This HTML file was created by the program doc_tsuite.pl. doc_tsuite.txt contains a tab delimited list of the files.

agn_blr_albedo.in measure rayleigh scattering of Lya

This model computes the albedo of a fairly standard BLR cloud. This is the type of model that was presented in the BLR albedo paper by Korista & Ferland, 1998, ApJ 495, 672.

The print diffuse continua command enters continuum fluxs into the emission line stack. The asserts then check that these continua have the expected brightness.

agn_lex00_u0.in intermediate-ionization x-ray ionized cloud from Lexington 2000

This is one of the "warm absorber" simulations presented at the Lexington 2000 meeting on nebulae. Pequignot et al. summarized in 2001ASPC..247..533P. It is necessary to also include the command no induced processes to obtain the results presented there. This disables UTA ionization, a process that was not included in the calculations presented in the paper.

agn_lex00_u1.in high-ionization x-ray ionized cloud from Lexington 2000

This is one of the "warm absorber" simulations presented at the Lexington 2000 meeting on nebulae. Pequignot et al. summarized in 2001ASPC..247..533P. It is necessary to also include the command no induced processes to obtain the results presented there. This disables UTA ionization, a process that was not included in the calculations presented in the paper.

agn_lex00_um1.in low-ionization x-ray ionized cloud from Lexington 2000

This is one of the "warm absorber" simulations presented at the Lexington 2000 meeting on nebulae. Pequignot et al. summarized in 2001ASPC..247..533P. It is necessary to also include the command no induced processes to obtain the results presented there. This disables UTA ionization, a process that was not included in the calculations presented in the paper.

agn_reflector.in model of Compton reflector

This is a model of the Compton reflector in AGN. It is a constant temperature since models of this region often make that assumption. A plot in Part I of Hazy shows the incident and reflected portions of the continuum. The code will complain that the cloud is Compton thick since it is not really designed to simulate this situation.

agn_S_curve_grid.in temperature across Spitzer thermal stability S curve

This computes a series of models that check the temperature through the S curve in the Fields et al. three-phase model of ISM stability.

agn_warm_absorber.in simple warm absorber model

this is a simple warm absorber model. It makes a plot of the transmitted continuum, and generates a list of lines with significant optical depths

aperture_beam_int.in test aperture beam command with intensity

This is a homogeneous sphere that is especially simple. The model is a test of the aperture command, a command that simulates observing part of an extended object. In this case the aperture is a beam contered on the center of the nebula, with a line of sight extending through the object.

The code carries along a dummy emission line ("Unit 1") with a constant intensity of 1e-10 erg cm-3 s-1. The line goes through all of the code's infrastructure, and when the calculation is complete, the program confirms that the "luminosity" of the line is the emitting volume times 1e-10. The aperture command is verified by asserting that the emission line has the correct "luminosity". In this case the inner radius is not specified so the returned value is unity.

aperture_beam_lum.in test aperture beam command with luminosity

This is a homogeneous sphere that is especially simple. The model is a test of the aperture command, a command that simulates observing part of an extended object. In this case the aperture is a beam contered on the center of the nebula, with a line of sight extending through the object.

The code carries along a dummy emission line ("Unit 1") with a constant intensity of 1e-10 erg cm-3 s-1. The line goes through all of the code's infrastructure, and when the calculation is complete, the program confirms that the "luminosity" of the line is the emitting volume times 1e-10. The aperture command is verified by asserting that this emission line has the correct "luminosity".

aperture_slit.in test aperture slit command with luminosity

This is a homogeneous sphere that is especially simple. The model is a test of the aperture command, a command that simulates observing part of an extended object. In this case the aperture is a long slit contered on the center of the nebula, extending beyond the outer reaches of the matter.

The code carries along a dummy emission line ("Unit 1") with a constant intensity of 1e-10 erg cm-3 s-1. The line goes through all of the code's infrastructure, and when the calculation is complete, the program confirms that the "luminosity" of the line is the emitting volume times 1e-10. The aperture command is verified by asserting that the emission line has the correct "luminosity".

blr_f92.in standard blr cloud in Ferland et al. 1992

This is similar to one of the BLR models presented in Ferland et al. (1992) for the well-studied Seyfert galaxy NGC 5548. It has a very large column density and is marginally optically thick to electron scattering. The spectrum is given relative to Lya, and the intensity of this line is reset to produce a spectrum that is on the same intensity scale as that paper.

blr_fp89.in final F+P 1989 BLR model table 3

Ferland and Persson (1989) presented this calculation of a BLR cloud. The differences between the present predictions and those given by FP are largely due to improved treatment of Balmer line escape and destruction. The spectrum is given relative to a Lya intensity of 100. The column density is VERY large, to reproduce intensities of low-ionization lines, especially the Ca II lines.

blr_hizqso.in high Z quasar cloud

This is a model of a very high metallicty BLR cloud. It checks the intensities of some of the brigher lines, and is a check that the code can converge a cloud with this high Z.

Secondary ionization is very important when H is highly ionized, due to very high He abundance. Sec ionization becomes important at the He+ - He ionization front, where H+/H is 1e-5.

blr_kk81.in old blr

This is the "standard" BLR model presented by Kwan and Krolik (1981).

>>refer blr cloud Kwan, J., & Krolik, J. 1981, ApJ, 250, 478

Compare line intensities to previous versions of CLOUDY by entering into table on page Error! Bookmark not defined..

The code caution that the resulting total pressure was not constant is to be expected. The KK calculation assumed constant gas pressure, but internally generature line radiation pressure is significant. Because of this the sum of gas plus radiation pressure was not constant although the gas pressure was.

blr_level2.in test dominant level2 lines

This model checks predictions for the "level2" lines. These are lines that are normally very weak, have Opacity Project wavelengths, and g-bar collision strengths. Phosphorus is given a large abundance so that its level2 lines are significant.

blr_n09_p18.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e18 cm2 s-1

This is one of the 5 models that sample the LOC plane.

blr_n09_p18_Z20.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e18 cm2 s-1, Z=20

This is one of the 5 models that sample the LOC plane.

blr_n09_p20.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e20 cm2 s-1

This is one of the 5 models that sample the LOC plane.

blr_n09_p20_Z20.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e20 cm2 s-1, Z=20

This is one of the 5 models that sample the LOC plane.

This simulation is optically thin in the Lyman continuum - no H ionization front is present. As a result it can be difficult to converge.

blr_n09_p22.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e20 cm2 s-1

This is one of the models that sample the LOC plane.

blr_n09_p22_Z20.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e22 cm2 s-1, Z=20

This is one of the models that sample the LOC plane.

blr_n11_p20.in BLR model, density 1e11 cm-3, flux of H-ion phots 1e20 cm2 s-1

This is one of the 5 models that sample the LOC plane.

blr_n11_p20_Z20.in BLR model, density 1e11 cm-3, flux of H-ion phots 1e20 cm2 s-1, Z=20

This is one of the 5 models that sample the LOC plane.

blr_n12_p19.in BLR model, density 1e12 cm-3, flux of H-ion phots 1e19 cm2 s-1

This is one of the 5 models that sample the LOC plane.

blr_n12_p19_Z20.in BLR model, density 1e12 cm-3, flux of H-ion phots 1e19 cm2 s-1, Z=20

This is one of the 5 models that sample the LOC plane.

blr_n13_p18.in BLR model, density 1e13 cm-3, flux of H-ion phots 1e18 cm2 s-1

This is one of the 5 models that sample the LOC plane.

blr_n13_p18_Z20.in BLR model, density 1e13 cm-3, flux of H-ion phots 1e18 cm2 s-1, Z=20

This is one of the 5 models that sample the LOC plane.

blr_n13_p22.in BLR model, density 1e13 cm-3, flux of H-ion phots 1e22 cm2 s-1

This is one of the 5 models that sample the LOC plane.

blr_n13_p22_Z20.in BLR model, density 1e13 cm-3, flux of H-ion phots 1e18 cm2 s-1, Z=20

This is one of the 5 models that sample the LOC plane.

blr_nf84.in early model of blr

This is an example of a "conventional" BLR calculation. The parameters are similar to those of Table 1 of Netzer and Ferland (1984). Notice that the ratio of Lyalpha to Hbeta ratio is much larger than observed.

>>refer blr model Netzer, H., & Ferland, G. J. 1984, PASP, 96, 593

blr_nf84_45deg.in early model of BLR, with illumination at 45 degree angle

This is an example of a "conventional" BLR calculation. The parameters are similar to those of Table 1 of Netzer and Ferland (1984). Notice that the ratio of Lyalpha to Hbeta ratio is much larger than observed.

>>refer blr model Netzer, H., & Ferland, G. J. 1984, PASP, 96, 593

blr_rnfa.in table 1 of Rees et al. ApJ 347, 648

This is the lower density cloud computed in Rees et al. (1989). Table 1 of that paper lists the predictions, which were a mean of those of Hagai Netzer's ION and roughly version 76 of CLOUDY. The lines are generally still in good agreement with the predictions of that paper. In particular the changes in the line fluxes shown in Figure 1 of that paper are reproduced quite well.

blr_rnfb.in table 1 of Rees et al. ApJ 347, 648

This is a very dense cloud, and was computed in Rees et al. (1989). Table 1 of that paper lists the predictions, which were a mean of those of Hagai Netzer's ION and roughly version 76 of CLOUDY. The lines are generally still in good agreement with the predictions of that paper. In particular the changes in the line fluxes shown in Figure 1 of that paper are reproduced quite well. The fluxes of Lya and Hb are not reproduced with great precision by this model because of changes in collision rates for hydrogen and especially the form of the escape probability function for subordinate lines. As Figure 1 of RNF showed the line intensities are very sensitive to density for these parameters.

coll_coronal.in model of active region of solar corona

This is a rough model of the solar corona. The test checks that the coronal equilibrium commands work. The gas is predominantly collisionally ionized.

coll_heat_only.in test code in limit where ONLY mechanical heating is present

This test is an optically thin collisionally ionized gas with no photoionization at all.

coll_t3.in coronal equilibrium at 10^4 K

This tests conditions of collisional equilibrium at low densities. This is one of a series of sims coll_t?.in which test ionization over a range of temperatures. This one, unlike the others, includes cosmic rays. Chemistry is important at this low temperature and the chemical network will collapse without a source of ionization. The cosmic rays provide this source of ionization.

coll_t4.in coronal equilibrium at 10^4 K

this tests conditions of collisional equilibrium at low densities

coll_t5.in coronal equilibrium at 10^5 K

This is a test collisional ionization equilibrium at 1e5 K.

coll_t6.in coronal equilibrium at 10^6 K

This test is an optically thin collisionally ionized gas.

coll_t7.in coronal equilibrium at 10^7 K

Test with only collisional ionization at a high temperature.

dynamics_orion_flow.in Orion nebula blister with wind

This is a model similar in spirit to the blister geometry H+ region model computed by Baldwin et al. (1991), but with a D-critical flow. Many physical processes have been disabled to make this simulationn faster. Grain physics is not done so the gas temperature is incorrect. The main purpose is to do a quick test of the dynamical flow with grain opacities included. The slow directory contains a full simulation of a flow like Orion.

dynamics_veryfast.in very fast wind model

This is meant to be a very fast calculation to use when running extensive debug-enabled runtimes.

dynamics_veryfast_rec.in very fast wind model

This is meant to be a very fast calculation to use when running extensive debug-enabled runtimes.

dynamics_wind.in test of equations of motion in a very highly ionized wind

This tests the radiative acceleration and terminal velocity of a wind in which only electron scattering is important. The parameters were chosen so that electron scattering is the dominant opacity source, so that the equations can be solved both numerically (in the example) and analytically (the expected solution given above). In a realistic wind the gas would be more neutral and line driving would dominate. The force multiplier, given in the punch wind output, is nearly unity as a result.

Checks:
- The radiative acceleration is correct (e- 9.543910-7 cm s-2).
- The terminal velocity should be 7.57 km s-1.
- Force multiplier near unity (no line driving since so highly ionized).
- Thickness of cloud correct (R-Ro + dr/2 should be 3.086391017 cm).

feii_hin.in test feii in high density limit

This checks that, at high particle densitites, in which the gas should be in collisional equilibrium, the level populations of the large model Fe+ ion go to the proper values, where the departure coefficients are all equal to unity.

feii_hirad.in feii in case of high radiation density limit

This checks that, at high radiation densitites, in which the gas is irradiated by a blackbody in strict thermodynamic equilibrium, the level populations of the large model Fe+ ion go to the proper values, where the departure coefficients are all equal to unity.

feii_pump.in test feii in continuum pumped limit

This is a constant temperature low ionization cloud, with BLR-like densities, which includes the large FeII atom. The tests check on the emission predicted in the Fe II bands.

This model tests the large FeII model in the optically thin, continuum pumped limit. The zone thickness is set to a small value (1 cm) so that full continuum hits atom.

feii_ste.in thermal equilibrium of FeII in STE limit

This model has a very high iron abundance, 100x H, and most Fe is in the form of Fe+. It is irradiated by a blackbody in strict thermodynamic equilibrium. We check that the temperature of the gas is equal to the radiation temperature, to confirm that the thermal properties of the model FeII atom obey thermodynamics.

feii_t4.in FeII emission in typical intermediate density photoionzied cloud

This model has a very high iron abundance, 100x H, and most Fe is in the form of Fe+. it has intermediate density and should produce and FeII spectrum something like an AGN. The set line precision 6 increases the number of significant figures in the wavelengths for each line. This is needed to get the right FeII inward band.

func_abund_fluc.in check fluctuating heavy-element abundances

This checks that the variable abundances option works

func_distance.in check that distance and "print flux earth" commands work

Normally the code predicts the intensity or luminosity of the emission lines. This test confirms that it can predict the flux recieved at the Earth instead. The model is the simplest and fastest that can be computed - a H-only constant temperature single zone. The total luminosity is set to 1e40 erg/s, and the ionization source is a laser at 2 ryd. With these set, the total luminosity in ionizing radiation, the total luminoisity in the incident continuum (the emission line labeled "Inci 0") will be 1e40.

The code will predict the flux at the Earth if both the distance to the oject is specified with the distance command, and this is requested with the print flux earth command. The distance was chosen so that the total flux at the Earth will be 1 erg/s. This is asserted at the end of the calculation.

func_dlaw.in test model with dlaw table

this model tests the dlaw density table command

func_fulltrace.in test full trace output

this checks that trace output functions correctly

func_globule.in test of globule command

This model uses the globule command, tests that the zoning logic works for this extreme case, and that the code is able to converge the globule model.

func_grid_line_ratios.in test generating line ratios in a grid run

This uses the grid command to compute line ratios for a wide range of density and temperature. The ionization is set to a uniform value and only a few elements are included. this makes the calculation faster and prevents recombination [O III] 4363 from becoming important (there is no O+3).

These are the line ratios mentioned as limits in the Johnstone et al. Spitzer cooling flow filament paper (2007).

func_hotgas_coolstar.in test very soft continuum, very hot gas

This is a test where the CMB is the only continuum source. It does not extend to energies where the code needs to work. There are special cases used in this situation, for continuum addressing, so this checks whether those still function.

func_ion_increase.in test model where ionization increases with depth

This density falls off faster than 1/r^2 so the ionization increases with depth. Most sims have decreasing rather than increasing ionization.

func_lines.in create output file with list of func_lines

This runs the standard "test" case, and then creates the line data and labels files. Test by itself includes many asserts, so no further asserts are needed here.

The file func_lines.lab is a useful list of all lines predicted by the code. Cut and paste this into other places when you need to find a particular emission line.

The func_lines lines.dat gives atomic data for all the lines, and their critical density at 10000 K. The large H2 and Fe II model atoms are turned on to include their lines.

func_map.in map of heating vs cooling

This is a test of the continuity of the code over a very large range of temperature. It was used to produce one of the thermal maps shown in Hazy.

Checks:
- No breaks in the heating and cooling curves where various approximations change.

func_sdrmin.in test set drmin command

This simulation tests the SET DRMIN command. It is a toy model of a planetary nebula that is designed to extend into the PDR. The minimum stepsize is deliberately set much too large so that we would immediately notice if the command was broken. It also tests if we still hit the correct outer radius when SET DRMIN is used. Without the SET DRMIN command this sim would need 410 zones (trunk@2760).

func_set_ion.in test impact of setting ionization

c class function c ======================================== c this script exercies the option to specify the ionization of a species

func_stopline1.in test stop line command

This is an example of a simple calculation that stops when a line reaches a specified intensity. The option to turn off elements with trivial abundances is used.

func_stopline2.in test stop line command

this is an example of a simple calculation that stops when a certain emission line ratio is reached

func_t10.in test very soft continuum, very hot gas

This is a test of the highest temperature the code can do.

func_t3.in test low temperature limit of code, 3K

This is a test of the lowest temperature the code can do. It runs a constant temperature of 3K

func_test.in run smoke test

This runs the smoke test command, which include several asserts. The tests the behavior of increasing the number of significant figures in printed wavelengths.

func_testmole.in this runs the standard, one command, test, which contains many asserts

This runs the "test mole" command, which include several asserts.

func_trans_punch.in first of func_trans_punch/transread pair, punch continuum

func_trans_punch.in and transread.in are a pair of tests that check that the code can punch a transmitted continuum then read it.

This sim must come before func_trans_read since it generates the punch file needed by func_trans_read. Alphabetical order insures this.

func_trans_read.in second of transpunch/transread pair, used transmitted continuum

func_trans_punch.in and func_trans_read.in are a pair of tests that check that the code can punch a transmitted continuum then read it.

grains_conserve_pp.in test energy conservation with vastly optically thick dust

This tests that multiple absorption / reemission by dust conserves energy Energy density and grain temperatures should be exactly 500 K

grains_conserve_sp.in test energy conservation with vastly optically thick dust, sphere geometry

This tests that multiple absorption / reemission by dust conserves energy in a spherical geometry. Radiation density temperature in last zone should be 500 * sqrt(1e21/1e26) = 1.5811 K

grains_hot.in test temperature of gas and dust in high energy density environment

This tests the grains in an extreme condition - irradiation by an AGN near the illuminated face of the molecular torus. The gas is predominantly heated by the grain electron photo-ejection.

grains_hot_wd01.in test temperature of gas and dust in high energy density environment

This tests the grains in an extreme condition - irradiation by an AGN near the illuminated face of the molecular torus. The gas is predominantly heated by the grains. The grain treatment has been reverted to Weingartner & Draine, 2001, which is NOT appropriate for these conditions. It is however a good test whether the old treatment is not broken....

grains_lte.in check that grains equilibriate at correct temp in ste limit

This test irradiates a set of grains with a true blackbody in strict thermodynamic equilibrium. We expect the grains (and everything else) to equilibriate at the blackbody temperature. The gas temperature is forced to the radiation temperature because the current molecule network (based on ISM approximations) does not go to LTE in the high-radiation density limit. The calculation asserts that all grain temperatures are very close to the radiation temperature.

grains_qheat.in cool atomic ISM with Si grain quantum heating

This sim produces dust emission with a Wein trail that is dominated by quantum heating emission.

grains_temp.in test all grain species temperature

This turns on all the grain species that are included in the distribution. A model of an ionized layer is done and the monitors confirm the resulting grain temperatures.

grains_temp_all.in test all grain species temperature

c grains_temp_all.in c class limit c ======================================== c

This is a relatively quick test of grains. The Orion and ISM silicate and graphitic grains are turned on and their equilibrium temperature checked.

h2_cr.in H2 with background cosmic ray ionization

This test conditions of cosmic ray ionization. Solar abundances with no dust are assumed so this involves gas-phase chemistry alone. The Solomon process is disabled with the "no induced processes' command so H2 is mainly dissociated by cosmic rays. This forms a pair with h2_cr_grains, which does include grains.

h2_cr_grains.in background cosmic ray ionization by suprathermal electrons only

This tests conditions of cosmic ray ionization and grain formation pumping. Solomon process is turned off with the "no induced processes" command so cosmic rays are the main dissociation process. This forms a pair with h2_cr which does not include grains, so relies only on gas-phase chemistry.

h2_hminus.in H2 populations in H- dominated limit

This tests large H2 model in limit of H- formation and Solomon destruction.

h2_pdr_leiden_f1.in low density and flux model 1

This is one of the tests in Rollig et al. 2007, A&A, 467, 187

h2_solomon.in H2 populations in solomon dominated limit

This test H2 in case of grain formation and solomon destruction

h2_t2000.in test large H2 molecule in shock-like conditions

This is a collisionally dominated H2 simulation. The temperature has been fixed at 2000K and the large molecule turned on. The calculation checks the returned value of the ortho to para densities. Cosmic rays and the incident continuum have little effect, the density is high, so the populations should be close to LTE.

h2_t500.in test large H2 molecule in PDR-like conditions

This is a dense molecular gas with background cosmic rays and the incident radiation field set to a small value. The lower levels are in LTE.

h_otsopen.in test ots, inward fractions for pure hydrogen, open geo, filling factor

This tests the total emission from a hydrogen Stromgren sphere using the OTS approximation. The conservation of the total number of ionizing photons, and the emitted spectrum, are all checked.

h_otspp.in plane parallel conservation and hydrogenic emission for pure hydrogen

This tests the total emission from a plane parallel pure hydrogen Stromgren sphere using the OTS approximation. The conservation of the total number of ionizing photons, and the emitted spectrum, are all checked.

h_otssp.in spherical conservation and hydrogenic emission for pure hydrogen

This tests the total emission from a spherical pure hydrogen Stromgren sphere using the OTS approximation. The conservation of the total number of ionizing photons, and the emitted spectrum, are all checked.

h_outopen.in test open geometry

This tests the total emission from an open geometry, hydrogen Stromgren sphere, using the outward only approximation. The conservation of the total number of ionizing photons, and the emitted spectrum, are all checked.

h_outpp.in plane parallel H-only, close, test hydrogenic emission

This tests the total emission from a plane parallel pure hydrogen Stromgren sphere using the outward only approximation. The conservation of the total number of ionizing photons, and the emitted spectrum, are all checked.

h_outsp.in spherical conservation and hydrogenic emission for pure hydrogen

This tests the total emission from a spherical pure hydrogen Stromgren sphere using the outward only approximation. The conservation of the total number of ionizing photons, and the emitted spectrum, are all checked.

h_t4_conemis.in continuous emission from H atom

This tests the continuous emission from the model H atom. The gas temperature is 10,000 K and the continuous emissivity is asserted for a range of wavelengths.

This was used to generate the plot in Hazy 2 comparing the emission from a pure hydrogen plasma with those of Ferland 1980.

//>>refer HI emission Ferland, G. J. 1980, PASP, 92, 596

h_t4_conemis_lon.in low-den continuous HI emission with 2-nu important

This is a mate to hatomt10.in except that the density is low enough for two-photon emission to be very imporant in the optical and uv.

h_t4_conemis_thick.in H I continuous emissivity, used for plot in hazy

This checks that the predicted hydrogen continuum is in good agreement with exact results in the optically thin nebular limit.

Checks:
- This output was used to generate figure h_t4_conemis_thick in Part I of HAZY.
- Continuum relative to Hbeta should agree with Ferland (1980) filter averaged results.
- Hbeta should agree with Case B predictions, and Q(H) 4861.

heatomt10.in continuous emission from HeI

This tests continuous emission from the He I atom. The laser is used so that the incident continuum is not included in the total emission.

heatomt10lon.in test low-den continuous emission from H atom, 2-nu is important

This is a mate to hatomt10.in except that everything is He at low density

heiont10.in continuous emission from HeII

This tests the He II continuous emission. The helium abundance is very large so that He II overwhelms other emission sources. The resolution of the continuum mesh is increased so that we get a better representation of the continuous emission.

helike_ar.in He-like argon emission

test He-like emission for argon

helike_c.in he-like carbon emission

test he-like carbon emission

helike_co.in He-like cobalt emission

test emission of He-like Co

helike_cu.in He-like copper emission

test emission of He-like Cu

helike_fe.in he-like iron emission

check He-like emission for iron

helike_mg.in he-like magnesium emission

test He-like Mg emission

helike_n.in He-like nitrogen emission

test He-like emission for N

helike_ne.in he-like neon emission

test He-like emission for oxygen

helike_ni.in he-like nickel emission

Test He-like Ni emission.

helike_o.in he-like oxygen ion vs. Bautista & Kallman 2000 Table 1, column 3

test He-like emission for oxygen

helike_si.in He-like silicon emission

test He-like emission for silicon

helike_zn.in He-like zinc emission

test emission for He-like Zn

hhe_otspp.in plane parallel conservation and H-like emission for H, He

This tests the total emission from a spherical pure H + He Stromgren sphere using the outward only approximation. The conservation of the total number of ionizing photons, and the emitted spectrum, are all checked.

hhe_otssp.in spherical conservation and H-like emission for H and He

This tests the total emission from a spherical pure H + He-like Stromgren sphere using the outward only approximation. The conservation of the total number of ionizing photons, and the emitted spectrum, are all checked. The geometry is plane paralel.

hhe_outpp.in plane parallel conservation emission for H, He gas

This tests the total emission from a spherical pure hydrogen Stromgren sphere using the outward only approximation. The conservation of the total number of ionizing photons, and the emitted spectrum, are all checked.

hhe_outppff.in plane parallel filling factor pure H, He gas

This is a plane-parallel constant temperature cloud with only hydrogen and helium. The gas has a filling factor of 0.1. Induced processes are turned off and a large H atom is used so that the hydrogen recombination spectrum will be close to Case B. The calculation stops beyond the hydrogen ionization front, because of the stop efrac command (it needs this since this is a constant temperature calculation, so the usual lower-temperature stopping criterion does not apply). The asserts confirm that energy is conserved and that the hydrogen spectrum is correct.

hhe_outsp.in spherical conservation and H-like emission for H, He

This tests a spherical cloud with only hydrogen and helium. Diffuse fields are transferred with the outward only approximation. The asserts check that the ionizing radiation is conserved.

hii_blister.in Lexington 1995 dust-free hii blister region

This is one of the test cases from the Lexington Meeting suite of nebulae (Ferland et al. 1995). It is a grain-free hii_blister HII region, similar to inner regions of the Orion Nebula, except for the absence of grains. The set of lines entered with the print line sum command lists the most powerful coolants in this model. This is one of the tabulated quantities in the Lexington Meeting, and is a fundamental test of energy conservation in the code. The ratio of the sum of these lines to Hb is equivalent to the Stoy ratio, used for determining stellar temperatures.

The "dielec kludge 0" command is to turn off my estimates of the DR rates for those elements that had none. This was only to allow comparison with other calculations that did not make similar estimates. For an actual calculation I would not include this command, since the guesses are better than nothing.

the turbulence is to stop the balmer lines from becoming optically thick since few other codes include an actual H atom, but use case b instead. The Orion HII region does have an observed turbulence of about 8 km/s.

This calculation stops near the H+ - H0 ionization front, where the temperature falls below the default lowest temperature of 4000 K. This model would have continued into the PDR had a lower temperature been specified with the STOP LOWEST TEMP command.

hii_coolstar.in dust free cool HII region model, Lexington 1995

This is one of the test cases from the Lexington Meeting suite of nebulae. It is a grain-free HII region ionized by a very cool star. Hydrogen is ionized but not helium so this tests the transport of the H Lyman continuum. The set of lines is entered with the print line sum command to test energy conservation.

hii_icf.in HII region with negative He/H ICF

This is an example of an H II region irradiated by a hard stellar continuum - one of the Mihalas NLTE stars. The hard continuum produces a negative He/H ionization correction factor, as discussed in Ballantyne, Ferland & Martin (2000). >>refer HeI icf by Ballantyne,D.R., Ferland, G.J., & Martin, P.G., 2000, ApJ 536, 773-777

hii_paris.in "New" Paris meeting HII region

This is one of the "standard" models computed at the Paris and Lexington meetings on photoionization and shock calculations. a bable in hazy compares the predictions of the current version of CLOUDY with predictions of a few of the other codes. It is necessary to iterate since some fine structure lines are optically thick. The set of lines entered with the print line sum command is used to obtain the total luminosity in detected lines, a measure of the Stoy temperature.

Checks:
- Hb close to case B, Q(H) 4861, intensities.
- Enter answers in Table Error! Reference source not found..

hlike_c.in H-like C VI case B

hlike_o.in H-like O VIII case B

igm_lalpha.in Ly alpha forest cloud

igm_primal.in cloud with primordial abundances exposed to background at Z=10

igm_z3.in redshift 1000 recombination epoch

This is a model of the universe near the recombination epoch, at a redshift of a thousand. The gas is exposed to a true blackbody at 3000 K, and the abundances are primordial.

ism.in cloud irradiated by ism background

TODO - look at temperature struture - it has jitter at about the level of convergence, up and down. Temp jitter caused by eden jitter. This model is nearly isothermal, jitter measures noise in solver, and is great chance to pin this down.

This is a test of the behavior of the code in the extreme of photoionization by a relatively hard continuum, at low densities. The continuum is the galactic background, attenuated by a column density of 10^22 cm-2. Ionization by galactic background cosmic rays is included. Case b appears since this region is deep in the ISM, and the Lyman lines are quite thick. This example checks whether the ionization balance, thermal balance, and electron density sum, are performed correctly in this limit.

Checks:
- Numerical stability of solution
- Thickness exact

ism_cosmicray.in background cosmic ray ionization by suprathermal electrons only

This test conditions of cosmic ray ionization. Molecules and charge transfer are disabled so that analytical estimates can be made.

ism_grid.in interstellar cloud irradiated by ism background

this shows an S-curve calculation - make plot showing density as X-axis and gas pressure (nT) as y-axis

the gas is ionized by the galactic background. the density varies between 1e-3 and 100 cm-3. this is the full range found in the diffuse ism. The components that are produced are CNM - cold neutral medium, density ~ 40 cm-3 WNM - n ~ 0.5 cm-3, WIM - warm ionized medium, n ~ 0.25 cm-3 HIM - hot ionized medium, n ~ 1e-3 cm-3, calculation DOES NOT reproduce observed temperature of HIM - we get ~1e4K but observed is ~1e6 K. HIM is shock, not photo, ionized

ism_hot_brems.in generate continuum due to hot ism in high Z,z starburst

This model generates a large column constant density cloud similar to the hot phase of the interstellar medium. The continuum is punched to generate one of the figures in Part 2 of Hazy.

There is a strange feature between 1.7e-3A and 2.2e-3A that is the N emission (head starting at 1.7e-3A with O absorption at 2.2e-3A. This model is strongly enriched in heavies so many metal edges, esp O, are optically thick.

>>TODO 1 the guess of the thickness of the first zone is badly too small, because this model is collisionally ionized, and it used Stromgren length - better to use collisional balance and dr - as result of this the model takes far too many zones

ism_jura.in check rate H2 forms on grain surfaces

This model started out life as the Tielens & Hollenbach 1985 pdr. The density was set to unity and the incident radiation field adjusted so that the two default grains have temperatures near 100K. The model asserts that the H2 formation rate on grain surfaces is close to the //>>refer H2 grain physics Jura, M., 1975, ApJ, 197, 575 rate.

ism_opacity.in generate standard ISM opacity curve

This example creates the file ism_opacity.opc which tabulates the total opacity of the gas as a function of energy. These plots are used in ISM studies to understand the transmission characteristics along a line of sight. The opacity depends on the dust to gas ratio, the gas phase abundances, and the level of ionization, all of which can be changed by altering parameters given above.

The model is of a 1 cm think parcel of gas which is optically thin in the Lyman continuum and Lyman lines. As a result the hydrogen emission line spectrum is close to case C. The model iterates so that the predicted ionization and emission know about this.

ism_set_cr_rate.in background cosmic ray ionization by suprathermal electrons only

This test conditions of cosmic ray ionization. Molecules and charge transfer are disabled so that analytical estimates can be made.

limit_casea_h_den13.in case A

Case A is a mathematical fiction; when the Lyman lines are optically thin continuum pumping must be important if the gas is ionized. Fluorescence is turned off with the no induced processes command. The density is set to a very high value (1015 cm-3) so that the 2s-2p states are well l-mixed, in keeping with standard case A assumptions. As a result, collisional excitation would dominate the level populations, and hydrogen collisions must be turned off with the hydrogen collisions off command. The Ly* optical depth is set to a small value. The set dr command sets the zone thickness to 1 cm. The abundances are set to a very small value so that the electron density is equal to the hydrogen density.
Checks:
- Departure coefficients for H, He levels
- Neutral fractions
- H* emissivity

limit_casea_h_den_temp.in Test model H in Case A limit

this tests the predicted H I and He I spectra in the Case B limit. The grid is over both density and temperature.

limit_caseb_h_hs87.in "Case B from Hummer and Storey"

limit_caseb_h_lot.in log density case B, T=500 log n=2

c limit_caseb_h_lot.in c class limit c ======================================== c

This tests the ionization and emission line spectrum for H case B at a low density and temperature.

limit_caseb_h_n8.in h_caseb_n8 high density case B

This test case compares the predictions of the multi-level hydrogen atom with the Storey and Hummer (1995) results. The set dr command sets the zone thickness to 1 cm. The case b command sets Lyman line optical depths to very large values.
Checks:
- Neutral fractions
- H* emissivity
- Relative line intensities

high density causes disagreemeent with HS - collisions

limit_caseb_he2_den8.in limit_caseb_he2_den8 He II case B

This test case compares the predictions of the multi-level hydrogen atom with the Storey and Hummer (1995) results. The set dr command sets the zone thickness to 1 cm. The case b command sets Lyman line optical depths to very large values.
Checks:
- Neutral fractions
- H* emissivity
- Relative line intensities

limit_caseb_he_den.in Test model H and He atoms in Case B limit

this tests the predicted He II spectra in the Case B limit.

this effectively turns off hydrogen to avoid the problem with every other heII line lying beneath an HI line. this is done by reducing the number of levels for H I.

this asserts the values are within 9% for the standard T = 1e4K and a range of densities. Actually they are all nearly within a few percent except at the lowest temperature of 5,000K.

limit_caseb_he_den4_temp4.in the best we can do to predict the HeI emission spectrum

This is close to the best and most complete model of He I that the code can do. it is not hacked to try to reproduce HS?

limit_caseb_he_den_temp.in Test model He atoms in Case B limit

this tests the predicted He II spectra in the Case B limit.

this effectively turns off hydrogen to avoid the problem with every other heII line lying beneath an HI line. this is done by reducing the number of levels for H I.

this asserts the values are within 15% for a range of density and temperature. Actually they are all nearly within a few percent except at the lowest temperature. The error greater than 10% occurs at the lowest temperature of 5,000K.

limit_caseb_hhe_den.in Test model H and He atoms in Case B limit

this tests the predicted H I and He I spectra in the Case B limit.

the grid is over density at the standard temperature of 1e4 K.

limit_caseb_hhe_den_temp.in Test model H and He atoms in Case B limit

this tests the predicted H I and He I spectra in the Case B limit. The grid is over both density and temperature.

limit_casec_h_den2.in H only optically thin in Lyman continuum

This is a pure hydrogen cloud that is optically thin in the Lyman continuum. The asserts check the emission in several H I lines and continua. This should be close to what really happens in a low column density cloud exposed to a continuum source that does not have strong Lyman lines. (The continuum source used is a pure blackbody, and so has no lines). So this is an example of "Case C" emission >>refer H case C Ferland, G.J. 1999, PASP, 111, 1524

limit_casec_h_den5.in case C

This is Case C, what really happens when optically thin gas is irradiated by a continuum with Lyman line continuum fluorescence allowed.
Checks:
- Departure coefficients for H, He levels
- Neutral fractions
- H* emissivity Case C is described in

>>refer H case C Ferland, G.J. 1999, PASP, 111, 1524

limit_compton_hi_t.in test high-T Compton energy exchange

This is the highest Compton temperature that can be computed in LTE on an IEEE 32-bit processor. This tests the code in the high-temperature Compton limit. Temperatures as high as 10^10 K can be computed successfully on CPUs with longer word lengths, such as a Cray or the new 64 bit processors.

Checks:
- The equilibrium temperature should be exactly 107.4 K (2.51239107 K).

limit_compton_lo_t.in test low-T Compton energy exchange

This tests the code in the low temperature Compton limit. The gas is illuminated by a 3 K blackbody in thermodynamic equilibrium. The equilibrium temperature should be exactly 3 K. It is necessary to add an extra component of free electrons to test the code in this limit with the eden command.

limit_compton_mid_t.in mid-T Compton energy exchange

This tests the behavior of the code in the Compton limit. The incident continuum is a blackbody in strict thermodynamic equilibrium. Strict thermodynamic equilibrium is expected for all constituents of the gas. The input stream also lists the expected photon fluxes for the incident continuum; this tests the normalization of the continuum, and its distribution. Grains are included to confirm their behavior in the LTE limit. The set dr command sets the zone thickness to 1 cm.

Checks:
- Luminosity, photon flux, over various energy intervals, 4*J at 912143.
- Electron temperature exactly 2*105 K.
- Grain temperature forced to 2*105 K by radiative processes.

limit_conserve.in test that energy is limit_conserved

This checks that energy is limit_conserved. The code always checks that it did not radiate more energy than was absorbed. This calculation extends well past the photo-dissociation zone into fully molecular gas, so that all of the incident radiation is absorbed. Grains, CMB, & CRs are not present so that only the incident radiation field powers the gas.

Small changes can affect this model to surprising extents because of the presence of a major thermal front at the H0 - H+ transition region.

limit_eden.in Martin Gaskell's funny model

This is mainly a test of the ability of the code to converge a model with a very strange electron density. The electrons are mainly contributed by heavy elements, and the gas is only slightly ionized.

Ionization of elements Fe, Mg, Si strongly affected by charge transfer with other heavy elements.

Checks:
- Electron density is correct.
- Hydrogen line spectrum strongly pumped by continuum.

limit_h_induc.in constant temper black body limit from Ferland and Rees 1988

This example tests whether induced processes force level populations of hydrogen to LTE when they are irradiated by a blackbody in strict thermodynamic equilibrium. The density is low enough value for radiation to dominate the rate equations coupling levels with each other and the continuum. The expectation is for all departure coefficients to equal unity.

Checks:
- Departure coefficients exactly unity.
- Grain temperatures are exactly 5*104 K.

limit_hi_ion.in very high ionization parameter limit

This tests a limit of very high ionization

limit_laser_1.in test of H ionization in optically thin limit

This checks the calculation of the hydrogen photoionization equilibrium. The continuum is a laser peaked at 1.5 Ryd, where the hydrogen photoionization cross section is 2.09*10-18 cm-2.

Checks:
- The hydrogen neutral fraction is nearly 2.00*10-4 (not exact since laser has finite width).
- Hb emissivity close to high density case A. The predicted TOTL 4861 intensity should be nearly 2.2 times the expected case B intensity.

H cross section is 2.09E-18 cm^2, rec coef is 4.18E-14 answer is neutral fraction 2.00E-4 also checks that only 3 iterations needed

limit_laser_2.in test of H and HeI ionization in optically thin limit

This checks the calculation of the hydrogen and helium photoionization equilibrium. The continuum is a laser peaked at 2.0 Ryd, and so can only ionize hydrogen and atomic helium.

Checks:
- The hydrogen neutral fraction is nearly Ho/H+=4.51*10-4 (not exact since laser has finite width).
- Hb emissivity close to high density case A. The predicted TOTL 4861 intensity should be nearly 2.2 times the expected case B intensity.
- Helium ionization should be Heo/He+ = 6.61*10-4.

H cross section is 0.927E-18 cm^2, rec coef is 4.18E-13 answer is Ho/H+ = 4.51e-4 HeI cross section is 6.54E-18 cm^2, rec coef is 4.32E-13 answer is Heo/He+ = 6.61e-5

limit_laser_200.in ionization in Auger-dominated limit

This checks the calculation of ionization equilibrium. The continuum is a laser peaked at 200 Ryd. It asserts ionization of C, O, and Fe. their ionization is dominated by the Auger effect.

Checks: Auger OK

limit_laser_200_low.in test ionization in Auger-dominated limit

This checks the calculation of ionization equilibrium. The continuum is a laser peaked at 200 Ryd. It asserts ionization of C, O, and Fe. their ionization is dominated by the Auger effect.

Checks: Auger OK

limit_laser_3.in test H and He ionization in optically thin limit

This checks the calculation of the hydrogen and helium photoionization equilibrium. The continuum is a laser peaked at 4.3 Ryd, where it can fully ionize both hydrogen and helium.

Checks:
- The hydrogen neutral fraction is nearly 4.18*10-4 (not exact since laser has finite width).
- Helium ion: The ratio He+/He++ should be 1.69*10-3 and the ratio Heo/He+ should be 2.86*10-4.
- Hb emissivity should be close to high-density case A. The predicted TOTL 4861 intensity should be nearly 2.2 times the expected case B intensity.

H cross section is 1.0E-18 cm^2, rec coef is 4.18E-13 answer is n(Ho)/n(H+)=4.18e-3 HeI cross section is 1.51E-18 cm^2, rec coef is 4.32e-13 answer is n(Heo)/n(He+)=2.86e-4, so Heo/He = 4.83e-7 HeII cross section is 1.30E-18 cm^2, rec coef is 2.20e-12 answer is n(He+)/n(He2+)=1.69e-3

limit_lowd0.in test low density limit

this test case is paired with lowdm6.in both tests read in the same set of asserts, those contained in the file lowd.dat, and they should get exactly the same answer

this is also the test of the print lines intensity command

limit_lowden.in test optically thin model that extends to very low densities

This model is optically thin, with density falling off as inverse square law, so ionization and temperature should be nearly constant. if outer radius increased by 2 dex problem with level3 will appear, several li seq lines (OVI, NeVIII) will fluctuate when density about 1e-9

We do not assert H lines since the cloud is optically thin and takes at least three iterations to converge optical depth scale, That is not the purpose of this sim

limit_lowdm6.in test low density limit

this test case is paired with lowd0.in both tests read in the same set of asserts, those contained in the file lowd.dat, and they should get exactly the same answer

this also tests the print line sort range command

limit_lowion_low.in test conditions of very low ionization matrix/simple solver

The lowion_pops.in and limit_lowion_low.in models form a pair that have identical boundary conditions but use the two different hydrogenic level populations solvers. The results should agree. lowion_pops.in uses the full solution with the associate matrix inversion. This can fail under conditions of extreme low ionization due to numerical instabilities and roundoff. The solver used in limit_lowion_low.in is much simpler and will work for any conditions.

The model is almost totally molecular.

limit_lowion_pops.in test conditions of very low ionization matrix/simple solver

The limit_lowion_pops.in and lowion_low.in models form a pair that have identical boundary conditions but use the two different hydrogenic level populations solvers. The results should agree. limit_lowion_pops.in uses the full solution with the associate matrix inversion. This can fail under conditions of extreme low ionization due to numerical instabilities and roundoff. The solver used in lowion_low.in is much simpler and will work for any conditions.

The model is almost totally molecular.

limit_lte_h_t50_cion.in collisionally ionized H in LTE limit

This is the limiting case pure hydrogen collisional ionization, There are no excitation or l-mixing collisions, so this tests whether collisional ionization - three body recombination works in detailed balance.

limit_lte_h_t50_coll.in collisionally excited H in LTE limit

This checks that the model H atom goes to LTE at high densities.

chng 06 aug 24, had not included collisional ionization, and so he-like departure coefficients were very large, around 202. comments said there were problems. turned on collisional ionization, no problems noted

chng 06 jul 22 with RP changes in high-n n-changing collisions the rates are now much smaller - needed to change density to be far higher and several quantities changed. at lower density (1e18 cm-3) the populations are very unphysical and runaway maser now occurs. this is only a homework problem and intended to only test n-changing collisions. with higher density this test is done.

limit_lte_he1_coll.in He atom at high densities

test whether he-like ion populations go to lte in high density limit. The level populations should be in LTE, and the departure coefficients should be unity.

limit_lte_he1_ste.in He atom in LTE at high densities

test whether a gas dominated by He goes to LTE in high-density limit. The level populations should be in LTE, the departure coefficients should be unity, and the temperature equal to the BB temp.

limit_lte_hhe_coll_t50.in H, He in LTE at high densities

This model is a test of the behavior of hydrogen and helium in the high density, collision dominated, limit. The temperature is preset, the hydrogen density is set to a very high value, and the ionization parameter is very low. The resulting model is collision dominated, so this case checks that the collision physics occurs in detailed balance. The predicted departure coefficients should all equal unity. The set dr command sets the zone thickness to 1 cm.

Checks:
- Hydrogen departure coefficients exactly unity.
- Helium departure coefficients near unity. (Density not high enough to bring helium departure coefficients exactly to unity.)
- H-, H2, H2+ H3+, and HeH+ departure coefficients exactly unity. `

limit_lte_hhe_induc.in radiation dominated H, He gas goes to STE

This is a H, He-only gas that is optically thin in the Lyman continuum. It is irradiated by a blackbody in strict thermodynamic equilibrium. The tests confirm that the gas temperature equilibriates close to the black body temperature.

limit_lte_hhe_ste.in H, He in STE

This is the ultimate test of the behavior of the code in the strict thermodynamic equilibrium limit. The temperature is not held constant, so the resulting equilibrium temperature determines whether cooling processes are treated properly in the detailed balance limit. The equilibrium temperature should be exactly 5*104 K, and all departure coefficients should equal unity. A small amount of grains are included to check that the grain thermal balance is handled properly in this limit.

Checks:
- Electron temperature exactly 5*104 K.
- Departure coefficients unity.

limit_lte_hminus.in H- goes to LTE

This checks that the negative hydrogen ion goes to thermodynamic equilibrium when irradiated by a blackbody in thermodynamic equlibrium. It was originally presented in >>refer H- test Ferland, G. J., & Persson, S. E. 1989, ApJ, 347, 656

limit_lte_metal.in STE with metals

This checks that the code goes to strict thermodynamic equilibrium for the case of a metal rich gas exposed to a true black body. The many heavy element lines should dominate cooling, so this is a test that the multilevel atoms go to LTE in the radiation-dominated limit.

Checks:
- Temperature should equilibrate at 20000 K.
- Departure coefficients should equal unity.

limit_recoil_ion.in test compton recoil ionization of hydrogen

H ionization is totally due to recoil ionization in this model. The assert checks the final hydrogen ionization.

limit_strom.in pure-H Stromgren sphere

This case checks that the code computes the geometry and emissivity correctly for a pure hydrogen spherical shell. The low temperature is chosen to avoid collisional ionization. The model stops at the Ho-H+ ionization front. The turbulence is to prevent the Balmer lines from becoming optically thick.
Checks
- Outer radius should be 4.16391017 cm.
- Predicted Hb, case B Hb, and Q(H) Hb, all agree.

limit_supra.in secondary ionization dominated gas

This model computes the ionization within cool gas that is totally ionized by suprathermal secondary electrons.

Charge transfer heating is VERY important in this simulation.

limit_vbhum.in compare with Van Blerkom and Hummer exact RT results

This is a test of the treatment of the diffuse fields, their transfer, and their effects on the ionization structure of a nebula. The comparison is made against the exact calculation published by Van Blerkom and Hummer (1967). The geometry is open, that is, similar to that assumed in most BLR calculations.

>>refer H ionization Van Blerkom, D., & Hummer, D. G. 1967, MNRAS, 137, 353

The diffuse ots command is entered in order to reproduce the Van Blerkom and Hummer results. The default assumption, outward only, does not agree as well. I changed the default from OTS to outward only to be in better agreement with predictions by Harrington and Rubin at the Lexington meeting. They have not checked whether their codes are in agreement with the Van Blerkom and Hummer paper.

Checks:
- Neutral fraction at illuminated face 5.8*10-4.
- Location of ionization front at 7.8*1016 cm.
- 34TOTL 486134 and 34CA B 486134 agree; both slightly lower than 34Q(H) 486134.
- Answers with OTS agree with 1967 results.

test hydrogen ground state rec effic against vb+h exact results this is their case e) - "zero condition" their answer for H0/Htot at the illuminated edge is approx 5.8E-4, and a Stromgren radius of approximately 7.7E16 cm

limit_veryveryfast.in very fast simulation for Purify/valgrind

This is meant to be a very fast calculation to use when running extensive debug-enabled runtimes.

nlr_lex00.in NLR model for Lexington 2000 Meeting

This is one of the test cases from the Lexington (1993) Meeting suite of nebulae. It is a grain-free NLR model.

nlr_liner.in NLR liner model

This is a model somewhat like the Liner parameters proposed by Ferland and Netzer (1983). A second iteration is performed to allow the calculation of the line radiation pressure.

>>refer nlr_liner model Ferland, G. J., & Netzer, H. 1983, ApJ, 264, 105

nlr_liner_grains.in liner model with grains

This is a model somewhat like the Liner parameters proposed by Ferland and Netzer (1983). A second iteration is performed to allow the calculation of the line radiation pressure. It includes grains and is so more realistic.

>>refer liner model Ferland, G. J., & Netzer, H. 1983, ApJ, 264, 105

nlr_paris.in Paris meeting NLR model

This is the NLR model presented in the Meudon meeting on model nebulae. The init file is entered to make the code behave more like version 84.

Checks:
- init file works

nova_dqher.in cold nova shell

This tests the code39s behavior in the limit posed by the metal rich low density nebula surrounding DQ Her (Ferland et al. 1984).
Checks:
- Thickness exact
- Thermal stability High-Z gas ionization at low temperature

nova_photos.in dense nova photosphere

this model is intensely affected by continuum pumping of atoms. The hydrogen ionizaiton is by lyman line pumping, followed by photoionization from excited states.

optimize_phymir.in test phymir optimizers

This checks whether the optimizer can recover a known solution. The line spectrum was calculated at T = 1e4 K and and n_H=1e5 cm^-3, and resulted in the given electron density. The model optimize_subplex.in is a copy of this file.

optimize_subplex.in test subplex optimizer

This checks whether the optimizer can recover a known solution. The line spectrum was calculated at T = 1e4 K and and n_H=1e5 cm^-3, and resulted in the given electron density. The model optimize_phymir.in is a copy of this file.

orion_hii_open.in conditions similar to Orion nebula blister

This is a model similar in spirit to the blister geometry HII region model computed by Baldwin et al. (1991). Size-resolved Orion grains are included. The constant pressure command does a hydrostatic equilibrium structure. The predicted emission-line spectrum is affected by the reddening of the internal grains. The resulting t2 analysis produces artificial results as a result. This has an open geometry, the original BFM paper was a closed geometry. (This makes little difference). Background cosmic rays are also included although these should have little effect on warm ionized gas. The emission line spectrum is given in surface brightness units, as in the BFM paper.

orion_hii_pdr.in constant pressure H+ region/pdr

This extends BFM from the H+ region into the PDR as in Abel et al 2005. This is the correct way to do a PDR calcualtion.

>>refer Orion model Baldwin, J., Ferland, G. J., >>refercon Martin, P. G., Corbin, M., Cota, S., Peterson, >>refercon B. M., & Slettebak, A. 1991, ApJ, 374, 580

>>refer physics HII/PDR Abel, N.P., Ferland, G.J., Shaw, G. & >>refercon van Hoof, P.A.M. 2005, ApJS, 161, 65

orion_hii_pdr_fast.in constant gas pressure H+ region/PDR

Orion HII region and PDR, simialr to orion_hii_pdr but much faster because of fast.ini

orion_hii_pdr_pp.in the Orion HII Region / PDR / Molecular cloud with an open geometry

similar to orion_hii_pdr except for plane parallel geometry

pdr_co_fully.in H2 and CO in fully molecular limit

test code in fully molecular limit this is a pair with pdr_co_fully_noneq - that tests non equilibrium chem

pdr_co_fully_noneq.in H2 and CO are fully molecular, non-equilibrium case

test code in fully molecular limit with Federman non-equilibrium chem this is a pair with pdr_co_fully.in, which does not include non-equil chem

pdr_coolbb.in illumination by cool STE blackbody