Asteroid Lightcurve Parameters                                 
                                                                                
                                                                                
C.-I. Lagerkvist             A.W. Harris          V. Zappala                    
Astronomiska Observatoriet   JPL 183-501          Oss. Astron. di Torino        
Box 515                      4800 Oak Grove Dr.   10025 Pino Torinese           
S-751 20 Uppsala             Pasadena, CA 91109   Italy                         
Sweden                       USA                                                
                                                                                
     The lightcurve data file consists of three parts:  the asteroid            
list, the reference list, and this explanation, which includes a list of        
footnotes at the end.  The reference list is numbered and sorted by             
first author plus date.  Each citation includes the year, all authors,          
journal or book name, volume, and first and last page numbers.                  
                                                                                
     The asteroid list is ordered by asteroid number, followed by the           
asteroid name, the period in hours, amplitude of variation or range of          
amplitude observed.
                                                                                
       FOOTNOTES AND ALTERNATE VALUES FOR AMBIGUOUS PERIODS                     
                                                                                
   4  Degewij and Zellner (1978) and Degewij et al. (1979) show that            
      variation is primarily due to albedo and not due to shape.  Taylor        
      (1985) found no asymmetry in the 10-hour lightcurve as claimed by         
      Taylor (1973) when he reobserved at similar aspect.  Magnusson (1986)     
      obtains a better solution for the pole position of Vesta with a           
      5-hour period than with a 10-hour period.                                 
   9  Correct period is 5.079 hrs.  Other values resulted from cycle            
      errors in compositing lightcurves.                                        
  26  P = 10.60 or 13.13 hours.                                                 
  56  P = 13.7 or 19.0 hours.                                                   
 139  P = 20.9 or 41.8 hours.                                                   
 249  P = 42.62 or 85.24 hours.                                                 
 288  Period may be a precession period (see 1220 footnote).                    
 372  P = 6.58, 8.67, or 12.83 hours.                                           
 387  P = 16.0, 24.0, or 48.0 hours.                                            
 393  P = 19.35 or 38.7 hours.                                                  
 439  P = 19.2 or 38.4 hours.                                                   
 683  P = 4.3, 5.3, or 8.6 hours.                                               
 704  Pole position inferred from YANG 65 observation.                          
 804  P = 7.42 or 14.851 hours.                                                 
 944  Accurate period quoted by Tedesco (in "Asteroids", ed. T. Gehrels,        
      Tucson: Univ. Ariz. Press, pp 1098-1107.)                                 
1220  A modulation of P=7.90 hr, Ampl=0.15 mag was observed near minimum        
      light of the longer period variation.  BINZEL 84B interprets this         
      as the real rotation period, with the long period being a preces-         
      sion period caused by an unseen satellite. 288 Glauke may be              
      another case of the same phenomenon.                                      
3552  P = 3 or 7 hours.