster. V0369 Tau |In the region of the Pleiades cluster. V0370 Tau |The member of the Pleiades cluster. V0371 Tau |VB ({Delta}(m) ~1m, 1.5"). The member of the Pleiades cluster. V0372 Tau |The member of the Pleiades cluster. V0373 Tau |In the region of the Pleiades cluster. V0374 Tau |In the region of the Pleiades cluster. V0375 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0376 Tau |The member of the Pleiades cluster. V0377 Tau |The member of the Pleiades cluster. V0378 Tau |The member of the Pleiades cluster. V0379 Tau |In the region of the Pleiades cluster. Possible member of the V0379 Tau |cluster. V0380 Tau |In the region of the Pleiades cluster. Possible member of the V0380 Tau |cluster. V0381 Tau |The member of the Pleiades cluster. V0382 Tau |The member of the Pleiades cluster. V0383 Tau |In the region of the Pleiades cluster. V0384 Tau |The member of the Pleiades cluster. V0385 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0386 Tau |TCSN 437. In the region of the Pleiades cluster. V0387 Tau |In the region of the Pleiades cluster. V0388 Tau |In the region of the Pleiades cluster. V0389 Tau |TCSN 439. In the region of the Pleiades cluster. V0390 Tau |In the region of the Pleiades cluster. V0392 Tau |In the region of the Pleiades cluster. Possible member of the V0392 Tau |cluster. V0394 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0395 Tau |In the region of the Pleiades cluster. V0396 Tau |In the region of the Pleiades cluster. V0397 Tau |In the region of the Pleiades cluster. V0398 Tau |In the region of the Pleiades cluster. Possible member of the V0398 Tau |cluster. V0399 Tau |The member of the Pleiades cluster. V0400 Tau |In the region of the Pleiades cluster. V0401 Tau |In the region of the Pleiades cluster. V0402 Tau |The member of the Pleiades cluster. V0403 Tau |The member of the Pleiades cluster. V0404 Tau |In the region of the Pleiades cluster. V0405 Tau |In the region of the Pleiades cluster. V0410 Tau |There are periodical light variations with P = 1.92d, A(V) = 0.21m, V0410 Tau |M - m = 0.5P [10056]. V0411 Tau |{mu} = 0.13", P = 143{deg}. Eruptive white dwarf. Usually there are V0411 Tau |quasi-perio- dic variations with A ~0.3m and periods P0 = 12.436 V0411 Tau |Min and P1 = 8.237 Min (P1/P0 = 0.6624) which are nonlinearly V0411 Tau |modulated by the third period PL ~0.135d (probably by the orbital V0411 Tau |period of a faint companion). V0421 Tau |Minor planet (586) Thekla. V0423 Tau |Min II 15.8. V0425 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0426 Tau |In the region of the Pleiades cluster. V0427 Tau |In the region of the Pleiades cluster. V0428 Tau |In the region of the Pleiades cluster. V0429 Tau |In the region of the Pleiades cluster. V0430 Tau |In the region of the Pleiades cluster. Possible member of the V0430 Tau |cluster. V0431 Tau |In the region of the Pleiades cluster. V0432 Tau |In the region of the Pleiades cluster. V0433 Tau |In the region of the Pleiades cluster. V0434 Tau |In the region of the Pleiades cluster. V0435 Tau |In the region of the Pleiades cluster. Possible member of the V0435 Tau |cluster. V0436 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0437 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0438 Tau |In the region of the Pleiades cluster. Possible member of the V0438 Tau |cluster. V0439 Tau |In the region of the Pleiades cluster. V0440 Tau |In the region of the Pleiades cluster. V0441 Tau |In the region of the Pleiades cluster. Possible member of the V0441 Tau |cluster. V0442 Tau |In the region of the Pleiades cluster. V0443 Tau |In the region of the Pleiades cluster. V0444 Tau |In the region of the Pleiades cluster. Possible member of the V0444 Tau |cluster. V0445 Tau |In the region of the Pleiades cluster. V0446 Tau |The member of the Pleiades cluster. V0447 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0448 Tau |The member of the Pleiades cluster. V0449 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0451 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0452 Tau |In the region of the Pleiades cluster. Possible member of the V0452 Tau |cluster. V0453 Tau |In the region of the Pleiades cluster. Possible member of the V0453 Tau |cluster. V0454 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0455 Tau |In the region of the Pleiades cluster. V0456 Tau |In the region of the Pleiades cluster. V0457 Tau |In the region of the Pleiades cluster. V0458 Tau |In the region of the Pleiades cluster. V0459 Tau |In the region of the Pleiades cluster. V0460 Tau |In the region of the Pleiades cluster. V0461 Tau |In the region of the Pleiades cluster. Possible member of the V0461 Tau |cluster. V0462 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0463 Tau |In the region of the Pleiades cluster. V0464 Tau |In the region of the Pleiades cluster. V0465 Tau |In the region of the Pleiades cluster. V0466 Tau |In the region of the Pleiades cluster. Possible member of the V0466 Tau |cluster. V0467 Tau |In the region of the Pleiades cluster. V0468 Tau |In the region of the Pleiades cluster. V0469 Tau |In the region of the Pleiades cluster. V0470 Tau |In the region of the Pleiades cluster. Possible member of the V0470 Tau |cluster. V0471 Tau |The member of the Hyades cluster. EA/D/(RS + WD) + XP. d = 0.0625P. V0471 Tau |There occurs a total eclipse of the white dwarf in Min I (A = 0.04m V0471 Tau |V, 0.36m U). P var. Min I = 2440612.67083 + 0.52118321d*E V0471 Tau |(JD2440570 - 970) [06250]; Min I = 2440898.80038 + 0.52118376d*E V0471 Tau |(JD2440880 - 41360), Min I = 2441665.46153 + 0.52118329d*E V0471 Tau |(JD2441660 - 42100) [10058]; since JD2441900 - see Table. Wave-like V0471 Tau |distorsion with the amplitude from 0.05m up to 0.27m and with the V0471 Tau |period close to the orbital one is observed in the light curve V0471 Tau |outside eclipses; sometimes there are also flares. The wave is V0471 Tau |migrating on phase in the direction of phase decreasing with a V0471 Tau |migration period of 191d [10060] or ~250d [10061]. The period of V0471 Tau |white dwarf rotation derived through X-ray observations Ppuls = V0471 Tau |554.73s [10062]. V0472 Tau |In the region of the Pleiades cluster. V0473 Tau |P = 2.7800d? V0474 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0475 Tau |In the region of the Pleiades cluster. V0476 Tau |In the region of the Pleiades cluster. V0477 Tau |In the region of the Pleiades cluster. V0478 Tau |In the region of the Pleiades cluster. V0479 Tau |VB A (BC 8.90m, 59", 357{deg}); (k - b)2 = 0.40. V0480 Tau |VB A (B 10.4m, 176", 303{deg}). The member of the Hyades cluster. V0481 Tau |In the region of the Pleiades cluster. V0483 Tau |The member of the Hyades cluster. V0484 Tau |The member of the Hyades cluster. V0485 Tau |In the region of the Pleiades cluster. V0486 Tau |Epoch of Max (U) is given. P =/ 10.61d? [10063]. V0487 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0487 Tau |On the photograph west is at the top and south to the right. V0488 Tau |The member of the Pleiades cluster. V0489 Tau |In the region of the Pleiades cluster. V0490 Tau |In the region of the Pleiades cluster. V0491 Tau |In the region of the Pleiades cluster. Possible member of the V0491 Tau |cluster. V0492 Tau |In the region of the Pleiades cluster. Possible member of the V0492 Tau |cluster. V0493 Tau |In the region of the Pleiades cluster. V0494 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0495 Tau |In the region of the Pleiades cluster. V0496 Tau |In the region of the Pleiades cluster. V0497 Tau |In the region of the Pleiades cluster. Possible member of the V0497 Tau |cluster. V0498 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0499 Tau |In the region of the Pleiades cluster. V0500 Tau |The member of the Pleiades cluster. V0501 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0502 Tau |The member of the Pleiades cluster. V0503 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0504 Tau |In the region of the Pleiades cluster. V0506 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0507 Tau |In the region of the Pleiades cluster. V0508 Tau |In the region of the Pleiades cluster. V0509 Tau |In the region of the Pleiades cluster. V0510 Tau |In the region of the Pleiades cluster. V0511 Tau |In the region of the Pleiades cluster. V0512 Tau |In the region of the Pleiades cluster. V0513 Tau |In the region of the Pleiades cluster. V0514 Tau |In the region of the Pleiades cluster. V0515 Tau |In the region of the Pleiades cluster. V0516 Tau |In the region of the Pleiades cluster. V0517 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0518 Tau |VB B (A 14.4m; B 10", 80{deg}). The member of the Pleiades cluster. V0519 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0520 Tau |In the region of the Pleiades cluster. Possible member of the V0520 Tau |cluster. V0521 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0522 Tau |In the region of the Pleiades cluster. V0523 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0524 Tau |In the region of the Pleiades cluster. V0525 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0526 Tau |In the region of the Pleiades cluster. V0527 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0528 Tau |In the region of the Pleiades cluster. V0529 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0530 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0531 Tau |In the region of the Pleiades cluster. V0532 Tau |In the region of the Pleiades cluster. V0533 Tau |In the region of the Pleiades cluster. V0534 Tau |In the region of the Pleiades cluster. V0535 Tau |In the region of the Pleiades cluster. V0536 Tau |In the region of the Pleiades cluster. V0537 Tau |In the region of the Pleiades cluster. V0538 Tau |The member of the Pleiadea cluster. V0539 Tau |In the region of the Pleiades cluster. Possible member of the V0539 Tau |cluster. V0540 Tau |The member of the Pleiades cluster. V0541 Tau |The member of the Pleiades cluster. V0542 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0543 Tau |In the region of the Pleiades cluster. V0544 Tau |In the region of the Pleiades cluster. V0545 Tau |Max = 2444896.678 + 0.355d*E, M - m = 0.42P, A(V) = 0.09m [10052]. V0545 Tau |The member of the Pleiades cluster. V0546 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0547 Tau |In the region of the Pleiades cluster. V0548 Tau |In the region of the Pleiades cluster. Possible member of the V0548 Tau |cluster. V0549 Tau |In the region of the Pleiades cluster. V0550 Tau |The member of the Pleiades cluster. V0551 Tau |In the region of the Pleiades cluster. V0552 Tau |In the region of the Pleiades cluster. V0553 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0554 Tau |In the region of the Pleiades cluster. V0555 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0556 Tau |In the region of the Pleiades cluster. V0557 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0558 Tau |In the region of the Pleiades cluster. V0559 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0560 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0561 Tau |In the region of the Pleiades cluster. V0562 Tau |In the region of the Pleiades cluster. V0563 Tau |In the region of the Pleiades cluster. V0564 Tau |In the region of the Pleiades cluster. V0565 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0566 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0567 Tau |In the region of the Pleiades cluster. V0568 Tau |In the region of the Pleiades cluster. V0569 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0570 Tau |In the region of the Pleiades cluster. V0571 Tau |In the region of the Pleiades cluster. V0572 Tau |In the region of the Pleiades cluster. V0573 Tau |In the region of the Pleiades cluster. V0574 Tau |In the region of the Pleiades cluster. V0575 Tau |In the region of the Pleiades cluster. V0576 Tau |In the region of the Pleiades cluster. V0577 Tau |In the region of the Pleiades cluster. V0578 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0579 Tau |In the region of the Pleiades cluster. V0581 Tau |In the region of the Pleiades cluster. V0582 Tau |In the region of the Pleiades cluster. V0583 Tau |In the region of the Pleiades cluster. V0584 Tau |In the region of the Pleiades cluster. V0585 Tau |In the region of the Hyades cluster. V0589 Tau |In the region of the Hyades cluster. V0594 Tau |In the region of the Pleiades cluster. V0595 Tau |In the region of the Pleiades cluster. V0596 Tau |In the region of the Pleiades cluster. Possible member of the V0596 Tau |cluster. V0597 Tau |In the region of the Pleiades cluster. V0598 Tau |In the region of the Pleiades cluster. V0599 Tau |In the region of the Pleiades cluster. V0600 Tau |In the region of the Pleiades cluster. V0601 Tau |In the region of the Pleiades cluster. V0602 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0603 Tau |In the region of the Pleiades cluster. V0604 Tau |In the region of the Pleiades cluster. V0605 Tau |In the region of the Pleiades cluster. V0606 Tau |In the region of the Pleiades cluster. V0607 Tau |In the region of the Pleiades cluster. V0608 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0609 Tau |In the region of the Pleiades cluster. V0610 Tau |The member of the Pleiades cluster. V0611 Tau |In the region of the Pleiades cluster. V0612 Tau |In the region of the Pleiades cluster. V0613 Tau |In the region of the Pleiades cluster. Possible member of the V0613 Tau |cluster. V0614 Tau |In the region of the Pleiades cluster. V0615 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0617 Tau |In the region of the Pleiades cluster. V0618 Tau |In the region of the Pleiades cluster. V0619 Tau |In the region of the Pleiades cluster. V0620 Tau |In the region of the Pleiades cluster. V0621 Tau |In the region of the Pleiades cluster. V0622 Tau |In the region of the Pleiades cluster. V0623 Tau |The member of the Pleiades cluster. V0624 Tau |The value of P1(A1 = 0.01m) is given in the Table. P2 = 0.017d, A2 V0624 Tau |= 0.007m. The member of the Pleiades cluster. V0625 Tau |In the region of the Pleiades cluster. V0626 Tau |In the region of the Pleiades cluster. V0627 Tau |The member of the Pleiades cluster. V0629 Tau |In the region of the Pleiades cluster. V0630 Tau |In the region of the Pleiades cluster. V0631 Tau |The member of the Pleiades cluster. V0632 Tau |The member of the Pleiades cluster. V0633 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0634 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0635 Tau |The member of the Pleiades cluster. V0636 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0637 Tau |In the region of the Pleiades cluster. V0638 Tau |The member of the Pleiades cluster. V0639 Tau |In the region of the Pleiades cluster. V0640 Tau |In the region of the Pleiades cluster. V0641 Tau |Max = 2444896.744 + 1.22d*E; M - m = 0.5P, A(V) = 0.03m [10052]. V0641 Tau |The member of the Pleiades cluster. V0642 Tau |The member of the Pleiades cluster. V0643 Tau |The member of the Pleiades cluster. V0644 Tau |The member of the Pleiades cluster. V0645 Tau |In the region of the Pleiades cluster. Possible member of the V0645 Tau |cluster. V0646 Tau |The member of the Pleiades cluster. V0647 Tau |The value of P1(A1 = 0.011m) is given in the Table. P2 = 0.070d, A2 V0647 Tau |= 0.006m. The member of the Pleiades cluster. V0648 Tau |In the region of the Pleiades cluster. V0649 Tau |In the region of the Pleiades cluster. V0650 Tau |The member of the Pleiades cluster. V0651 Tau |In the region of the Pleiades cluster. V0652 Tau |The member of the Pleiades cluster. V0653 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0654 Tau |In the region of the Pleiades cluster. Possible member of the V0654 Tau |cluster. V0655 Tau |In the region of the Pleiades cluster. V0656 Tau |In the region of the Pleiades cluster. V0657 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0658 Tau |In the region of the Pleiades cluster. V0659 Tau |In the region of the Pleiades cluster. V0660 Tau |Max = 2444896.453 + 0.23541d*E, M - m = 0.5P, A(V) = 0.20m [10052]. V0660 Tau |The member of the Pleiades cluster. V0661 Tau |In the region of the Pleiades cluster. V0662 Tau |In the region of the Pleiades cluster. V0663 Tau |In the region of the Pleiades cluster. V0664 Tau |The member of the Pleiades cluster. V0665 Tau |In the region of the Pleiades cluster. Not a member of the region. V0666 Tau |In the region of the Pleiades cluster. V0667 Tau |The member of the Pleiades cluster. V0668 Tau |In the region of the Pleiades cluster. V0669 Tau |In the region of the Pleiades cluster. V0670 Tau |In the region of the Pleiades cluster. V0671 Tau |In the region of the Pleiades cluster. V0672 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0673 Tau |In the region of the Pleiades cluster. Possible member of the V0673 Tau |cluster. V0674 Tau |In the region of the Pleiades cluster. V0675 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0676 Tau |In the region of the Pleiades cluster. V0677 Tau |The member of the Pleiades cluster. V0678 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0679 Tau |The member of the Pleiades cluster. V0680 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0681 Tau |In the region of the Pleiades cluster. V0682 Tau |In the region of the Pleiades cluster. V0683 Tau |In the region of the Pleiades cluster. V0684 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0685 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0686 Tau |In the region of the Pleiades cluster. V0687 Tau |In the region of the Pleiades cluster. V0688 Tau |In the region of the Pleiades cluster. V0689 Tau |In the region of the Pleiades cluster. V0690 Tau |In the region of the Pleiades cluster. V0691 Tau |In the region of the Pleiades cluster. V0692 Tau |In the region of the Pleiades cluster. Possible member of the V0692 Tau |cluster. V0693 Tau |In the region of the Pleiades cluster. V0694 Tau |In the region of the Pleiades cluster. V0696 Tau |The member of the Hyades cluster. V0697 Tau |The member of the Hyades cluster. V0698 Tau |Type INB? V0700 Tau |The member of the Pleiades cluster. V0701 Tau |In the region of the Pleiades cluster. V0702 Tau |In the region of the Pleiades cluster. V0703 Tau |The member of the Pleiades cluster. V0705 Tau |In the region of the Pleiades cluster. V0706 Tau |In the region of the Pleiades cluster. V0707 Tau |In the region of the Pleiades cluster. V0709 Tau |In the region of the Pleiades cluster. V0710 Tau |VB A (B 16m, 3.5", 180{deg}). V0711 Tau |VB A (B 8.83m, A = 8.023", E = 0.18, Porb = 2101 yr); SB2 (Porb = V0711 Tau |2.83774d [10070]). Migration period of the distortion wave is about V0711 Tau |10.5 yr [10072]. The range of combined light variation is given. V0712 Tau |In the region of the Pleiades cluster. V0713 Tau |In the region of the Pleiades cluster. V0714 Tau |In the region of the Pleiades cluster. V0715 Tau |In the region of the Pleiades cluster. V0716 Tau |In the region of the Pleiades cluster. V0717 Tau |In the region of the Pleiades cluster. V0718 Tau |In the region of the Hyades cluster. V0725 Tau |SB1 (Porb = 110.8d [10076]). X-ray outbursts occur periodically V0725 Tau |near the periastron passages of the pulsar with P = Porb. The V0725 Tau |amplitude of the corresponding variations of visual brightness of V0725 Tau |the system A(V) = 0.03m. The period of pulsar rotation Prot var V0725 Tau |[10077]. Prot = 104.17s (JD2442531), 103.806s (JD2442728), 103.882s V0725 Tau |(JD2443505), 103.8402s (JD2443620) [10074]; 103.647s (JD2444521), V0725 Tau |103.423s (JD2445292), 103.3429ss(JD2445623) [10078]. V0726 Tau |Min II 11.2. V0727 Tau |In the region of the Pleiades cluster. V0728 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0729 Tau |Max = 2439024.46 + 152.35d*E (JD2438680 - 39415); Max = 2440127.78 V0729 Tau |+ 313.86d*E (JD2439415 - 40510). H2O maser. V0732 Tau |In the region of the Pleiades cluster. V0733 Tau |In the region of the Pleiades cluster. V0734 Tau |In the region of the Pleiades cluster. V0735 Tau |In the region of the Pleiades cluster. V0736 Tau |In the region of the Pleiades cluster. V0737 Tau |In the region of the Pleiades cluster. V0738 Tau |In the region of the Pleiades cluster. The chart in [08559] is V0738 Tau |wrong. V0739 Tau |In the region of the Pleiades cluster. V0740 Tau |In the region of the Pleiades cluster. V0741 Tau |In the region of the Pleiades cluster. V0742 Tau |In the region of the Pleiades cluster. V0743 Tau |In the region of the Pleiades cluster. V0744 Tau |In the region of the Pleiades cluster. V0746 Tau |In the region of the Pleiades cluster. V0747 Tau |In the region of the Pleiades cluster. V0748 Tau |In the region of the Pleiades cluster. V0749 Tau |In the region of the Pleiades cluster. V0750 Tau |In the region of the Pleiades cluster. V0751 Tau |In the region of the Pleiades cluster. V0752 Tau |In the region of the Pleiades cluster. V0753 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0754 Tau |In the region of the Pleiades cluster. V0755 Tau |In the region of the Pleiades cluster. V0756 Tau |In the region of the Pleiades cluster. V0757 Tau |In the region of the Pleiades cluster. V0758 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0759 Tau |In the region of the Pleiades cluster. V0760 Tau |In the region of the Pleiades cluster. V0761 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0762 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0763 Tau |In the region of the Pleiades cluster. V0764 Tau |In the region of the Pleiades cluster. V0765 Tau |In the region of the Pleiades cluster. V0767 Tau |In the region of the Pleiades cluster. V0768 Tau |In the region of the Pleiades cluster. V0769 Tau |In the region of the Pleiades cluster. V0770 Tau |In the region of the Pleiades cluster. V0771 Tau |In the region of the Pleiades cluster. V0772 Tau |In the region of the Pleiades cluster. V0773 Tau |There are also quasisinusoidal light variations with P = 3.43d and V0773 Tau |A(V) = 0.13m [10056]. V0774 Tau |VB A (B 6.96m, G5IV, 66.8", 315{deg}). V0775 Tau |The member of the Hyades cluster. V0776 Tau |VB A (B 7.5m, 1.4", 333{deg}, 1958; C 8.7m, 77.2", 233{deg}, 1925); V0776 Tau |SB1 (Porb = 57.25d). The member of the Hyades cluster. V0777 Tau |VB A (B 8.12m V, 0.0088", 173.2{deg}, 1980.6). The member of the V0777 Tau |Hyades cluster. V0778 Tau |Min II 17.0. P var. Min I = 2438680.546 + 0.434842d*E (JD2436528 - V0778 Tau |38841); Min I = 2439765.488 + 0.434846d*E (JD2439559 - 41031); V0778 Tau |since JD2440129 - see Table. V0780 Tau |VB A (B 15.8m V, 0.3", 310{deg}, 1974); {mu} = 0.364", P = V0780 Tau |163{deg}. V0781 Tau |Min II 9.3. V0782 Tau |In the region of the Pleiades cluster. V0783 Tau |In the region of the Pleiades cluster. V0784 Tau |In the region of the Pleiades cluster. V0785 Tau |The member of the Pleiades cluster. V0787 Tau |In the region of the Pleiades cluster. V0788 Tau |In the region of the Pleiades cluster. V0789 Tau |The member of the Pleiades cluster. V0790 Tau |The member of the Pleiades cluster. V0791 Tau |In the region of the Pleiades cluster. V0792 Tau |Near V752 Tau. Identical to it? In the region of the Pleiades V0792 Tau |cluster. V0793 Tau |The member of the Pleiades cluster. V0794 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0795 Tau |In the region of the Pleiades cluster. V0796 Tau |The member of the Pleiades cluster. V0797 Tau |In the region of the Pleiades cluster. Not a member of the cluster. V0798 Tau |In the region of the Pleiades cluster. V0799 Tau |In the region of the Pleiades cluster. V0800 Tau |In the region of the Pleiades cluster. V0801 Tau |In the region of the Pleiades cluster. V0802 Tau |In the region of the Pleiades cluster. V0804 Tau |In the region of the Pleiades cluster. V0805 Tau |The member of the Hyades cluster. V0807 Tau |VB A (B = GH Tau, 21.4", 193{deg}). V0808 Tau |Porb = 11.93d. The member of the Hyades cluster. V1144 Tau |SB, Porb = 13.88d. V1148 Tau |Type LBV: is also possible. SB, Porb = 2.2075d. V1152 Tau |Type E: with P = 11.080d is also possible. V1161 Tau |Variability needs confirmation. V1212 Tau |Dwarf nova in Taurus. V1226 Tau |Variable brown dwarf. V1229 Tau |MinII 6.88. V1230 Tau |MinII 14.49. V1234 Tau |MinII 12.9. V1237 Tau |The depth of MinII is 0.19. V1238 Tau |MinII 8.87. V1239 Tau |MinII 10.76. V1241 Tau |The depth of Min II 0.22m. The primary component var, DSCT:, P1 = V1241 Tau |0.16454d, P2 = 0.13721d. V1243 Tau |VB (A 9.1m var, F1; B 9.9m, F8:, 0.3", 24{deg}, 1991). V1248 Tau |OH maser. V1258 Tau |SiO maser. V1260 Tau |MinII - MinI = 0.57P. V1268 Tau |VB A (B 7.8m, A2V, 7", 207{deg}, 2004). V1282 Tau |SB2, Porb > 6000d? V1283 Tau |SB1, Porb = 7.05051d. V1284 Tau |Min II = 15.17. V1287 Tau |Min II = < 8.69. MinII - MinI = 0.39P. V1295 Tau |Min II = 11.35. V1299 Tau |VB AB (9.3m, 9.3m, 0".4, 252{deg}, 2007). V1304 Tau |SB. V1305 Tau |Amplitude(Min II)= 0.2mag. V1311 Tau |Min II = 14.59. V1322 Tau |P = 0.585d is also possible. V1326 Tau |P = 1.651d is also possible. V1332 Tau |Min II = 11.78. Possily a pulsating star with a twice shorter V1332 Tau |period. V1337 Tau |SB2. V1345 Tau |P = 11.66d is also effect. V1347 Tau |SB2. V1350 Tau |SB2. V1352 Tau |Min II = 13.1 :. V1355 Tau |Min II = 14.2. V1356 Tau |Min II = 11.37. MinII - MinI = 0.57P. V1364 Tau |VB AB. V1367 Tau |Min II = 11.15. V1369 Tau |Min II = 12.43. V1370 Tau |Min II = 11.28. V1374 Tau |Min II = 13.9. V1384 Tau |Multiperiodic. P1 is presented in the Table; P0 = 0.1397914d. V1392 Tau |Multiperiodic. P0 is presented in the Table; P1 = 0.0579031d. V1403 Tau |Close VB. V1412 Tau |P=0.3409505d is also possible. V1414 Tau |P = 0.195018d is also possible. alf Tau |VB A (B 13.5m, M2V, 31", 110{deg}). The star is surrounded by an alf Tau |infrared emission envelope with the diameter of about 10". In the alf Tau |region of the Hyades cluster. zet Tau |Min II 3.05. tet 2 Tau |VB A (B 4.85m, 0.02077", 19.6{deg}, 1980.59); SB1 (Porb = 140.728D, tet 2 Tau |E = 0.75 [10087]). The value of P1(A1 = 0.017m B) is given in the tet 2 Tau |Table. P1 var. Later P1 = 0.07541d (A1 = 0.023m B), P2 = 0.0831d tet 2 Tau |(A2 = 0.013m B). Possibly eclipsing with the elements: Min = tet 2 Tau |2445358.38 + 140.734d*E, A = 0.02m B. The member of the Hyades tet 2 Tau |cluster. lam Tau |Min II 3.54. Triple system. The eclipsing system rotates around the lam Tau |third component with P = 33.025d [10090]. In the region of the lam Tau |Hyades cluster. rho Tau |The member of the Hyades cluster. ups Tau |VB A (B 6.5m, 0.020"). The member of the Hyades cluster. S Tel |The AAVSO chart, approved by Harvard Observatory in 1951, S Tel |corresponds to the star at the coordinates in the Table. Most S Tel |observations of S Tel reported in the 20th century probably refer S Tel |to this star. There remains doubt if the original CPD-55 9313 was S Tel |the same star [N0030]. U Tel |P var [00001]. SiO maser. RR Tel |A symbiotic Nova. In 1889 - 1930, 12m - 14m pg (according to RR Tel |[00625], irregular variations; according to [00017], Max = 2411490 RR Tel |+ 384d*E, with irregularities). In 1930 - 1944, 12.5m - 16.5m pg, RR Tel |Max = 2430145 + 386.73d*E [01649]. An outburst from 14m to 7m in RR Tel |October, 1944. On JD2441426 - 2444899, 5.06m - 6.74m J, P = 387d RR Tel |[09989]. The data in [N0002] reveal current $V$-band variations RR Tel |with a small amplitude and nearly the same period [00001]. A period RR Tel |of 11.38 years, presumably the orbital one, was reported in RR Tel |[N0031]. The spectrum in the Max of the outburst was F5 without RR Tel |emissions, then a rich emission spectrum was formed. Since the RR Tel |1970s, TiO absorption bands are being noted. Radio source, soft RR Tel |X-ray source. RS Tel |Semiregular variations, P = 49.0d [N0002]. RV Tel |VB (0.6", 294{deg}, 1946). SS Tel |SiO maser. SU Tel |VB B (A 13.6m B, 12" nf). TY Tel |OH, SiO maser. UY Tel |VB. YY Tel |No emission lines in the spectrum. AG Tel |VB A (B 13.7m B, 20" sp). AN Tel |A secondary period about 27d. AX Tel |[A/H] = -0.7. BB Tel |Not red [00001]. BI Tel |[Fe/H] = -1.96. BL Tel |[Fe/H] = -0.66. The depth of Min II is about 0.1m. The primary BL Tel |component varies approximately between 7.09m and 7.27m V, the BL Tel |periods revealed in these pulastins are 92.5d and 64.8d [N0033]. BO Tel |[A/H] = -0.3. CK Tel |VB B (A 15.0m, 12" s). DZ Tel |VB A (B 15.9m, 15" np). EH Tel |VB A (B 15.6m R, 5" nf). EU Tel |The chart in [06286] is wrong. FX Tel |VB (4"). GM Tel |VB A (B 16.6m, 10" p). HH Tel |[Fe/H] = -1.02. HR Tel |Type EW with a twice longer period is possible. HY Tel |[Fe/H] = -0.17. KK Tel |Porb = 0.08453d. KN Tel |VB A (B 15.6m B, 13" sf). LW Tel |Possibly identical to NSV10695. MT Tel |[Fe/H] = -1.85. NS Tel |Strong O'Connell effect. PS Tel |V39 (NGC 6584). Cluster non-member? P = 0.1422d or 0.1657d is PS Tel |possible. PT Tel |V27 (NGC 6584). Cluster non-member. PU Tel |V24 (NGC 6584). Cluster non-member. PV Tel |SB2. PX Tel |V15 (NGC 6584). Cluster non-member. PZ Tel |SB2. QR Tel |P(osc) = 13.0 min. QS Tel |Porb = 0.097187d. QU Tel |Multiperiodic, P = 257s is dominant. QZ Tel |VB B (A 9" sp). The variability is probably due to the fainter (B) QZ Tel |component [HIP]. The variability range for combined light is given. V0340 Tel |The data from [N0002] do not confirm the tabulated period [00001]. V0343 Tel |O'Connell effect, MaxII 9.18m. V0349 Tel |Multiperiodic, P2 = 1.2719d. V0356 Tel |MinII - MinI = 0.48P. V0358 Tel |A twice shorter period is not excluded. V0359 Tel |MinII - MinI = 0.78P. VB (8.8m, 11.4m, 4", 239{deg}, 1991). V0362 Tel |VB (9.5m, 12.2m, 3", 140{deg}, 1991). V0368 Tel |P varies, dP/dt = -0.18 x 10^(-5) d/yr. V0374 Tel |The first-overtone period is tabulated; for the fundamental mode, P V0374 Tel |= 0.47907d. V0379 Tel |VB A (B 18.52m, 2.4"). V0381 Tel |VB (11", 6{deg}, 2000); combined magnitudes are tabulated. For the V0381 Tel |first-overtone period, see the Table; P0 = 0.46781d; the amplitude V0381 Tel |ratio (1O/F) is 1.05. V0384 Tel |VB A (B 6.5",40{deg}, 1999). V0388 Tel |Double-mode pulsations. P0 is given in the Table, P1 = 0.1127701d. V0388 Tel |P1/P0 = 0.7564. V0389 Tel |Blazhko effect, P = 10.82d. V0398 Tel |VB A (B 14.4mB, 10", 8{deg}, 2000). V0409 Tel |Type EW with a twice longer period is also possible. V0418 Tel |P varies. V0432 Tel |P = 52.3d is superposed. V0436 Tel |A twice longer period is not excluded. V0445 Tel |VB A (B 4", 322{deg}, 2000). V0466 Tel |VB A (B 15.1mG, 10", 91{deg}, 2000); the range in the Table can be V0466 Tel |influenced by the companion. V0470 Tel |P varies. V0475 Tel |O'Connell effect. V0478 Tel |Blazhko effect. V0487 Tel |Blazhko effect, P(Bl) = 52.8d. V0488 Tel |Blazhlo effect, P(Bl) = 37d. V0489 Tel |VB A (15.1mG; B 16.0mG, 5", 233{deg}, 2000). V0507 Tel |VB B (A 14.8mG; B 15.3mG, 3", 69{deg}, 2000). The range in the V0507 Tel |Table is for combined brightness. R Tri |P var. Max = 2412167 + 267.3d*E (JD2412000 - 16000); Max = 2416972 R Tri |+ 262.6d*E (JD2416000 - 20000); since JD2420000 - see Table. Maser R Tri |(H2O). S Tri |P var. Max = 2418541 + 248.9d*E (JD2418000 - 31000); since S Tri |JD2431000 - see Table. T Tri |P var. Max = 2420535 + 320.6d*E (JD2420000 - 27000); since T Tri |JD2427000 - see Table. U Tri |{Delta}(S) = 1.3. V Tri |Min II 11.0. X Tri |VB A (B 13.3m, 6.7", 55.3{deg}, 1952). Usual brightness in Max X Tri |8.88. d = 0.013P; Min II 9.07. According to [10043], a two-peaked X Tri |flare-like event of 35 min duration ({Delta}(V) = 0.33m) was X Tri |observed at JD2445594.4550. P var. Min = 2422722.269 + 0.9715342d*E X Tri |(JD2422700 - 26600); Min = 2426946.508 + 0.9715390d*E (JD2426600 - X Tri |33400); Min = 2433504.397 + 0.9715290d*E (JD2433400 - 35500); Min = X Tri |2435687.422 + 0.9715352d*E (JD2435500 - 39200); Min = 2439375.373 + X Tri |0.9715277d*E (JD2439200 - 42500) [07603]; since JD2442500 - see X Tri |Table. Y Tri |Var No.2 (M33). VB A (B 17.28m B, 26.4" np). RS Tri |VB A (B 11.98m, 6.0", 214{deg}, 1962). d = 0.016P; Min II 10.4, Min RS Tri |II - Min I = 0.56P. RU Tri |VB A (B 12m, 21.8", 88{deg}). Min II 11.8:. RW Tri |The depth of Min I 1.12m - 2.21m. D = 0.052P - 0.086P, d ~0.03P. P RW Tri |var? [03434,09858, 9859]. Strong fluctuations of light outside RW Tri |eclipses. the lower the brightness outside the eclipse, the deeper RW Tri |the Min. In J, K light Min II of 0.16m J depth was found at the RW Tri |phase 0.50P [10053]. Flat spectrum of the accretion disc with RW Tri |emission lines. RX Tri |Max = 2426577 + 192d*E (JD2426500 - 31800); since JD2432800 - see RX Tri |Table. According to [04029], P = 100d? RY Tri |Red. ST Tri |Min II 14.5. SW Tri |Blazhko effect is possible. SY Tri |Blazhko effect is possible. TT Tri |In the region of the galaxy M 33. TZ Tri |ADS 1697 A (B 6.72m, F6V, SB2, Porb = 2.2365d, 3.9", 71{deg}, TZ Tri |1973); SB2 (P = 14.732d). Secondary variations on ~100d time scale. TZ Tri |H and K CaII emission was noted only for one of the two G-stars. AW Tri |Min II = 13.7. AY Tri |Min II = 14.45. AZ Tri |Min II = 14.3. BB Tri |Min II = 14.3 :. BC Tri |Min II = 12.08. Type RRC with a twice shorter period is possible. BE Tri |Min II = 13.2. BF Tri |Min II = 14.5 :. BI Tri |Min II = 12.65. VB AB (4", 227{deg}, 1997). BM Tri |Min II = 13.3 :. BO Tri |Min II = 12.0. BP Tri |Min II = 14.6. BQ Tri |Min II = 12.8. BR Tri |Min II = 13.3. BT Tri |Min II = 14.7. BU Tri |Min II = 14.9. BV Tri |Min II = 14.3. BX Tri |Min II = 12.60. CC Tri |Min II = 13.6. CD Tri |Min II = 12.3. CL Tri |Min II = 12.07. CM Tri |Min II = 14.3. CN Tri |Min II = 12.25. CP Tri |Min II = 10.95. The identification with the missed BD star, BD +33 CP Tri |460 = NSV 00856, suggested in [80121] seems unjustified. CR Tri |Min II = 14.7. CS Tri |Min II = 11.4. DE Tri |P = 30.6d is not excluded. DI Tri |P1 is presented in the Table. P0 = 0.559708d; P1/P0 = 0.7459. DK Tri |VB B (A = GCVS NAME!!!; AB 14", 211{deg}, 2016). DL Tri |VB A (B = GCVSNAME!!!, 14", 211{deg}, 2016). alf Tri |SB (Porb = 1.767 d). R TrA |SB? U TrA |For moments of Max0 (fundamental mode) see Table. Max1 (first U TrA |overtone) = 2443266.05 + 1.824881d*E. RR TrA |Min II 10.60, dII = 0.025P. RW TrA |(k - b)2 = 0.30. {Delta}(S) = 1. SU TrA |The chart in [06286] is wrong. TW TrA |VB. TY TrA |The chart in [06286] is wrong. UW TrA |The chart in [06286] is wrong. UZ TrA |The chart in [06286] is wrong. XX TrA |The chart in [06286] is wrong. XY TrA |The chart in [06286] is wrong. BH TrA |According to [04637], L type. CI TrA |Possibly P < 0.3d. DI TrA |The chart in [06286] is wrong. DV TrA |Three Max and three Min are observed during a cycle. Max1 ({phi} = DV TrA |0.0P) 13.2m; Max2 ({phi} = 0.2P) 14.2m; Max3 ({phi} = 0.6P) 13.5m. DV TrA |Min1, Min2, Min3 ~16.0m. DZ TrA |The chart in [06286] is wrong. EH TrA |Shallow Min II is possible. EK TrA |n star of a pair. For the mean cycle between normal maxima see EK TrA |Table. The mean cycle between supermaxima 442.1d (JD2435200 - EK TrA |39700), 551.5d (JD2439700 - 44050). Superhumps ({delta}(M) = 0.26m EK TrA |V) with P = 0.06492d, M - m = 0.26P [09945]. EL TrA |Min II 10.9. EM TrA |Min II 10.4. EN TrA |According to [07934], RV: type. EP TrA |Min II 9.5. EQ TrA |Min II 9.0. P var. Min = 2416267.614 + 2.709220d*E (JD2416000 - EQ TrA |29000); since JD2429000 - see Table. ER TrA |P > 220d. FH TrA |The elements need confirmation. FK TrA |The elements need confirmation. FM TrA |P >= 220d. GN TrA |Min II 12.0. GR TrA |Blazhko effect. HP TrA |Deep Min II. The elements need improvement. HV TrA |Min II? 14.8. Min II - Min I = 0.55P. IM TrA |P >= 150d. Epoch of Min is given. IW TrA |Min II 14.5:. The elements need confirmation. KX TrA |2U 1639-62? P.K.326 -10{deg} 1. Gas velocities up to 5000 km/s KX TrA |[09958]. KY TrA |TrA X-1 = A1524-61. KZ TrA |4U 1626-67. Lx/Lopt ~2000. VB B (A 14.9m; B25", 189{deg}). KZ TrA |Barycentric period parameters for pulses [04534]: Min = JED KZ TrA |2443931.2394789; P = 7.6776762s, DP/dt = (-4.95 +-0.02)*10**(-11). KZ TrA |{Delta}(m) pulse = 0.02m - 0.17m. Porb = 2491.06s or 2492.32s KZ TrA |[04558]. Flares with {Delta}(m) up to 0.4m with intervals ~20 min KZ TrA |correlated with X-ray flares [04536]. LM TrA |The chart in [08661] is wrong. LP TrA |VB A (B 11.5m, 25", 123{deg}; C 12.0m, BC 6"). MZ TrA |MinII 8.73. NO TrA |MinII 8.85. NT TrA |MinII - MinI = 0.57P. NY TrA |VB A (B 5", 62{deg}, 2000). V0336 TrA |Min II = 11.1. V0338 TrA |VB A (6.3mJ; B 10.3mJ, 7", 265{deg}, 2000). V0344 TrA |VB B (A = NEXT STAR IN THE LIST; AB 13", 304{deg}, 2000). V0345 TrA |VB A (B = PREVIOUS STAR IN THE LIST, 13", 304{deg}, 2000). V0347 TrA |Blazhko effect, P=118.05d. V0348 TrA |Double-mode pulsations. The Table contains light elements for the V0348 TrA |first overtone. Second overtone: Max = 2453600.091 + 0.1224057d x V0348 TrA |E. P2/P1 = 0.8279. V0351 TrA |P = 49.5d is superposed. V0362 TrA |Several close companions. T Tuc |P var. Max = 2410138 + 250.76d*E (JD2410000 - 14400); Max = 2414900 T Tuc |+ 248.88d*E (JD2414400 - 22000); Max = 2432160 + 250.00d*E T Tuc |(JD2422900 - 35000); since JD2437700 - see Table. U Tuc |In the region of the Small Magellanic Cloud. SMS non-member. P var. U Tuc |Max = 2421190 + 258.12d*E (JD2412600 - 22000); Max = 2427487 + U Tuc |262.83d*E (JD2422000 - 28000); Max = 2437808 + 257.70d*E (JD2428000 U Tuc |- 39150); since JD2440900 - see Table. V Tuc |In the region of the Small Magellanic Cloud. SMS non-member. The V Tuc |depth of Min II 0.11m. W Tuc |(k - b)2 = 0.09, {Delta}(S) = 7:. P var? RR Tuc |In the region of the Small Magellanic Cloud. VB A (B 17m, 6", RR Tuc |90{deg}). RV Tuc |In the region of the Small Magellanic Cloud. VB. SS Tuc |In the region of the Small Magellanic Cloud. HV 1877. Earlier was SS Tuc |erroneously identifded with HV 1887. SU Tuc |In the region of the Small Magellanic Cloud. HV 1922. According to SU Tuc |[09980], alternatively may be identical to HV 1920. SX Tuc |In the region of the Small Magellanic Cloud. VB (B 16m? P). SY Tuc |In the region of the Small Magellanic Cloud. Min II 15.4. TV Tuc |In the region of the Small Magellanic Cloud. The variable's TV Tuc |position in 2' to the north of CPD -73{deg} 64 [09980] makes it TV Tuc |impossible to identify it with HV 2041. TZ Tuc |In the region of the Small Magellanic Cloud. SMS non-member. VB A TZ Tuc |(B 13m sp). UW Tuc |In the region of the Small Magellanic Cloud. SMC non-member. UX Tuc |In the region of the Small Magellanic Cloud. SMS non-member.In the UX Tuc |neighbourhood OF 47 Tuc; probably cluster non-member. P var. [Fe/H] UX Tuc |= -1.8. YY Tuc |The elements need improvement; current elements with the epoch from YY Tuc |[07984] are given. (k - b)2 = 0.03. {Delta}(S) = 8:. AD Tuc |In the region of the Small Magellanic Cloud. SMS non-member. AD Tuc |{Delta}(S) = 4.9. AF Tuc |In the region of the Small Magellanic Cloud. SMS non-member. AH Tuc |In the region of the Small Magellanic Cloud. SMS non-member. P var. AI Tuc |In the region of the Small Magellanic Cloud. SMS non-member. In the AI Tuc |region of the globular cluster NGC 362. P var. AK Tuc |In the region of the Small Magellanic Cloud. SMS non-member. P var. AL Tuc |In the region of the Small Magellanic Cloud. SMS non-member. AM Tuc |The elements should be checked. [Fe/H] = -1.82. {Delta}(S) = 9.9. AO Tuc |The elements need improvement. {Delta}(S) = 5. AP Tuc |In the region of the Small Magellanic Cloud. SMS non-member. AQ Tuc |In the region of the Small Magellanic Cloud. SMS non-member.In the AQ Tuc |region of the globular cluster 47 Tuc. Min II 10.48. AR Tuc |In the region of the Small Magellanic Cloud. SMS non-member. AU Tuc |In the region of the Small Magellanic Cloud. SMS non-member. AV Tuc |In the region of the Small Magellanic Cloud. SMS non-member. BD Tuc |In the region of the Small Magellanic Cloud. SMS non-member. BE Tuc |In the region of the Small Magellanic Cloud. BF Tuc |In the region of the Small Magellanic Cloud. [A/H] = -0.7. BG Tuc |In the region of the Small Magellanic Cloud. SMS non-member. BH Tuc |In the region of the Small Magellanic Cloud. VB A (B 14.28m, 10" BH Tuc |n). BS Tuc |(k - b)2 = 0.10. BZ Tuc |P var. Max = 2429849.448 + 127.78d*E (JD2410000 - 35100) [03641]; BZ Tuc |Max = 2441193.541 +127.27d*E (JD2435100 - 43500) [A.M. van BZ Tuc |Genderen, AsAp Suppl 52, 423, 1983]; since JD 2443500 - see Table. CF Tuc |In the region of the Small Magellanic Cloud. SMS non-member. Soft CF Tuc |X-ray source. Distortion wave. {Delta}(m) = 0.057m [10065]. Min II CF Tuc |7.52. DX Tuc |Type RRC: is also possible. EM Tuc |Min II = 12.6. EN Tuc |Min II = 8.61. EP Tuc |Blazhko effect, P = 63d. EX Tuc |SB2. EY Tuc |In the region of the SMC galaxy, non-member. tet Tuc |For the period of the main oscillation (A = 0.0132m) see Table. tet Tuc |Other instable frequences were also noted. R UMa |Maser (H2O). S UMa |S 1.5/6 e. P var. Max = 2398325 + 224.51d*E (JD2394000 - 2405000); S UMa |Max = 2405290 + 230.20d*E (JD2405000 - 10500); Max = 2417530 + S UMa |223.96d*E (JD2410500 - 23500); Max = 2426324 + 228.53d*E (JD2423500 S UMa |- 28800); since JD2428800 - see Table. T UMa |Maser (H2O). W UMa |ADS 7494 A (B 12.35m, 6.5", 44{deg}, 1963). dI = 0.037P; Min II W UMa |8.43, dII = 0.028P. Soft X-ray source. LX/Lbol = 1.7*10**(-4). P W UMa |var. Min I = 2420980.8093 + 0.333638880d*E (JD2416000 - 21000); Min W UMa |I = 2420980.8093 + 0.333636993d*E (JD2421000 - 33000) [01760]; Min W UMa |I = 2435918.4169 + 0.33363832d*E (JD2433000 - 41000) [05327]; since W UMa |JD2441000 - see Table. The light curve shape, including depths of W UMa |minima, var. A moving wave with {Delta}(m) = 0.025m y and P ~1100d W UMa |[10067] was noted. A flare ({Delta}(m) = 1.5m, {lambda} 3300 A, W UMa |{delta}({lambda}) = 50 A, JD2438511.7, {delta}(t) = 7 min) was W UMa |announced [05788]. The system contains gaseous streams, dark spots W UMa |on the surface of the components. H and K CaII emission. Z UMa |Usually 2 Max and 2 Min during a cycle. RV UMa |P var. Max = 2417861.434 + 0.4680618d*E (JD2417800 - 25000); Max = RV UMa |2425053.675 + 0.4680654d*E (JD2425000 - 29000) [00188]; Max = RV UMa |2438459.945 + 0.468062d*E (JD2429000 - 40000) [03506]; since RV UMa |JD2440000 - see Table. Blazhko effect, Pi = 92.12d (JD2436229 - RV UMa |38114) [09835]. Pi var. [Fe/H] = -1.04; {Delta}(S) = 3.5. RW UMa |DI < 0.08P; Min II 10.34, DII = 0.10P. [Fe/H]A = -0.1, [Fe/H]B = RW UMa |-1.0. P var? Distortion wave, A = 0.11m V. SU UMa |The cycle of normal maxima 5d - 35d [09782,03791]. Three different SU UMa |mean values of the mean cycle of supermaxima change each other SU UMa |being active at different time intervals: P1 = 161.5d; P2 = 203.9d; SU UMa |P3 = 248.1d (P = 201.7d) [09276]. Porb = 2.06d/N (N = 26, 27, 28) SU UMa |or 3.1h. Surrounded by a faint halo (28' diameter) of soft X-ray SU UMa |sources. SW UMa |SB. Superior conjunction of the accretion disc T = 2445376.8601 + SW UMa |0.0567433d*E [09836]. SX UMa |P var strongly. Before JD2418800 Max = 2416200.486 + 0.3071148d*E; SX UMa |Max = 2418800.213 + 0.3071345d:*E (JD2418800 - 22500) [00001]; Max SX UMa |= 2422653.5032 + 0.30711855d*E (JD2422500 - 26000) [10083]; Max = SX UMa |2426400.418 + 0.3071555d*E (JD2426000 - 29500); Max = 2430000.250 + SX UMa |0.3071301d*E (JD2429500 - 34000), Max = 2438508.751 + 0.3071363d*E SX UMa |(JD2434000 - 39000); since JD2441500 - see Table. [Fe/H] = -1.82, SX UMa |{Delta}(S) = 9.9. TU UMa |P var [03506]. [Fe/H] = -1.05, {Delta}(S) = 7.6. TW UMa |d = 0.002P; Min II 12.3:. TX UMa |Min II 7.13. P var. Min I = 2416426.801 + 3.063297d*E (JD2416000 - TX UMa |22000); Min I = 2427926.492 + 3.063337d*E (JD2424200 - 30000); Min TX UMa |I = 2433440.431 + 3.063300d*E (JD2430000 - 38000) [09839]; since TX UMa |JD2438000 - see Table. TY UMa |P var, non-linear term: +6.4d*10**(-11)*E**2. dI = 0.05P, dII = TY UMa |0.00P. The light curve shape var. 12.10 <= Min I <= 12.14, 12.06 <= TY UMa |Min II <= 12.12. UX UMa |The shape of the eclipse light curve, the mean level of light UX UMa |outside eclipses, the depth of Min var. Deviations from the UX UMa |tabulated elements may reach +-0.002d. Rapid brightness UX UMa |oscillations (28.54s <= P <= 30.02s) are sometimes observed UX UMa |[07304]. Soft X-ray source. UY UMa |Min II 12.9. VV UMa |Min II 10.26. P var. Min I = 2439245.408 + 0.6873793d*E (JD2425600 VV UMa |- 40200) [09843]; Min I = 2440768.6280 + 0.687367d*E (JD2440200 - VV UMa |42700); since JD2442700 - see Table. VX UMa |Maser (H2O). WX UMa |Mu {alpha} = -0.4094s, {mu} {delta} = +0.955", VB B (A = BD WX UMa |+44{deg} 2051, dM2, 8.74m V; B 28", 133{deg}; common {mu}). Soft WX UMa |X-ray source. LX/LV = 0.095. XY UMa |Mu {alpha} = -0.0055s, {mu} {delta} = -0.175". P var. Non-linear XY UMa |term: +2.77d*10**(-11)*E**2. The brightness outside eclipses var by XY UMa |0.16m V. The depth of Min I is 0.48m - 0.67m, that of Min II is XY UMa |0.19m. Migrating wave. XZ UMa |Min II 10.2. P var? Min = 2444986.445 + 1.2223105d*E (JD2414990 - XZ UMa |45000); since JD2445000 - see Table. AA UMa |Min II 11.53, Max II 10.94. The elements should be checked. AC UMa |VB B (A = BD + 65G671, 9.97m V, B-V = +0.50m; B 19", 114{deg}, AC UMa |1957). The chart in [08953] is wrong. AD UMa |Blazhko effect is possible. Pi = 35d - 40d, {delta}(A) = 0.2m. AE UMa |The fundamental mode P0 is given in the Table. P1 = 0.066527d, AE UMa |Pbeat = 0.293616d [09869]. Max 10.86 - 11.10, Min 11.46 - 11.52. AF UMa |d = 0.05P. AK UMa |The elements need improvement. AN UMa |The epoch of Min for periodic (P = Porb) light variations with A <= AN UMa |1m B is given. Min II is present. B - V = 0.0 in Max light, +0.5 AN UMa |during an eclipse; U - B = -1.1. Circular polarization in B light AN UMa |-9% to -35%; linear polarization 0% - 13% with a sharp Max near Max AN UMa |light. Rapid changes (A = 0.03m, f = 0.4 - 0.8 Hz). The mean light AN UMa |level and the light curve shape var. During the low state (B ~19m) AN UMa |the light variability with porb disappears, emission lines occur AN UMa |only during 10% of Porb, IR excess is noted. Soft X-ray source, AN UMa |var. Emissions of H, HeI, He II, NIII, FeII. AW UMa |dI = 0.06P:; Min II 7.08, dII = 0.11P. The light curve shape var. P AW UMa |var. Min I = 2442150.4385 + 0.43873234d*E (JD2438000 - 42200); AW UMa |since JD2442200 - see Table. AX UMa |P var. Max = 2435951.354 + 0.53510d*E (JD2435900 - 38200) [04375]; AX UMa |during JD2445000 - 45900 - see Table. BE UMa |d = 0.006P. Outside eclipses var 14.8m <= B <= 16.0m (reflection BE UMa |effect). The depth of eclipses for {lambda} lambda 3330 - 3700 A is BE UMa |greater than 4.3m,that for {lambda} lambda 5265 - 6005 A is 1.5m. BG UMa |Min II 10.93. Alternative type EW. BH UMa |Min II 12.3. BI UMa |Min II 15.8. BK UMa |[Fe/H] = -1.29, {Delta}(S) = 6.6. BL UMa |Min II 16.2. BM UMa |The depth of Min II 0.80m. BN UMa |[Fe/H] = -1.65, {Delta}(S) = 8.9. BP UMa |D <= 0.04P. The elements need confirmation. CE UMa |In the region of the cluster of galaxies Abell 1213. SN 1966 CE UMa |{omicron}? CF UMa |Groombridge 1830 B (A = BD +38{deg} 2285, V = 6.45m, B - V = CF UMa |+0.75m, G8 subdwarf, B 2", 165{deg}). A possible flare on February CF UMa |27, 1968. A brightening of the combined light by 0.6m pg on April CF UMa |27, 1939 [09881]. Maybe the object does not exist [09882]. CH UMa |X-ray source 1E 1003 +67. LX/Lopt = 0.04. CM UMa |P var? CQ UMa |The epoch of Max in U and B light coinciding with that of Min in V CQ UMa |light is given. A(U) = 0.06m, A(B) = 0.06m. CR UMa |The elements for Max in U light are given. In B and V bands no CR UMa |periodicity is apparent. A(U) = 0.03m. CW UMa |Mu = 0.27", P = 300{deg}. DF UMa |ADS 8242A (B 11.4m, 1.8", 60{deg}, 1960). The data for combined DF UMa |brightness are given in the Table. SB1, Porb = 1.033824d. Mu DF UMa |{alpha} = +0.0131s, {mu} {delta} = -0.038". Besides rapid DF UMa |variations (V = 10.14m, {Delta}(V) = 0.05m), long term variations DF UMa |are possible. DG UMa |Blazhko effect is possible. DK UMa |Soft X-ray source, lg Lx/Lv = -3.5. [Fe/H] = -0.38. DL UMa |Eclipses with P = 0.42d [04706]. DM UMa |SB1 (Porb = 7.492d). Min = 2444026.97 + 7.478d*E (1979 - 1982); DM UMa |1981 - 1984 - see Table. Two Min in the light curve in 1981 - 1982. DN UMa |ADS 8347 ABC (A 7.2m vis; B 9.0m vis, 0.121", 142.0{deg}, 1981.5; C DN UMa |8.3m vis, 4.0", 42{deg}, 1980; D = BS 4561, A1pCrEuSr:, V = 7.03m, DN UMa |B - V = +0.01m, 63.0", 114{deg}). The range of combined brightness DN UMa |for the three components is given. It is not known which of the DN UMa |components varies. The component D was used as a comparison star. DN UMa |Min II 6.73, Min II - Min I = 0.504P. GM UMa |SB, discrepant Porb = 3.2424d. HH UMa |Type EW: is also possible. HN UMa |Type DSCT: is also possible. HU UMa |VB A (B = GSC 3014.0222 = L265-581, 24", 250 {deg}, common proper HU UMa |motion). II UMa |Type RR: is also possible. LU UMa |SB1, Porb = 13.572 d. MM UMa |Variable brown dwarf. MS UMa |MinII 12.50. MT UMa |MinII 12.09. MV UMa |SB. NO UMa |SB2? NS UMa |The period was improved in [79045] compared to [79025] using new NS UMa |data. VB A (B 12.5mV, 15", 48{deg}, 1999). The tabulated amplitude NS UMa |was influenced by the companion. NT UMa |A twice shorter period is possible [79100]. NU UMa |A twice shorter period is not excluded. VB (A 9.6mHp; B 11.9mHp, NU UMa |1.1", 39{deg}, 1991). NY UMa |Porb = 42.628d. OR UMa |Min II = 12.4. OT UMa |Min II = 12.48. OV UMa |Min II = 11.10. OX UMa |Min II = 12.14. OY UMa |Min II = 13.3. PP UMa |Blazhko effect, P = 46d:. PS UMa |Min II = 12.78. MinII - MinI = 0.466P. PU UMa |Light elements for eclipsing variations in quiescence (19.1m - PU UMa |21.2m) are tabulated. PV UMa |SB, Porb = 80.53d. PW UMa |Min II = 11.5. PX UMa |Slow variations on time scale of several days are also present. PZ UMa |Min II = 13.1. QQ UMa |Min II = 14.1. QT UMa |Min II = 11.70. QV UMa |Min II = 14.25. V0337 UMa |Min II = 14.20. V0342 UMa |The depth of MinII is 0.40 mag. V0343 UMa |Min II = 14.35. V0351 UMa |Porb = 0.0992d. V0354 UMa |Min II = 11.12. V0355 UMa |The white-dwarf pulsation period is tabulated, with an amplitude V0355 UMa |about 0.05m. Another period detected photometrically is 320 minutes V0355 UMa |or 344 minutes. Porb = 0.0573083d. V0356 UMa |Min II = 13.0. V0357 UMa |Min II = 12.8. V0358 UMa |Min II = 12.45. V0359 UMa |Multiperiodic. V0360 UMa |Min II = 14.0. V0362 UMa |Min II = 14.6. V0363 UMa |Min II = 14.0. V0364 UMa |Min II = 13.95. V0365 UMa |Min II = 13.10. V0366 UMa |Min II = 14.2 :. V0374 UMa |Multiperiodic, 4 harmonics. V0379 UMa |P1 is given in the Table. P0 = 0.494909d, P1/P0=0.7446. V0380 UMa |Pulsates in the first overtone (see Table) and fundamental (Max = V0380 UMa |2454876.9243 + 0.47451d x E) modes. P1/P0 = 0.743. V0384 UMa |Type EW with a twice longer period is also possible. V0389 UMa |Double-mode pulsations. The Table gives the first-overtone light V0389 UMa |elements. For the fundamental mode, Max = 2454847.9552 + 0.47119d x V0389 UMa |E. P1/P0 = 0.744. V0415 UMa |P = 1.56575d is also possible. V0417 UMa |O'Connell effect. V0430 UMa |Other detected periods are 0.0037005d and 0.0024173d. V0441 UMa |VB A (B = V442 UMa, 2.0", 136{deg}, 2002). The range in the Table V0441 UMa |is for combined brightness. V0442 UMa |VB B (A = V441 UMa; AB 2.0", 136{deg}, 2002). O'Connell effect. V0448 UMa |P1 is presented in the Table. P0 = 0.481662d; P1/P0 = 0.7445. V0452 UMa |VB A (A 14.0mV; B 15.7mV, 18", 233{deg}, 2000). V0460 UMa |Distortion wave: P = 3.697d. V0462 UMa |P1 is presented in the Table. P0 = 0.484580d; P1/P0 = 0.7441. V0464 UMa |P1 is presented in the Table. P0 = 0.483830d; P1/P0 = 0.7450. V0465 UMa |The mean brightness varies. V0470 UMa |P1 is presented in the Table. P0 = 0.516157d; P1/P0 = 0.7464. V0471 UMa |P1 is presented in the Table. P0 = 0.548171d; P1/P0 = 0.7455. V0473 UMa |P1 is presented in the Table. P0 = 0.497336d; P1/P0 = 0.7456. V0474 UMa |Double-mode pulsations. The other period is 0.0496142d. V0475 UMa |P1 is presented in the Table. P0 = 0.557528d; P1/P0 = 0.7462. V0475 UMa |Additional non-radial mode, P = 0.433241d. V0477 UMa |P1 is presented in the Table. P0 = 0.474709d; P1/P0 = 0.7440. V0479 UMa |P1 is presented in the Table. P0 = 0.524939d; P1/P0 = 0.7463. V0486 UMa |Type EW with a twice longer period is also possible. V0497 UMa |Double-mode pulsations. For the P0 period, see the Table. P1 = V0497 UMa |0.0526002d; P1/P0 = 0.77418. V0498 UMa |Period varies? eps UMa |SB (P=4.15A). Interferometric binary? (0.053", 94.5{deg}, 1975.4). eps UMa |In 1976 - 1983 attempts to resolve the binary interferometrically eps UMa |were not successful. In the UMa moving cluster. ups UMa |ADS 7534 A (B 11.5m, 11.3", 295{deg}, common {mu}). The light curve ups UMa |shape and A var. R UMi |H2O maser. S UMi |P var. Max = 2422604 + 321.9d*E (JD2413000 - 23000); Max = 2432200 S UMi |+ 331.5d*E (JD2423000 - 32800); Max = 2436080 + 322.5d*E (JD2433000 S UMi |- 37000); Max = 2439011 + 326.5d*E (JD2437000 - 41500); since S UMi |JD2441500 - see Table. T UMi |P var. Max = 2428332 + 315.48d*E (JD2416500 - 29500); Max = 2436415 T UMi |+ 310.05d*E (JD2429500 - 37200); Max = 2442389 + 315.5d*E T UMi |(JD2437200 - 43600); since JD2443600 - see Table. U UMi |P var. Max = 2416975 + 323.1d*E (JD2416500 - 21000); Max = 2428804 U UMi |+ 331.3d*E (JD2421000 - 29780) [00001]; Max = 2429789 + 320.6d*E U UMi |(JD2429780 - 34600) [00960]; Max = 2434600 + 331d*E (JD2434600 - U UMi |36300); Max = 2437853 + 322.6d*E (JD2436300 - 39000); since U UMi |JD2439000 - see Table. V UMi |Mean brightness var with P2 = 760d. W UMi |Min II 8.66; d = 0.02P. P var? Non-linear term in the elements is W UMi |possible: -7.7d*10**(-10)*E**2. X UMi |P var? Max = 2424224 + 343d*E (JD2423800 - 25100) [00684]; since X UMi |JD2438100 - see Table. RR UMi |SB (Porb = 749.4d [09896]). RT UMi |Min II 10.86. RU UMi |Min II 10.20. RZ UMi |Min II 13.5. SZ UMi |Variability needs confirmation. VV UMi |MinII - MinI = 0.52P:. VZ UMi |Min II = 13.5. WW UMi |Min II = 12.55. WX UMi |Min II = 15.1. WY UMi |The ultraviolet-light amplitude is at least 1.6m. WZ UMi |Min II = 13.1. AA UMi |Min II = 12.68:. AK UMi |Type ELL with a twice longer period is not excluded. AN UMi |VB A (14.4mV; B 15.8mV, 8", 63{deg}, 2000). The variability range AN UMi |in the Table is for combined light. BD UMi |MinII - MinI = 0.544P. BE UMi |d = 0.05P. The mean brightness outside eclipses strongly varies. BE UMi |Quasi-periodic variations outside eclipses with P1 = 0.0402525d, P2 BE UMi |= 0.0352080d and four other periods. alf UMi |VB A (B 8.20m, F3V, 18.3", 218{deg}); SB1 (Porb = 10969d, E = 0.655 alf UMi |[09904]). P var. There is a non-linear term in the elements: alf UMi |+1.9877d*10**(-7)*E**2. The amplitude of light and radial velocity alf UMi |variation decreased in 1982. A(V) = 0.04m (1984). gam UMi |P var. Max = 2424301.78 + 0.14335d*E [10097]; Max = 2427904.468 + gam UMi |0.14335d*E [10098]. Elements given in the Table represent gam UMi |observations in 1964 - 1968. According to [09906] Vr var in 1922 gam UMi |with P = 0.108449d. eps UMi |VB A (B 12.5m, 76.9", 3{deg}). Min II 4.21. S Vel |Min II 7.83; d = 0.041P. P var? There is a non-linear term in the S Vel |elements given in the Table: +4.47d*10**(-9)*E**2. W Vel |P var. Max = 2415053 + 384.3d*E (JD2414600 - 17400); Max = 2426080 W Vel |+ 399.9d*E (JD2422400 - 27300); Max = 2429990 + 388.0d*E (JD2427300 W Vel |- 30100); Max = 2438328 + 398.7d*E (JD2430100 - 38800); since W Vel |JD2438800 - see Table. OH emission. Y Vel |P var. Max = 2415900 + 438.6d*E (JD2411500 - 15900); Max = 2419930 Y Vel |+ 447.7d*E (JD2415900 - 19930); Max = 2425755 + 452.8d*E (JD2421600 Y Vel |- 27600); Max = 2434150 + 439.5d*E (JD2427600 - 34200); since Y Vel |JD2434200 - see Table. Z Vel |P var. Max = 2415445 + 435.96d*E (JD2415000 - 25100); Max = 2425462 Z Vel |+ 417.99d*E (JD2425100 - 29700) [00960]; since JD2429200 - see Z Vel |Table. RR Vel |Min II 10.9. RS Vel |P var. Max = 2410403 + 421d*E (JD2410400 - 16800) [09961]; since RS Vel |JD2415450 - see Table. RU Vel |VB A (B 12m sf). According to [00017], Max = 2414390 + 63d*E. RW Vel |P var. Max = 2413553 + 430.4d*E (JD2413500 - 18500); Max = 2420610 RW Vel |+ 465.7d*E (JD2418500 - 25700); since JD2425700 - see Table. RX Vel |Min II 10.5. RY Vel |[A/H] = -0.3. P var. Max = 2440246.67 + 28.1270d*E (JD2419000 - RY Vel |40250) [05366]; since JD2443900 - see Table. SW Vel |P var. Max = 2434872.95 + 23.473d*E - 3.75d*10**(-5)*E**2 SW Vel |(JD2412500 - 35500) [09636]. Since JD2440700 - see Table. SX Vel |The light curve has double maximum. The epoch of the primary SX Vel |(second) maximum is given in the Table. TT Vel |Min II 10.7. UW Vel |In the region of the open cluster NGC 3033. YZ Vel |Min II 12.8; DII = 0.040P; Min II - Min I = 0.537P. ZZ Vel |Min II 10.0. AA Vel |Min II 9.9. AC Vel |Min II 9.11. AF Vel |(k - b)2 = 0.06. Blazhko effect is possible [10110]. AH Vel |SB? [10111]. In the region of the open cluster Collinder 173. AI Vel |Mu = 0.11", P = 76{deg}; (k - b)2 = 0.23. Light oscillations with AI Vel |the period P0 given in the Table are superimposed by oscillations AI Vel |with P1 = 0.08620868d and twice smaller amplitude. According to AI Vel |[10112] P0 is constant, P1 is increasing. AK Vel |In the region of the open cluster Collinder 173. AL Vel |d = 0.072P. AO Vel |In the region of the open cluster Collinder 173. Min II 9.55:. AO Vel |There is apsidal line motion. There is a sinusoidal term in the AO Vel |elements given in the Table: +0.058d*sin({phi}), where {phi} = AO Vel |2{pi}(E - 5338)/11500, and E values are counted from JD2415810.66. AO Vel |Min II = 2424270.125 + 1.5845993d (E - 5338) - -0.058d*sin({phi}); AO Vel |Min II - Min I = 0.792d - 0.116d*sin({phi}). AP Vel |P1 = 2.19984d; P1/P0 = 0.703. M - m var (0.25P <= M - m <= <= AP Vel |0.50P) [03710]. AQ Vel |d = 0.05P. The depth of Min II 0.05m. AS Vel |Min II 8.4; Min II - Min I = 0.55P. AT Vel |d = 0.03P. In the region of the open cluster Collinder 173. AU Vel |In the region of the open cluster Collinder 173. AV Vel |In the region of the open cluster Collinder 173. AW Vel |In the region of the open cluster Collinder 173. AX Vel |The first overtone mode light variation elements with the period P1 AX Vel |are given in the Table; the amplitude of the first overtone mode AX Vel |light variation A1 exceeds that of the fundamental mode, A0:A1(V) = AX Vel |1.5A0(V). For the fundamental mode P0 Max hel = 2443878.885 + AX Vel |3.673174d*E. P1/P0 = 0.706; M - m var: 0.24P <= M - m <= 0.50P:. AY Vel |Min II 9.7. AZ Vel |Min II 13.0. In the region of the open cluster Collinder 173. BB Vel |P < 20d. In the region of the open cluster Collinder 173. BC Vel |Min II 12.3. BD Vel |d = 0.04P. BE Vel |Min II 12.5. BF Vel |The depth of Min II 0.04m. BM Vel |Min II 13.0. In the region of the open cluster NGC 2547. In the BM Vel |region of the open cluster Collinder 173. BO Vel |Min II 14.2. BP Vel |Min II 13.7. BR Vel |The shape of the light curve varies. BT Vel |Min II 14.8. BU Vel |Min II 10.96; Min II - Min I = 0.522P. In the region of the open BU Vel |cluster Collinder 173. BV Vel |In the region of the open cluster Collinder 173. BW Vel |Min II 14.3. BX Vel |In the region of the open cluster Tr 10. BZ Vel |Min II 10.4; Min II - Min I = 0.57P. CK Vel |D ~0.3d. CL Vel |Min II 13.4. CR Vel |d = 0.05P. CS Vel |[A/H] = 0.1. Possible member of the open cluster Ruprecht 79. CU Vel |The period of superhumps ~0.08d, A = 0.4m [10115]. CV Vel |Min II 7.17. CW Vel |d = 0.024P. The depth of Min II 0.1m pg. CZ Vel |Min II 11.1. DF Vel |Min II 13.4. DH Vel |Min II 13.7. DK Vel |VB A (B 12.50m, 22", 315{deg}; C 16m, 10", 60{deg}). DL Vel |Min II 12.1. DM Vel |P = 123d? DQ Vel |Min II 11.0. DS Vel |Min II 10.8. DT Vel |(k - b)2 = 0.24. DX Vel |Min II 10.3. In the region of the open cluster Col 213. EH Vel |Min II 13.4. EL Vel |In the region of the open cluster Collinder 173. EO Vel |Min II 11.90, DII = 0.07P. Apsidal motion: Min II - Min I = 3.15d + EO Vel |0.00003d*E. Min II = 2441716.75 + 5.32969d*E. EP Vel |In the region of the open cluster IC 2395. ES Vel |Min II 12.7. ET Vel |Min II 12.1. EU Vel |Min II 13.8. EY Vel |d = 0.04P:. FM Vel |Min II 12.9. FS Vel |{Delta}(S) = 10. FT Vel |Min II 10.5. FW Vel |Min II 10.0. FX Vel |Min II 10.5. The shape of the light curve varies. FY Vel |Min II 7.03. Type ELL? [06827]. FZ Vel |VB A (B 12.08m, 24.2", 338{deg}). GG Vel |VB A (B 11.2m, 6", {delta}({alpha}) = 0). P = 2.950432d? GP Vel |Min II 6.90. Min II - Min I = 0.55P. The shape of the light curve GP Vel |varies. There are probably long-period light oscillations: Min = GP Vel |2442681.6 + 93.3d*E (A ~0.02m) [10051]. The period of X-ray pulses GP Vel |var: 282.8913s (1975.5) [10125]; 282.919s (1975.7) [10126]; GP Vel |282.869s (1976.4), 282.838s (1976.9) [10127]; 282.80s (1978.9) GP Vel |[10128]; 282.745s (1979.3), 282.7874s (1980.3), 282.87s (1981.0) GP Vel |[10129]; 282.93s (1981.9 - 1982.9); 282.9306s (1983.2) [10078]. GV Vel |In the region of the open cluster NGC 2660. HU Vel |Pulsar PSR 0833-45. In the nebula Vela SNR. Star M [08276]. The HU Vel |pulsed radiation varies in radio, optical and {gamma} rays with P = HU Vel |0.089s. P var [10136- 10139]: P = 0.089233318274s (JD2442553 - HU Vel |680), P = 0.089234713929s (JD2442700 - 848), P = 0.089244007685s HU Vel |(JD2443654 - 676), P = 0.089245406487s (JD2443719 - 850) [10137]; P HU Vel |= 0.089256985348s (JD2444795.84) [10138]. HV Vel |A member of the open cluster IC 2391. HW Vel |P = 0.26133d? A member of the open cluster IC 2391. HX Vel |VB A (B 7.1m, 0.3", 313{deg}, 1949); in the region of the open HX Vel |cluster IC 2395. Min II 5.50:. HY Vel |VB A (B 5.7m, 76.6"); a member of the open cluster IC 2391. Min II HY Vel |4.90. IL Vel |A var (0.02m <= A <= 0.15m). Beat period 10.075d (Min A = 2443175.5 IL Vel |+ 10.075d*E). IM Vel |VB A (B 9.73m, 3.3", 179{deg}, 1948). The double wave of light IM Vel |variations with rotation period Prot = 2.85204d and A = 0.03m is IM Vel |superimposed by oscillations with the periods P1 = 0.00812815d (A1 IM Vel |= 0.0043m), P2 = 0.00808206d (A2 = 0.0035m), P3 = 0.00810503d (A3 = IM Vel |0.0008m), P4 = 0.004052519d (A4 = 0.0009m), P5 = 0.004064065d (A5 = IM Vel |0.0004m), P6 = 0.004041031d (A6 = 0.0004m), P7 = 0.00815128d (A7 = IM Vel |0.0004m) [09208]. IN Vel |P = 65 - 70d, IP Vel |VB A (B 11.2m V, 2.1", 200{deg}, 1929). P > 1.25d. IQ Vel |Min II 12.94; Min II - Min I = 0.500P. IS Vel |A(U) var: 0.005m <= A(U) <= 0.018m. IT Vel |Min II 7.08. P = 23.52d? OQ Vel |The type is doubtful. V0360 Vel |Several close companions. V0390 Vel |P = 89.9 d is also possible. SB, Porb = 499 d. V0405 Vel |A twice shorter period is not excluded. VB (9", 346{deg}, 1976). V0409 Vel |MinII - MinI = 0.28P. V0420 Vel |Not CoD-45 05845 (identification suggested in [79235]). V0447 Vel |Min II = 11.91. V0448 Vel |Min II = 11.96. P varies. dP/dt = -0.44 x 10^(-5) d/yr. V0451 Vel |Min II = 7.49. V0452 Vel |Min II = 11.01. V0454 Vel |Min II = 7.65. V0456 Vel |The depth of MinII is 0.45 mag. V0457 Vel |Multiperiodic. V0458 Vel |Multiperiodic. V0459 Vel |Multiperiodic. V0460 Vel |Blended. Multiperiodic. V0461 Vel |After subtraction of the BE trends, EA variations 8.33m - 8.45m, V0461 Vel |MinII 8.44. V0464 Vel |The depth of MinII is 0.30 mag. V0465 Vel |Min II = 14.32. V0467 Vel |Min II = 11.00:. The tabulated ephemeris is for eclipses. V0467 Vel |Pulsations: P = 0.432728d, amplitude 0.05m. V0469 Vel |Min II = 9.51. V0472 Vel |An atypical emission-line star with periodic brightness variations. V0479 Vel |Min II = 9.22. V0483 Vel |Min II = 8.25. VB AB (8.79m, 9.19m, 1.0", 53{deg}, 1991). V0484 Vel |Min II = 9.91. V0487 Vel |Cycles about 280d in maximum light with an amplitude up to 1m. V0495 Vel |Min II = 10.47. V0496 Vel |Min II = 9.21. V0497 Vel |Min II = 9.63. VB AB (10.1m, 10.4m, 0.2", 150{deg}, 1991). V0503 Vel |Min II = 8.98. VB AB (9.2m, 11.2m, 0.6", 107{deg}, 1945). V0504 Vel |Min II = 18.20. Cluster non-member. V0505 Vel |Min II = 18.54. Cluster non-member. V0506 Vel |Min II = 17.60. Cluster non-member. V0507 Vel |Min II = 17.21. Cluster non-member. V0508 Vel |Min II = 17.89. Cluster non-member. V0509 Vel |Min II = 20.33. Cluster non-member. V0510 Vel |Cluster non-member. V0511 Vel |Min II = 20.00. Cluster non-member. V0512 Vel |Min II = 17.84. Cluster non-member. V0513 Vel |Min II = 19.29. Cluster non-member. V0514 Vel |Cluster non-member. V0516 Vel |A twice longer period is also possible. VB A (B 12.0m, 2", 29{deg}, V0516 Vel |1945). V0518 Vel |Min II = 12.14. V0519 Vel |Pulsates in the first (see Table) and second (Max = 2453426.48 + V0519 Vel |0.939354d x E) overtone modes. P2/P1 = 0.8052. V0526 Vel |Double-mode pulsation. For the fundamental-mode period, see the V0526 Vel |Table. P1 = 0.0624889d, P1/P0 = 0.8062. V0528 Vel |Multiperiodic, 4 harmonics. V0533 Vel |SB2. V0540 Vel |Double-mode pulsation. P2 = 0.1765777d. V0547 Vel |SB2. V0548 Vel |Multiperiodic. P2 = 0.0482189d. V0551 Vel |Multiperiodic. gam 2 Vel |VB A (B 4.22m, 41.3", 220{deg}). SB2 (Porb = 78.5002d [10119]). In gam 2 Vel |HII region. T0 = 2433633.0 is the epoch of the conjunction where gam 2 Vel |the O component is in front [10119]. lam Vel |VB A (B 14.8m, 18.2", 137{deg}). omi Vel |A member of the open cluster IC 2391. P(VR) = 2.74d. P = 2.76d? omi Vel |SB1? The epoch of the light maximum is given. Close binary system? R Vir |P var. Max = 2381914 + 145.77d*E (JD2338900 - 2402000); Max = R Vir |2402321 + 144.90d*E (JD2402000 - 18000); Max = 2418268 + 145.48d*E R Vir |(JD2418000 - 30000); Max = 2430489 + 148.32d*E (JD2430000 - 34000); R Vir |Max = 2434193 + 144.63d*E (JD2434000 - 38500); Max = 2438829 + R Vir |147.45d*E (JD2438500 - 43000); since JD2443000 see Table. Maser R Vir |(SiO). S Vir |P var. Max = 2399014 + 374.7d*E (JD2398600 - 2405000); Max = S Vir |2412970 + 376.2d*E (JD2412000 - 23500, on average); Max = 2423502 + S Vir |381.52d*E (JD2423500 - 23000); since JD2433000 - see Table. Maser S Vir |(H2O, SiO). T Vir |Maser (OH, H2O, SiO). V Vir |P var. Before JD2427000 Max = 2400467 + 250.17d*E; Max = 2427225 + V Vir |246.54d*E (JD2427000 - 31500); since JD2431500 - see Table. W Vir |The epoch of Min is given. P var. Min = 2404151.168 + 17.2707d*E W Vir |(JD2403000 - 23200); Min = 2423200.837 + 17.2634d*E (JD2423200 - W Vir |29700); since JD2429700 - see Table. The light curve shape var. W Vir |[Fe/H] = -1.03. X Vir |VB A (B 12m, dK4, 0.6', ~50{deg}). The brightenings of 1871 and X Vir |1882 may be due to misidentification [01651]. Z Vir |P var. Max = 2409683 + 309.19d*E (JD2408000 - 18500); since Z Vir |JD2418500 - see Table. RS Vir |Maser (OH, H2O, SiO). P var. Max =2412592 + 351.29d*E (JD2412000 - RS Vir |31000); since JD2431000 - see Table. RT Vir |Maser (OH, H2O, SiO). According to [10145], observations of RT Vir |1970-1977 are not in agreement with the P value in the Table. RU Vir |P var? Max = 2425120 + 435.9d*E (JD2414000 - 31500); since RU Vir |JD2431500 - see Table. RV Vir |P var. Max = 2412272 + 268.39d*E (JD2412000 - 31500); since RV Vir |JD2431500 - see Table. RX Vir |VB (B 13.0m vis, 1.1", 107{deg}, 1939). According to photoelectric RX Vir |observations [06450,08837], 8.72m - 8.81m V. Const? [06450]. SS Vir |P var. Max = 2415910 + 352.75d*E (JD2415900 - 21500); Max = 2421913 SS Vir |+ 361.7d*E (JD2421500 - 26500); Max = 2428359 + 350.12d*E SS Vir |(JD2426500 - 40000); since JD2440000 - see Table. ST Vir |P var. Max = 2425005533 + 0.4108494d*E (JD2422000 - 29100) [10146]; ST Vir |Max = 2436702.513 + 0.4108168d*E (JD2433000 - 39000) [03415]; since ST Vir |JD2439000 - see Table. Blazhko effect? {Delta}(S) = 0.8. SU Vir |P var. Max = 2415040 + 213.7d*E (JD2415000 - 19500); Max = 2419926 SU Vir |+ 210.96d*E (JD2415000 - 31500); Max = 2437378 + 210.2d*E SU Vir |(JD2431500 - 38500); since JD2438500 - see Table. SV Vir |P var? The mean elements are given. Maser (H2O). SZ Vir |Possibly EW with a very small A. TV Vir |VB A (B P). TW Vir |Porb = 0.182666d [09430]. Variability of ellipsoidal character in H TW Vir |light: P = Porb/2, A(H) = 0.13m. X-ray source. TX Vir |VB A (B 15m, 0.3' P). TY Vir |[Fe/H] = -1.7. TZ Vir |P2 = 6900d is superimposed? UU Vir |[Fe/H] = -0.3. {delta}[S] = 0.7. UW Vir |d = 0.011P. P var. Min = 2419942.513 + 1.8106818d*E (JD2415000 - UW Vir |34500); since JD2441000 - see Table UY Vir |d = 0.014P; Min II 8.1. VV Vir |Min II 12.2:. VW Vir |SN 1895 (NGC 4424). XX Vir |[Fe/H] = -1.5. {Delta}(S) = 9:. YZ Vir |[A/H] = -0.9. AD Vir |P var. Max = 2425259.259 + 0.5522109d*E (JD2419000 - 31000); since AD Vir |JD2431000 - see Table. AF Vir |P var. Max = 2429051.697 + 0.4838214d*E (JD2419500 - 36000); Max = AF Vir |2436718.3758 + 0.4838386d*E (JD2436000 - 37500) [10159]; since AF Vir |JD2440000 - see Table. DM var. AG Vir |The depth of Min II up to 0.44m. The light curve shape and A var. AG Vir |dI = 0.03P:, dII = 0.66P. Min II - Min I = 0.512P. P var. Min = AG Vir |2434487.4297 + 0.6426489d*E (JD2424500 - 34500); since JD2434500 - AG Vir |see Table. AH Vir |ADS 8472 A (B 13.2m, 1.3", 17{deg}). The combined brightness is AH Vir |given, dI = 0.07P. The depth of Min II 0.53m, dII = 0.00P. The AH Vir |light curve shape var. P var. Min = 2434841.3963 + 0.40751843d*E AH Vir |(JD2425000 - 35000) [05222]; Min = 2435573.710 + 0.40752192d*E AH Vir |(JD2435000 - 41400); Min = 2441411.460 + 0.40753186d*E (JD2441400 - AH Vir |44000); since JD2444000 - see Table. AK Vir |VB B (A = BD -17{deg} 3996; B 44", 286{deg}). AL Vir |P var [A/H] = -0.7. AN Vir |P2 ~1000d is superimposed. AO Vir |VB A (B 11.4m vis, 6.9", 321{deg}, 1956, common Vr). {delta}(M) is AO Vir |possibly in error because of the companion. P var. Max = 2413949 + AO Vir |256.88d*E (JD2412900 - 21000); since JD2421000 - see Table. AS Vir |P var. The Table gives the mean elements valid after JD2425600. AS Vir |Blazhko effect? [03506]. (k - b)2 = 0.08. AT Vir |P var. Max = 2426831.367 + 0.5258053d*E (JD2420500 - 35000) AT Vir |[00188]; since JD2435000 - see Table. (k - b)2 = 0.00, {Delta}(S) = AT Vir |6.0. AU Vir |[Fe/H] = -1.84, {Delta}(S) = 10.1. AV Vir |{Delta}(S) = 5.5. AW Vir |Min II 11.67. AX Vir |Min II 10.24. AY Vir |Maser (H2O). AZ Vir |Min II 11.37. BB Vir |Blazhko effect? BC Vir |P var. Max = 2419922.289 + 0.56451468d*E (JD2419900 - 30100); the BC Vir |Table gives current elements. BD Vir |P var. Min = 2424971.720 + 2.548410d*E (JD2424900 - 32000); since BD Vir |JD2432000 - see Table. BF Vir |Min II 10.72. Total eclipses. P var. Min = 2416595.67 + 0.64057d:*E BF Vir |(JD2414000 - 19000); Min = 2440331.809 + 0.64057631d*E (JD2426000 - BF Vir |41000); since JD2441000 - see Table. BH Vir |Min II 10.24. Distortion wave? ({Delta}(V) = 0.04m). BN Vir |P var. Max = 2419865.422 + 0.39127585d*E (JD2419800 - 28300); since BN Vir |JD2432600 - see Table. BO Vir |P var. Max = 2419513.388 + 0.52005916d*E (JD2419500 - 33000); since BO Vir |JD2433000 - see Table. BQ Vir |P var? BS Vir |[Fe/H] = -1.84. {Delta}(S) = 10.1. BV Vir |P var. Max = 2426070.488 + 0.4965803d*E (JD2419900 - 28500); since BV Vir |JD2436600 - see Table. BW Vir |P var. Max = 2420247.403 + 0.4706660d*E (JD2420200 - 26800); since BW Vir |JD2426800 - see Table. CG Vir |Min II 10.9. CK Vir |[Fe/H] = -2.0. CM Vir |d = 0.05P. P var. Min = 2425411.330 + 3.40167d*E (JD2423900 - CM Vir |28400) [00001]; during JD2432200 - 34200 - see Table. CS Vir |The epoch of Max in B light is given. SB (Porb = 1618d). IR excess CS Vir |(4.8 mkm). CU Vir |ADS 9152 A (B 11.9m, G1V, 60", 212{deg}). CW Vir |The epoch of min is given. CX Vir |The depth of Min II 0.30m. DK Vir |According to [10189], P1 = 0.1162d, P2 = 0.1086d. (k - b)2 = 0.20. DL Vir |SB (Porb = 2286d). The spectrum shows the A-component of the DL Vir |eclipsing system and the G8III star around which the eclipsing DL Vir |system is orbiting. DM Vir |Min II 9.49. DII = DI. DN Vir |P >= 100d. DT Vir |Mu {alpha} = -0.044s, {mu} {delta} = -0.02". SB? Rotation period DT Vir |1.535d [10014], A = 0.05m V. DV Vir |Blazhko effect? EF Vir |According to [04784], const?, 16.1m pg. EP Vir |IR excess (4.8 mkm). EQ Vir |SB; [Fe/H] = -0.08. Min = 2441129.585 + 3.914169D*E + EQ Vir |0.0001803345d*E**2, A = 0.10m V, M - m = 0.40P. Soft X-ray source, EQ Vir |lg FX/FV = -2.07. EW Vir |P >= 100d. EX Vir |P >= 100d. EY Vir |P >= 100d. FF Vir |The P value for magnetic field variations is given. FG Vir |ADS 8471 A (B 13.51m, 25", 352{deg}, 1909; C 11.85m, 74", 195{deg}, FG Vir |1909). FI Vir |Mu {alpha} = +0.043s, {mu} {delta} = -1.22". FL Vir |VB AB (A = 0.76", P = 16A). Both components show flares? The range FL Vir |of combined brightness is given. Mu {alpha} = -0.118s, {mu} {delta} FL Vir |= +0.26". FM Vir |SB2, Porb = 38.324d. FN Vir |Mu {alpha} = -0.064s, {mu} {delta} = +0.28". SB? X-ray source, FN Vir |LX/Lbol = -3.55. FO Vir |Min II 6.67. FQ Vir |Deep Min II. GG Vir |Multiperiodicity, 0.023d <= P <= 0.083d, A <= 0.02m. GH Vir |P var. GK Vir |The secondary is a red dwarf (M0 - M6). GL Vir |Mu {alpha} = -0.087s; {mu} {delta} = +0.23". GM Vir |P ~1.6d/n. GQ Vir |Mu {alpha} = -0.045s, {mu} {delta} = -0.44". GR Vir |The depth of Min II 0.41m. GU Vir |P var. Max = 2439236.36 + 0.466562d*E (JD2438100 - 39300); during GU Vir |JD2441300 - 42600 - see Table. LV Vir |Type RR: is also possible. MW Vir |Type DSCTC: is also possible. NN Vir |Type EW: is also possible. PS Vir |MinII 12.2. PT Vir |MinII 13.54. PU Vir |MinII 11.68. PY Vir |MinII 10.04. QU Vir |MinII 12.03. QX Vir |MinII 12.6. QZ Vir |SB1 (Porb = 0.05881873d [09304]). V0338 Vir |A twice longer or a twice shorter period is not excluded. V0354 Vir |Blazhko effect, P = 59d: [80026]. V0357 Vir |Blazhko effect? [80422]. V0378 Vir |P = 0.268012d is also possible. V0379 Vir |Porb = 0.061412d. V0385 Vir |P = 0.447390d is also possible. V0391 Vir |Min II = 13.6. V0406 Vir |Quasi-periodic variations with a cycle about 0.39d. Porb = V0406 Vir |0.05592d. V0414 Vir |P = 0.492859d is also possible. V0415 Vir |Min II = 10.32. V0419 Vir |Blazhko effect, P = 65.69d. V0439 Vir |Multiperiodic. V0461 Vir |P = 0.153332d is also possible. V0466 Vir |Blazhko effect, P = 62.9:d. V0467 Vir |Min II = 9.69. V0476 Vir |P varies? V0492 Vir |P = 0.407024d is also possible. V0503 Vir |Min II = 16.10. V0533 Vir |P = 0.186684d is also possible. V0546 Vir |Min II = 10.48. V0551 Vir |Blazhko effect, P = 48d. V0560 Vir |Blazhko effect. V0585 Vir |P varies. Before JD 2453700, Max = 2451961.85 + 0.60163d x E. V0589 Vir |Min II = 14.20. V0591 Vir |Min II = 12.38. V0593 Vir |P = 0.186389d is also possible. Associated with an X-ray source. V0594 Vir |Multiperiodic. V0613 Vir |P strongly varies. V0630 Vir |The Table presents the light elements for the first overtone. For V0630 Vir |the fundamental mode, Max = 2454800.650 + 0.524429d x E. P1/P0 = V0630 Vir |0.7453. V0644 Vir |Double-mode pulsations. The Table gives the first overtone light V0644 Vir |elements. For the fundamental mode, Max = 2454800.145 + 0.455977d x V0644 Vir |E. P1/P0 = 0.7426. V0659 Vir |Double-mode pulsations. The Table contains light elements for the V0659 Vir |first overtone. Fundamental mode: Max = 2454800.750 + 0.505828d x V0659 Vir |E. P1/P0 = 0.7450. V0674 Vir |P1 is presented in the Table. P0 = 0.485546d; P1/P0 = 0.7444. V0675 Vir |P0 is presented in the Table. P1 = 0.347029d; P1/P0 = 0.7415. V0679 Vir |P1 is presented in the Table. P0 = 0.481836d; P1/P0 = 0.7436. V0680 Vir |P1 is presented in the Table. P0 = 0.496630d; P1/P0 = 0.7451. V0681 Vir |P1 is presented in the Table. P0 = 0.494004d; P1/P0 = 0.7453. V0684 Vir |P1 is presented in the Table. P0 = 0.478307d; P1/P0 = 0.7433. V0685 Vir |P1 is presented in the Table. P0 = 0.495555d; P1/P0 = 0.7447. V0686 Vir |P1 is presented in the Table. P0 = 0.494463d; P1/P0 = 0.7445. V0691 Vir |P1 is presented in the Table. P0 = 0.539888d; P1/P0 = 0.7461. V0693 Vir |The data for 1SWASP J130711.90+084159.9 in [82030] are combined V0693 Vir |measurements for a non-variable star (V = 14.9m) near the SuperWASP V0693 Vir |position and the real variable. V0694 Vir |P1 is presented in the Table. P0 = 0.464667d; P1/P0 = 0.7430. V0696 Vir |P1 is presented in the Table. P0 = 0.469383d; P1/P0 = 0.7433. V0698 Vir |P1 is presented in the Table. P0 = 0.516959d; P1/P0 = 0.7452. V0699 Vir |P1 is presented in the Table. P0 = 0.559293d; P1/P0 = 0.7468. V0703 Vir |P1 is presented in the Table. P0 = 0.476683d; P1/P0 = 0.7441. V0704 Vir |P1 is presented in the Table. P0 = 0.476846d; P1/P0 = 0.7446. V0705 Vir |P1 is presented in the Table. P0 = 0.477771d; P1/P0 = 0.7438. V0707 Vir |P1 is presented in the Table. P0 = 0.486191d; P1/P0 = 0.7437. V0708 Vir |P1 is presented in the Table. P0 = 0.483093d; P1/P0 = 0.7438. V0711 Vir |P1 is presented in the Table. P0 = 0.545077d; P1/P0 = 0.7457. V0723 Vir |Additional non-radial mode, P = 0.2702020d; P(Blazhko) = 10.7d. V0730 Vir |Type EW with a twice longer period is also possible. V0734 Vir |P1 is presented in the Table. P0 = 0.462283d; P1/P0 = 0.7428. V0735 Vir |P1 is presented in the Table. P0 = 0.545647d; P1/P0 = 0.7468. V0737 Vir |P1 is presented in the Table. P0 = 0.485785d; P1/P0 = 0.7439. V0740 Vir |Period varies? V0742 Vir |P1 is presented in the Table. P0 = 0.552328d; P1/P0 = 0.7459. A V0742 Vir |close VB. alf Vir |The Table gives the epoch of Min for the ellipsoidal variability alf Vir |and Porb. The depth of Min II up to 0.08m. SB 2. e = 0.205 +- alf Vir |0.004. Apsidal motion: Pi = 108a +- 5a. Pulsations: P var, P = alf Vir |0.17378587d (1908 - 1956); since 1956 Max = 2445405.63 + alf Vir |0.17378680d*E [10181]. A var. 3 companions according to lunar alf Vir |occultation observations: 3.1m, 0.0025"; 4.5m, 0.05"; 7.5m, 0.5". alf Vir |Soft X-ray source, LX/Lbol = 2.9*10**(-8). psi Vir |Binary? (lunar occultations). R Vol |P var. Max = 2415238 + 441d*E (JD2394100 - 2418800) [10143]; since R Vol |JD2422700 - see Table. S Vol |P var. Max = 2415042 + 397.6d*E (JD2415000 - 24200), Max = 2428880 S Vol |+ 392.1d*E (JD2423000 - 28900), Max = 2434113 + 401.7d*E (JD2428900 S Vol |- 34900), Max = 2434910 + 387.2d*E (JD2434900 - 39200); since S Vol |JD2439200 - see Table. T Vol |P var. Max = 2413135 + 189.8d*E (JD2413100 - 14600); Max = 2416870 T Vol |+ 171.8d*E (JD2414600 - 16900); Max = 2416870 + 176.8d*E (JD2416800 T Vol |- 24400); Max = 2424460 + 170.8d*E (JD2424400 - 27200); Max = T Vol |2429925 + 182.3d*E (JD2427200 - 30000); since JD2440000 see Table. RX Vol |P < 20d? ST Vol |SP component of a very close pair. SV Vol |The shape of the light curve varies. TX Vol |Min II 10.5. P var. Min I = 2416789.869 + 5.38845d*E (JD2415100 - TX Vol |26000), Min I = 2431150.345 + 5.3887d*E (JD2426000 - 31400), Min I TX Vol |= 2433542.609 + 5.388d*E (JD2431400 - 33600) [00001]; since TX Vol |JD2433600 see Table. YZ Vol |A twice shorter period is not excluded. AD Vol |VB A (B 14.8mpg, 19", 260{deg}, 2000). AH Vol |Min II = 11.8. AL Vol |P0 is tabulated, P1 = 0.38521d. AO Vol |A close VB. R Vul |P var. Max = 2400169 + 138.3d*E (JD2400100 - 02700), Max = 2402779 R Vul |+ 136.76d*E (JD2402700 - 19800), Max = 2419880 + 137.45d*E R Vul |(JD2419800 - 24400), Max = 2424413 + 136.76d*E (JD2424400 - 28500 R Vul |[00960]; Max = 2429331 + 135.9d*E (JD2428500 - 32000) [00001]; R Vul |since JD2432000 see Table. S Vul |In the region of the open cluster C 1947 + 272 [10123]. P var. Max S Vul |= 2401772 + 67.37d*E (JD2401760 - 6400), Max = 2408180 + 67.70d*E S Vul |(JD2408170 - 14950), Max = 2415285 + 68.26d*E (JD2415300 - 22800), S Vul |Max = 2423468 + 67.72d*E (JD2423450 - 27200), Max = 2428227 + S Vul |68.18d*E (JD2428220 - 31300) [00761]; Max = 2432775 + 67.51d*E S Vul |(JD2431300 - 34500) [10148]; Max = 2437150 + 68.66d*E (JD2436800 - S Vul |39600), Max = 2441507 + 67.344d*E (JD2439600 - 43000) [10124]; S Vul |since JD2443000 see Table. [A/H] = 0.1. T Vul |P var. Max = 2419372.151 + 4.435589d*E (JD2409880 - 34000); since T Vul |JD2434000 see Table. V Vul |Min II 8.65. P var. Min I = 2414912.9 + 74.96d*E (JD2414900 - V Vul |20840), Min I = 2420909.8 + 75.686d*E (JD2420900 - 24810), Min I = V Vul |2425072.9 + 76.344d*E (JD2425050 - 30000), Min I = 2430023.5 + V Vul |75.957d*E (JD2430000 - 32500) [10149]. Study of period variation V Vul |and changes of Min II by Min I see also in [00767,010150]. W Vul |In the region of the open clusters NGC 6882, NGC 6885. X Vul |P var. Max = 2420636.337 + 6.319301d*E (JD2417000 - 34000) [00768]; X Vul |since JD2435000 - see Table. Z Vul |VB A (B 12.0m, 13", 359{deg}). Min II 7.58. P var. Min I = Z Vul |2425456.117 + 2.454926d*E (JD2413200 - 37000) [00063]; since Z Vul |JD2437000 - see Table. RS Vul |Min II 6.86; Min II - Min I = 0.508P. RU Vul |A var. P var. Max = 2416266 + 155.95d*E (JD2415000 - 36000), Max = RU Vul |2436779 + 150.7d*E (JD2436000 - 38800), Max = 2438855 + 153.4d*E RU Vul |(JD2438800 - 41620), Max = 2441193 + 138.5d*E (JD2441620 - 42600); RU Vul |since JD2442600 - see Table. RX Vul |P var. Max = 2420301 + 438d*E (JD2418900 - 22500) [04018]; since RX Vul |JD2424700 - see Table. RZ Vul |Slow variations of mean brightness with P = 1410D and A = 2m are RZ Vul |superimposed by fluctuations with the cycle 40 - 100d and A up to RZ Vul |1m. SU Vul |In the region of the open cluster NGC 6882, NGC 6885. SV Vul |[Fe/H] = 0.23. P var. There is a nonlinear term in the elements SV Vul |given in the Table: -0.0001814d*E**2. SX Vul |In the region of the open cluster NGC 6940. UU Vul |Published coordinates in [01622] are wrong. VV Vul |Min II 12.1; d = 0.026P. P var. Min I = 2416670.527 + 3.411224d*E VV Vul |(JD2416600 - 27500) [00134]; since JD2426000 - see Table. VW Vul |Porb = 0.0731d [10160]. VY Vul |Min II 14.4:. WW Vul |There is quasi-periodicity in light minima with the cycle 404d. XZ Vul |Min II 11.4. P var. Min I = 2426477.525 + 3.0895116d*E (JD2416900 - XZ Vul |36000) [04427]; since JD2436000 - see Table. AB Vul |The depth of Min II 0.02m. AD Vul |Min II 0.010P. AF Vul |Min = 2436545.23 + 0.954d*E (JD2436200 - 900) [03148]. AR Vul |In the region of the open cluster Stock 1. AT Vul |Min II 9.3; d = 0.02P. AW Vul |Min II 10.9; d = 0.020P. AX Vul |d = 0.018P. AY Vul |d = 0.020P. P var. Min hel = 2436128.388 + 2.4124239d*E (JD2418500 AY Vul |- 40700); since JD2440700 - see Table. AZ Vul |Min II 11.9. BB Vul |In the region of the open cluster NGC 6940. BE Vul |VB A (BC 11.92m, 50", 320{deg}). Min II 9.90. P var. Min I = BE Vul |2426144.490 + 1.55205d*E (JD2426140 - 28880), Min I = 2430698.203 + BE Vul |1.5520442d*E (JD2430690 - 34660), Min I = 2435340.373 + 1.552052d*E BE Vul |(JD2435340 - 40070); since JD2440100 - see Table. BF Vul |Elements given in the Table represent well only the bright maxima. BF Vul |The fainter maxima are represented by the elements: Max = 2427731 + BF Vul |95.4d*E. BI Vul |Min II 14.86. P var? Min I = 2424759.70 + 0.251828d*E [00193]; BI Vul |since JD2444750 - see Table. BN Vul |{Delta}(S) = 7. P var. Max = 2414815.759 + 0.5941295d*E (JD2414000 BN Vul |- 30000) [00388]; Max = 2434244.333 + 0.59412538d*E (JD2430000 - BN Vul |36000) [00616]; Max = 2438265.386 + 0.59412763d*E (JD2436000 - BN Vul |41000) [09009]; since JD2441000 - see Table. BO Vul |Min II 10.6. P var. Min I = 2429984.332 + 1.9459123d*E (JD2415000 - BO Vul |30000) [00007]; Min I = 2432379.766 + 1.9459206d*E (JD2427000 - BO Vul |35000), since JD2435300 - see Table. BP Vul |Min II 10.5. BS Vul |Min II 11.10. BT Vul |d = 0.03P; Min II 12.3. BU Vul |P var. Min = 2431006.204 + 0.5689904d*E (JD2426500 - 31100) BU Vul |[00001]; since JD2433500 - see Table. BV Vul |S 6.5/6-. BW Vul |P var. Max = 2424000.171 + 0.20102229d*E (JD2424000 - 26500), Max = BW Vul |2426500.079 + + 0.20102933d*E (JD2426500 - 31500), Max = = BW Vul |2432000.054 + 0.20103513d*E (JD2431500 - 41000); since JD2441000 - BW Vul |see Table. CD Vul |Min II 11.9. CK Vul |Max 2331186:. Connected with nebulae. Type NR? CS Vul |Min II 13.6. DR Vul |Min II 9.19; DII = 0.132P. There is apsidal motion with the period DR Vul |37.8 years. Elements given in the Table contain supplementary DR Vul |terms: -0.07165d*sin(0.05863{deg}*E) - 0.00269d* DR Vul |*sin(0.11726{deg}*E). Min II = 2440301.7934 + 2.2508645d*E + DR Vul |0.07165d* *sin(0.05863{deg}*E) - 0.00269d*sin(0.11726{deg}*E). P DR Vul |var? [10185]. The depth of minima varies. DY Vul |VB A (B 13.0m V, 14", 300{deg}). EH Vul |P var. Max = 2429609 + 185d*E (JD2429600 - 30600); since JD2430800 EH Vul |- see Table. EP Vul |S 6.5/5. EQ Vul |Min II 12.5; Min II - Min I = 0.31P; DII = 0.050P, dII = 0.010P. ER Vul |P var. Min I = 2440182.2593 + 0.69809510d*E (JD2433100 - 40200) ER Vul |[08592]; since JD2440100 - see Table. 7.35m <= Min II <= 7.44m. The ER Vul |shape of the light curve and depths of minima vary. ES Vul |VB A (B 10.1m, 1.6", 126{deg}). ET Vul |[A/H] = -0.4. P var. Max = 2425110.63 + 54.33d*E (JD2422900 - ET Vul |26600), Max = 2432875.80 + 54.33132d*E (JD2432700 - 35430), Max = ET Vul |2438656.99 + 53.81d*E (JD2436050 - 39035), Max = 2439253.55 + ET Vul |54.24d*E (JD2439035 - 40990) [10168]; since JD2441900 - see Table. EU Vul |Min II 13.3. EV Vul |Min II 11.9. P var. Min I = 2428750.459 + 2.822084d*E (JD2428400 - EV Vul |36400) [04027]; Min I = 2436748.37 + 2.82220d*E (JD2436380 - 750) EV Vul |[03732]; since JD2441500 - see Table. EX Vul |d = 0.03P. EY Vul |The depth of Min II 0.05m. FG Vul |In the region of the open cluster NGC 6940. Star 120. The epoch of FG Vul |light minimum is given. FH Vul |P var. The elements given in the Table are valid since JD2436000. FK Vul |Blazhko effect. FM Vul |Min II 13.0. FN Vul |d = 0.02P; Min II 14.2. FP Vul |Min II 15.6. FQ Vul |Min II 12.9. Apsidal motion with P = 280 years. Correction of FQ Vul |mispints in [04248] see in [04244]. FR Vul |Probably the period must be doubled. FS Vul |Min II 15.2. FU Vul |sp component of a close pair. FW Vul |Min II 12.9. FY Vul |sp component of a close pair. Cycle 30 - 70d [04027]. FZ Vul |Min II 13.9. GG Vul |P var. Max = 2427681.0 + 106.5d*E (JD2427500 - 28850); since GG Vul |JD2428850 - see Table. GH Vul |P = 2.5d? GI Vul |Min II 13.8. GK Vul |Red. GN Vul |Min II 12.4; d = 0.04P. GO Vul |Min II - Min I = 0.515P. The depth of Min II 0.03m. GP Vul |Min II 11.2; Min II - Min I = 0.48P. GQ Vul |nf component of a close triple group of stars. P var. Max = GQ Vul |2434399.825 + 12.647241d*E (JD2426100 - 38000) [04414]; since GQ Vul |JD2444600 - see Table. GR Vul |Min II 13.3. The chart in [04244] is wrong. GT Vul |Min II 15.8. GU Vul |Min II 12.2. GV Vul |Probably the period must be doubled. Probably the period must be GV Vul |doubled. HI Vul |Min II 12.6. HP Vul |The depth of Min II 0.04m. HS Vul |Min II 14.2. HU Vul |Blazhko effect? HV Vul |P var. Max = 2437165.449 + 0.419906d*E (JD2437100 - 38670); since HV Vul |JD2438670 - see Table. Blazhko effect? HW Vul |P var. Max = 2429077.0 + 75.44d*E (JD2427190 - 29080), Max = HW Vul |2429077.0 + 73.94d*E (JD2429070 - 32470); since JD2432350 - see HW Vul |Table. IU Vul |P var. Max = 2434656 + 320.2d*E (JD2432700 - 37860) [04427]; since IU Vul |JD2437860 - see Table. IW Vul |Min II 13.1. KN Vul |Min II 13.4. KO Vul |Red. KS Vul |Very red. LT Vul |Multiperiodicity: P1 = 0.109414d, A1(V) = 0.0234m; P2 = 0.11094d, LT Vul |A2(V) = 0.0074m; P3 = 0.1215d, A3(V) = 0.0070m (JD2444054 - 096) LT Vul |[10173]; P1 = 0.109621d, A1(B) = 0.0340m; P2 = 0.093528d, A2(B) = LT Vul |0.0136m (JD2444071 - 465) [10193]. LU Vul |Nova Vul 1968 N2. LV Vul |Nova Vul 1968 N1. VB A (B 18m, 6", 115{deg}). LW Vul |Min II 16.3. MN Vul |Min II 16.1; Min II - Min I = 0.518P; DII = 0.10P. MO Vul |Min II 14.8. P var? MR Vul |P2 = 111.0d? MT Vul |Multiperiodicity: P2 = 119.93d (A2 = 0.3m), P3 = 25.02d (A3 = MT Vul |0.4m:). MX Vul |P = 181.8d? NO Vul |Min II 14.1. NS Vul |VB A (B 8.8m, A0, 0.73", 273{deg}, 1978.6), The range of combined NS Vul |light variation is given. PS Vul |VB A (B 10.0m, 0.4", 105{deg}, 1980.0); SB2. PT Vul |P1 = 256.12714s (A1 = 1.14%), Max1 = 2445166.660914 HJED; P2 = PT Vul |256.33205s (A2 = 1.09%), Max2 = 2445166.659424 HJED; P3 = PT Vul |128.11496s (A3 = 0.37%), Max3 = 2445166.660024 HJED. {mu} = PT Vul |0.1508", P=1.6{deg}. PU Vul |Pre-outburst SP M4 (1958). Gradual light increase in 1977 - 79 up PU Vul |to 8.7m V; in 1979 A = 0.29M V, Min I = 2443943.39 + 78.12d*E PU Vul |[10197]. In the max of 1979 Sp F5Ia - F8-9I. In February 1980 an PU Vul |abrupt light decrease started; the star reached V = 13.65m by early PU Vul |September. By September, 1981 the star recovered from the deep Min PU Vul |of 500d duration. During the 1980 - 81 minimum Sp M5 with TiO PU Vul |bands, emissions of H{alpha}, NaD, [OII], FeII, rare earths. In PU Vul |1982 - 84 8.35m - 8.87m V, Sp became F again. Simetimes H{alpha}, PU Vul |H{beta} emissions have been detected, often with P Cyg profiles. V0398 Vul |Not identical to IRC+30416 = NSV 12861. V0469 Vul |Red, despite Sp B in the literature. V0477 Vul |Multiperiodic, P2 = 0.0644149d. V0479 Vul |Multiperiodic, P2 = 0.10114d. V0491 Vul |MinII - MinI = 0.327P. VB AB (10.9m, 11.1m, 0.6", 223{deg}, 2010). V0495 Vul |MinII - MinI = 0.544P. V0498 Vul |Superhumps: P = 0.05990d. A possible cycle between outburtsts is V0498 Vul |about 1000d. V0507 Vul |Period varies. Light elements for JD 2454200-2455150 are tabulated. V0507 Vul |For JD 2452750-2453950, Max = JD 2453169.815 + 0.336042 x E. V0523 Vul |O'Connell effect. Unusually red for the EW type. VB B (A 14.6m; AB V0523 Vul |4", 43{deg}, 1991). V0524 Vul |P = 0.685447d and type EW are also possible. V0528 Vul |P = 0.471026d is also possible. V0532 Vul |VB A (B 8", 94{deg}, 2000; C 5", 247{deg}, 2000). V0533 Vul |P = 0.267441d is also possible. V0536 Vul |P = 0.269786d is also possible. V0539 Vul |P = 0.3098d is also possible. V0540 Vul |Other possible periods: 0.418246d or 0.294669d. V0543 Vul |P = 0.274336d is also possible. V0544 Vul |P = 1.60142d is also possible. V0554 Vul |VB A (12.1mG; B 14.2mG, 11", 173{deg}, 2000). V0566 Vul |VB A (13.5mG; B 15.8mG, 8", 126{deg}, 2000); the range in the Table V0566 Vul |is influenced by the companion. V0571 Vul |Projected on the planetary nebula M27 = NGC 6853. V0572 Vul |VB A (B 10.96mV, 34", 3{deg}, 2015). V0575 Vul |VB A (13.8mG; B 14.5mG, 2.7", 64{deg}, 2000). The variability range V0575 Vul |in the Table is for combined light. --------------------------------------------------------------------------------