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
title check rate H2 forms on grain surfaces
c
c commands controlling continuum =========
c first continuum is FIR hot grain continuum produced in
c unmodeled HII Region
blackbody, t = 75 K
intensity 2.7 (total)
c this is hot star continuum
black 30000
intensity 1.90 range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
cosmic rays, background
c
c commands for density & abundances =========
hden 0
grains ism, abundance log 0.16 no qheat
init file="ism.ini"
abundances he -1.01 c -3.52 n-8 o-3.30 ne-8 mg-5.89
continue si -6.10 s -5.10 cl=-7 ar-8 fe -6.60
c
c commands controlling geometry =========
sphere
c stop when gas is fully neutral
stop efrac -10
c stop when gas is cold
stop temperature 10 linear
stop zone 1
c
c other commands for details =========
c set the gas temperature
constant temperature 100 K
case b
c
c commands controlling output =========
normalize to "C 2" 157.6m
c uv lines are strongly pumped by stellar continuum, break out contribution
print line pump
print line optical depths
print ages
punch hydrogen 21 cm last "ism_jura.21cm"
c
c ism_jura.in
c class limit
c ========================================
c
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
title generate standard ISM opacity curve
c
c commands controlling continuum =========
table agn
ionization parameter -3
c
c commands for density & abundances =========
grains no qheat
c
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
iterate
c
c commands controlling output =========
punch total opacity last "ism_opacity.opc" units kev
c
c ism_opacity.in
c class limit
c ========================================
c
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
title background cosmic ray ionization by suprathermal electrons only
c
c commands controlling continuum =========
cosmic ray rate -16
c this will be VERY faint black 50000
ionization parameter -25
black 50000
c
c commands for density & abundances =========
hden 5
element hydrogen ionization 1 0.00000001
c
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
constant temperature 1000 K
c turn off molecules to test only ions
no molecules
c must turn off charge transfer and its heating, which would dominate,
c since we want to test cr heating and ionization
no charge transfer
no ctheat
c must turn of photoionization by recombining species,
c since we want to test cr heating and ionization
no photoionization
c any time photoionization is turned off, it is best to also
c turn off induced processes, which include pumping in the lyman lines
no induced processes
c
c commands controlling output =========
print ages
c
c ism_set_cr_rate.in
c class limit
c ========================================
c
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
title case A
c
c Seaton, M.J, 1959 MN 119, 90,
c 4pi j(beta) 5.56E-26
c for this model total H-beta=4.745
c b(2)=3.73E-3 (3)=3.69E-2 (4)=0.091 (5)=0.145 (6)=0.193
c n.b. very different results if not l-mixed
c
c commands controlling continuum =========
black body, T = 50000 K
ionization parameter -2
c
c commands for density & abundances =========
hden = 13;
init file="honly.ini"
c
c commands controlling geometry =========
stop lyman optical depth -6
stop zone 1
set dr 0
c
c other commands for details =========
no induced processes (OK) ;N.B. case A is a fiction; no incuded transitions
atom h-like collisions off ; must turn off all collisions
constant temperature = 10000 K
iterate
c
c commands controlling output =========
c this should make the predicted totl Hbeta near unity for case a
normalize to "CaBo" 4861 = 2.23
print populations h-like
print departure coefficients
c
c limit_casea_h_den13.in
c class limit
c ========================================
c
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
title Test model H in Case A limit
c grid over nebular range of density and temperature to check Case A H
c
c commands controlling continuum =========
c create H+
laser 2 Ryd
ionization parameter -2
c
c commands for density & abundances =========
init "honly.ini"
hden 2. vary
grid 2 6 2
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
no scattering escape
case A hummer no Pdest no photoionization
no induced processes
constant temperature 4. vary
grid 5,000K to 20,000K in 5,000K steps
c
c commands controlling output =========
atom H-like print levels
c
c fixit the wavelength range is adjusted to avoid the Lyman lines
c the Lyman a / 2 photon ratio is wrong at high Tempetaure -
c is there a temperature dependent branching ratio to n=2 out
c of the collapsed level?
c
c limit_casea_h_den_temp.in
c class limit
c ========================================
c
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"
title "Case B from Hummer and Storey"
init "honly.ini"
laser 1.1
ionization parameter -1
constant temperature 4
case b hummer no photoionization no pdest
atom h-like element hydrogen levels resolved 30
no induced processes
no level2
no scattering escape
set dr -20
hden 4
stop zone 1
iterate
print populaions h-like
print departure h-like
c
c
c limit_caseb_h_hs87.in
c class limit
limit_caseb_h_lot.in log density case B, T=500 log n=2
title log density case B, T=500 log n=2
c
c commands controlling continuum =========
black body, T = 2.e5 K
ionization parameter -1
c
c commands for density & abundances =========
hden = 2
init file="honly.ini"
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
constant temperature = 500
c want H and he fully stripped so we can check H He spectra
case b hummer no photoionization no pdest
no induced processes (OK)
iterate
c
c commands controlling output =========
print diffuse continua
normalize to "Ca B" 4861
c
c does not agree with Hummer & Storey, as explained by Ferguson & Ferland
c until 03 jun 02, used small atom, which had smaller differences
c turn on large atom to get best answer
atom h-like levels resolved 20
c
punch results "limit_caseb_h_lot.rlt" last
c
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
title h_caseb_n8 high density case B
c
c commands controlling continuum =========
black body, T = 2.e5 K
ionization parameter -1
c
c commands for density & abundances =========
hden = 8
init file="honly.ini"
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
c this will not affect the main model, but will test CR heating rate
cosmic ray background
case b hummer no photoionization no Pdest
no scattering escape
no induced processes (OK)
constant temperature = 20000
iterate
c
c commands controlling output =========
normalize to "Ca B" 4861
punch results "limit_caseb_h_n8.rlt"
punch ionizing continuum "limit_caseb_h_n8.cion"
c
c
c limit_caseb_h_n8.in
c class limit
c ========================================
c
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
title limit_caseb_he2_den8 He II case B
c
c commands controlling continuum =========
table agn
ionization parameter 0
c
c commands for density & abundances =========
hden = 8
element helium abundance 1
init file="ism.ini"
c
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
atom h-like element helium levels resolved 15
case b hummer no photoionization no Pdest
no induced processes (OK)
constant temperature = 50,000K
c
c commands controlling output =========
punch results "limit_caseb_he2_den8.rlt"
c
c
c limit_caseb_he2_den8.in
c class limit
c ========================================
c
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
title Test model H and He atoms in Case B limit
c grid over nebular range of density and temperature to check Case B H & He
c
c commands controlling continuum =========
laser 5 Ryd
ionization parameter -2
c
c commands for density & abundances =========
init "hheonly.ini"
hden 2. vary
grid 2 6 2
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
normalize to "He 2" 4686
case b hummer no Pdest no photoionization
no scattering escape
c prevent H I excited levels from being predicted
atom H-like element hydrogen levels 3
constant temperature 4.
c
c commands controlling output =========
atom H-like print levels
c
c
c limit_caseb_he_den.in
c class limit
c ========================================
c
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
title the best we can do to predict the HeI emission spectrum
c
c commands controlling continuum =========
laser 2
ionization -1
c
c commands for density & abundances =========
hden 9000 linear
set eden 4
element helium abundance -1
init file "hheonly.ini"
c
c commands controlling geometry =========
stop zone 1
set dr -6.95424
c
c other commands for details =========
atom he-like levels 30
atom he-like collapsed levels 70
atom he-like gbar vriens
constant temper 4
case b no photoionzation no pdest
iterate
c
c commands controlling output =========
normalise to "He 1" 4471
print departure he-like helium
print line faint 0.01
c punch fits last "limit_caseb_he_den4_temp4.fit"
punch diffuse continuum "limit_caseb_he_den4_temp4.dif" last no title units microns
punch continuum "limit_caseb_he_den4_temp4.con" last no title units microns
c
c
c limit_caseb_he_den4_temp4.in
c class limit
c ========================================
c
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
title Test model He atoms in Case B limit
c grid over nebular range of density and temperature to check Case B H & He
c
c commands controlling continuum =========
laser 5 Ryd
ionization parameter -2
c
c commands for density & abundances =========
init "hheonly.ini"
hden 2. vary
grid 2 6 2
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
normalize to "He 2" 4686
case b hummer no Pdest no photoionization
no scattering escape
c prevent H I excited levels from being predicted
atom H-like element hydrogen levels 3
constant temperature 4. vary
grid 5,000K to 20,000K in 5,000K steps
c
c commands controlling output =========
atom H-like print levels
c
c
c limit_caseb_he_den_temp.in
c class limit
c ========================================
c
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
title Test model H and He atoms in Case B limit
c grid over nebular range of density and temperature to check Case B H & He
c
c commands controlling continuum =========
c create H+ and He+
laser 2.0 Ryd
ionization parameter -2
c
c commands for density & abundances =========
init "hheonly.ini"
hden 2. vary
grid 2 6 2
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
no scattering escape
case b hummer no Pdest no photoionization
constant temperature 4.
c
c commands controlling output =========
atom H-like print levels
c
c
c limit_caseb_hhe_den.in
c class limit
c ========================================
c
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
title Test model H and He atoms in Case B limit
c grid over nebular range of density and temperature to check Case B H & He
c
c commands controlling continuum =========
c create H+ and He+
laser 2 Ryd
ionization parameter -2
c
c commands for density & abundances =========
init "hheonly.ini"
hden 2. vary
grid 2 6 2
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
no scattering escape
case b hummer no Pdest no photoionization
constant temperature 4. vary
grid 5,000K to 20,000K in 5,000K steps
c
c commands controlling output =========
atom H-like print levels
c
c
c limit_caseb_hhe_den_temp.in
c class limit
c ========================================
c
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
title H only optically thin in Lyman continuum
c
c commands controlling continuum =========
blackbody 40000
ionization -2
c
c commands controlling geometry =========
stop thickness 16
c
c commands for density & abundances =========
hden 2
init file "honly.ini"
c
c other commands for details =========
iterate
constant temper 10000
no level2
c
c commands controlling output =========
print diffuse continuum
print line inward
normalize to "Ca B" 4861 = 1 % normalize to exact result
punch overview "limit_casec_h-den2.ovr" last
punch fine optical depths last "limit_casec_h-den2.fin" range 0.9 1.02 every 1
punch optical depths last "limit_casec_h-den2.opt"
punch continuum "limit_casec_h-den2.con" last units microns
punch dr "limit_casec_h-den2.dr" last
c
c limit_casec_h-den2.in
c class limit
c ========================================
c
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
title case C
c
c commands controlling continuum =========
black body, T = 50000 K
ionization parameter -2
c
c commands for density & abundances =========
hden = 5
init file="hheonly.ini"
c
c commands controlling geometry =========
set dr -10
stop zone 1
c
c other commands for details =========
iterate
stop lyman optical depth -6
constant temperature = 10000 K
c
c commands controlling output =========
normalize to "Ca B" 4861
print h-like populations
print departure coefficients
c
c limit_casec_h_den5.in
c class limit
c ========================================
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
title test high-T Compton energy exchange
c
c commands controlling continuum =========
c as hot as STE bb can be on IEEE 32-bit cpu
c equilibrium temperature should also be 2.51e7
c since gas radiated by true blackbody will equilibriate
c at its temperature
blackbody 7.4 STE
c
c commands for density & abundances =========
hden 10
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
atom h-like element oxygen levels 5
atom h-like element oxygen levels collapsed 30
set temperature convergence 0.0001
iterate
print h-like departure element oxygen
c
c commands controlling output =========
c
c limit_compton_hi_t.in
c class limit
c ========================================
c
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
title test low-T Compton energy exchange
c
c commands controlling continuum =========
black linear 3 lte
brems 5
ionizat -5
c
c commands for density & abundances =========
hden -10
init file "hheonly.ini"
eden 0
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
set temperature convergence 0.0001
iterate 3
c
c commands controlling output =========
c
c limit_compton_lo_t.in
c class limit
c ========================================
c
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
title mid-T Compton energy exchange
c test of thermal equil in limit_compton_mid_t limit; temp should EXACTLY equal 2E5K
c check continuum partition;
c energy range, photon densities, luminosities, follow
c 0.25-1. Q=26.6470 L=15.8190 c 1-1.807 Q=26.8867 L=16.3766
c 1.807-4 Q=27.3042 L=17.0948 c 4-20 Q=27.2041 L=17.3179
c 20 -- Q=22.9038 L=22.9038 c total lumin 17.5597
c nufnu(912A) = 1.8029E+16
c
c commands controlling continuum =========
black body t = 2.e5 K lte
c
c commands for density & abundances =========
hden = 6
init file "hheonly.ini"
c
c commands controlling geometry =========
stop zone 1
stop lyman continuum optical depth = -6
set dr 0
c
c other commands for details =========
set temperature convergence .0001 % decrease error on heat-cool match
c
c commands controlling output =========
print line faint .1
print departure coef
c
c limit_compton_mid_t.in
c class limit
c ========================================
c
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
title test that energy is limit_conserved
* trace temperature convergence 0 2
c
c commands controlling continuum =========
c primary continuum is a hot blackbody
black body, temp=5.5
intensity total -4
c add cosmic background
backbround
c
c commands controlling geometry =========
c don't stop the calculation until all energy used up
c in order to check energy conservation
stop temperature 3 linear
c cloud will go very deep with temperature near 3K without this
stop thickness 20
c
c commands for density & abundances =========
no molecules
metals -0.5
hden 1.0
constant pressure
c
c other commands for details =========
iterate
c want a clean calculation
failures 3
c this allows for more molecular gas beyond what we model
double optical depths
c must increase number of levels since so optically thick
atom co levels 30
c
c commands controlling output =========
punch pressure "limit_conserve.pre"
punch pressure history "limit_conserve.his"
punch cooling "limit_conserve.col"
punch heating "limit_conserve.het"
punch dr "limit_conserve.dr"
punch overview "limit_conserve.ovr1"
punch overview last "limit_conserve.ovr"
punch results "limit_conserve.rlt"
punch element carbon "limit_conserve.car"
punch element neon "limit_conserve.ne"
punch element magnesium "limit_conserve.mag"
punch element silicon "limit_conserve.sil"
punch molecules "limit_conserve.mol"
c
c limit_conserve.in
c class hii pdr
c ========================================
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
title Martin Gaskell's funny model
c used to test that electron density convergence is ok
c hydrogen line spectrum strongly pumped by continuum
c all elements > H have HIGH abundances
c ionization of elements Fe, Mg, Si strongly affected
c by charge transfer
c
c commands controlling continuum =========
black 4000
lumin 27.2
c
c commands for density & abundances =========
hden 5.138
abundances all 1000
c
c commands controlling geometry =========
radius 15
stop zone 1
set dr 0
c
c other commands for details =========
constant temper 5500
c
c commands controlling output =========
print line faint -3
c
c limit_eden.in
c class limit
c ========================================
c
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
title constant temper black body limit from Ferland and Rees 1988
c tests whether departure coef are forced to unity by induced processes
c
c commands controlling continuum =========
black body, t = 50000 lte
c
c commands for density & abundances =========
hden 10
init file="hheonly.ini"
c
c commands controlling geometry =========
stop lyman continuum optical depth -6
set dr -10
stop zone 1
c
c other commands for details =========
iterate
constant temper 50000
c
c commands controlling output =========
print populations h-like
print heating
print departure coef
print line faint -1
c
c limit_h_induc.in
c class limit
c ========================================
c
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
title very high ionization parameter limit
c commands controlling continuum =========
table agn
ionization parameter 15
c commands controlling geometry =========
hden 0
stop zone 1
c other commands for details =========
iterate
c
c commands controlling output =========
punch heating "limit_hi_ion.het"
punch cooling "limit_hi_ion.col"
c
c
c func_hi_ion.in
c class function
c ========================================
c
This tests a limit of very high ionization
limit_laser_1.in test of H ionization in optically thin limit
title test of H ionization in optically thin limit
c
c commands controlling continuum =========
laser 1.5 Ryd
phi(h) 10
c
c commands for density & abundances =========
hden 1
init file="hheonly.ini"
c
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
constant temperature = 4
iterate to convergence
c
c commands controlling output =========
c
c limit_laser_1.in
c class limit
c ========================================
c
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
title test of H and HeI ionization in optically thin limit
c
c commands controlling continuum =========
laser 2.0 Ryd
intensity -0.3604
c
c commands for density & abundances =========
hden 1
init file="hheonly.ini"
abundances all -10
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
constant temperature = 4
iterate to convergence
c
c commands controlling output =========
c
c limit_laser_2.in
c class limit
c ========================================
c
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
title ionization in Auger-dominated limit
c
c commands controlling continuum =========
laser 200 Ryd
phi(h) 10
c
c commands for density & abundances =========
hden 1
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
iterate to convergence
constant temperature = 5
c
c commands controlling output =========
c
c limit_laser_200.in
c class limit
c ========================================
c
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
title test ionization in Auger-dominated limit
c
c commands controlling continuum =========
laser 200 Ryd
phi(h) 5
c
c commands for density & abundances =========
hden 1
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
iterate to convergence
constant temperature = 4
c
c commands controlling output =========
c
c
c
c
c
c limit_laser_200_low.in
c class limit
c ========================================
c
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
title test H and He ionization in optically thin limit
c
c commands controlling continuum =========
laser 4.3 Ryd
phi(h) 10
c
c commands for density & abundances =========
hden 1
abundances all -10
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
iterate to convergence
constant temperature = 4
c
c commands controlling output =========
c
c limit_laser_3.in
c class limit
c ========================================
c
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
title test low density limit
c this and limit_lowdm6 should get same results
c
c commands controlling continuum =========
table agn
ionization parameter -2
c
c commands for density & abundances =========
hden 0
abundances old solar 84
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
iterate
c
c commands controlling output =========
normalize to "H 1" 4861 0.86
print line sort wavelength range 100 1m
punch cooling last "limit_lowd0.col"
punch continuum last "limit_lowd0.con"
c
c all asserts for both sims are in this file
init file="lowd.dat"
c
c limit_lowd0.in
c class limit
c ========================================
c
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
title test optically thin model that extends to very low densities
c
c commands controlling continuum =========
table agn
ionization parameter 0
c
c commands for density & abundances =========
hden -2 to the -2 power
init file="ism.ini"
c
c commands controlling geometry =========
sphere
c this will take density down to 1e-8, below stated limit
radius 10 13
c
c other commands for details =========
c
c commands controlling output =========
punch overview "limit_lowden.ovr" last
c
c limit_lowden.in
c class limit
c ========================================
c
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
title test low density limit
c this and limit_lowd0 should get same results
c
c commands controlling continuum =========
table agn
ionization parameter -2
c
c commands for density & abundances =========
hden -6
abundances old solar 84
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
iterate
c
c commands controlling output =========
normalize to "H 1" 4861 0.86
print line sort wavelength range 100 1m
punch cooling last "limit_lowdm6.col"
punch continuum last "limit_lowdm6.con"
c
c all asserts are in this file
init file="lowd.dat"
c
c limit_lowdm6.in
c class limit
c ========================================
c
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
title test conditions of very low ionization matrix/simple solver
c
c commands controlling continuum =========
blackbody 50000
ionization parameter -30
c
c commands for density & abundances =========
hden 2
init file "hheonly.ini"
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
atom h-like matrix lowt
atom he-like matrix lowt
no molecules
constant temperature 100
c
c commands controlling output =========
c
c limit_lowion_low.in
c class limit
c ========================================
c
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
title test conditions of very low ionization matrix/simple solver
c
c commands controlling continuum =========
blackbody 50000
ionization parameter -30
c
c commands for density & abundances =========
hden 2
init file "hheonly.ini"
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
atom h-like matrix pops
atom he-like matrix pops
no molecules
constant temperature 100
c
c commands controlling output =========
c
c
c limit_lowion_pops.in
c class limit
c ========================================
c
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
title collisionally ionized H in LTE limit
c
c commands controlling continuum =========
black body, T = 50000 K
ionization parameter -8
c
c commands for density & abundances =========
hden = 20
set eden 20
init file="hheonly.ini"
c
c commands controlling geometry =========
stop lyman optical depth -6
set dr -10
stop zone 1
c
c other commands for details =========
constant temperature = 50000 K
c want pure collisional model
no induced processes (OK)
atom h-like collisional excitation off
atom h-like collisions l-mixing off
atom he-like collisional excitation off
atom he-like collisions l-mixing off
atom he-like collapsed levels 20
iterate
c
c commands controlling output =========
print h-like departure coefficients
print he-like departure coefficients
print populations h-like
print departure coefficients
c
c limit_lte_h_t50_cion.in
c class limit
c ========================================
c
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
title collisionally excited H in LTE limit
c
c commands controlling continuum =========
black body, T = 50000 K
ionization parameter -8
c
c commands for density & abundances =========
hden = 20
init file="hheonly.ini"
c
c commands controlling geometry =========
stop lyman optical depth -6
stop zone 1
set dr 0
set eden 20
c
c other commands for details =========
no induced processes (OK)
atom h-like collisions l-mixing off
atom he-like collapsed levels 20
atom he-like collisions l-mixing off
constant temperature = 50000 K
iterate
c
c commands controlling output =========
print h-like departure coefficients
print h-like populations
print he-like departure coefficients
print populations h-like
c
c limit_lte_h_t50_coll.in
c class limit
c ========================================
c
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
title He atom at high densities
c
c commands controlling continuum =========
laser 2
ionization -3
c
c commands for density & abundances =========
hden 18
set eden 18
element helium abundance -1
init file "hheonly.ini"
c
c commands controlling geometry =========
stop zone 1
set dr -10
c
c other commands for details =========
atom he-like levels 10
atom he-like collapsed levels 20
constant temper 20000 K
iterate
c
c commands controlling output =========
print he-like departure helium
normalise to "He 1" 4471
print line faint -2
c
c limit_lte_he1_coll.in
c class limit
c ========================================
c
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
title He atom in LTE at high densities
c
c commands controlling continuum =========
blackbody 50000 STE
c
c commands for density & abundances =========
hden 18
* set eden 18
c a high he abundance so that it dominates
element helium abundance 1
init file "hheonly.ini"
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
atom he-like levels 7
atom he-like collapsed levels 30
iterate
c
c commands controlling output =========
print he-like departure helium
print h-like departure hydrogen
normalise to "He 1" 4471
print line faint -2
punch heating "limit_lte_he1_ste.het"
punch cooling "limit_lte_he1_ste.col"
punch dr "limit_lte_he1_ste.dr"
c
c limit_lte_he1_ste.in
c class limit
c ========================================
c
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
title H, He in LTE at high densities
c test from Ferland and Rees 88, collisions drive H to LTE
c collisions should drive all departure coef to unity
c
c commands controlling continuum =========
black body t = 50000
ionization parameter -5
c
c commands for density & abundances =========
hden = 19
init file="hheonly.ini"
set eden 20
c
c commands controlling geometry =========
set dr -10
stop zone 1
stop lyman optical depth -6
c
c other commands for details =========
constant temperature = 50000
iterate
c
c commands controlling output =========
print departure coefficients h-like
print populations h-like
print departure coefficients h-like helium
print populations h-like helium
print departure coefficients he-like
print populations he-like
punch dr "limit_lte_hhe_coll_t50.dr" last
c
c limit_lte_hhe_coll_t50.in
c class limit
c ========================================
c
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
title radiation dominated H, He gas goes to STE
c
c commands controlling continuum =========
black body, t = 50000 STE
c
c commands for density & abundances =========
hden 4
init file="hheonly.ini"
c
c commands controlling geometry =========
stop lyman continuum optical depth -6
set dr -10
stop zone 1
c
c other commands for details =========
iterate
set temperature convergence 0.002
c
c commands controlling output =========
print populations h-like
print heating
print departure coef
print line faint -1
c
c limit_lte_hhe_induc.in
c class limit
c ========================================
c
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
title H, He in STE
c from Ferland and Rees 1988
c this tests whether thermal processes go to STE
c
c commands controlling continuum =========
black body, t = 50000 STE
c
c commands for density & abundances =========
hden 10
init file="hheonly.ini"
c
c commands controlling geometry =========
stop lyman optical depth -6
set dr -10
stop zone 1
c
c other commands for details =========
iterate
c
c commands controlling output =========
print heating
print populations h-like
print departure coef h-like
print departure coef he-like
c
c limit_lte_hhe_ste.in
c class limit
c ========================================
c
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
title H- goes to LTE
c
c commands controlling continuum =========
c this is a second way to get STE and tests the energy density option
blackbody 5000 energy density 5000K
c
c commands for density & abundances =========
hden 10
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
iterate
constant temperature 5000
c
c commands controlling output =========
print populations h-like hydrogen
print departure coef
c
c limit_lte_hminusin
c
c class limit
c ========================================
c
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
title STE with metals
c this tests whether thermal processes go to STE
c
c commands controlling continuum =========
c a dilution factor of 1 is one way to get STE
black body, t = 20000 dilution 1
c
c commands for density & abundances =========
hden 10
abundances starburst 5
c
c commands controlling geometry =========
stop zone 1
stop lyman optical depth -6
set dr -10
c
c other commands for details =========
iterate
c
c commands controlling output =========
print departure coef
print populations h-like
punch heating "limit_lte_metal.het" last
punch cooling "limit_lte_metal.col" last
c
c limit_lte_metal.in
c class limit
c ========================================
c
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
title test compton recoil ionization of hydrogen
c
c commands controlling continuum =========
laser 2000 ryd
ionization parameter -5
c
c commands for density & abundances =========
hden 0
init "honly.ini"
c
c commands controlling geometry =========
set dr 14
stop zone 10
c
c other commands for details =========
iterate
no secondary ionization
constant temperature 1000
c
c commands controlling output =========
c
c
c limit_recoil_ion.in
c class limit
c ========================================
c
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
title pure-H Stromgren sphere
c the answer is R(Stromgren) = 4.16E17 cm
c
c commands controlling continuum =========
blackbody 50000 K
q(h) 49
c
c commands for density & abundances =========
hden 4
init file "honly.ini"
abundances all -10
c
c commands controlling geometry =========
sphere static
radius 16
stop efrac -0.5
c
c other commands for details =========
no level2
turbulence 20 km/s
constant temper 7500
iterate
c
c commands controlling output =========
punch overview last "limit_strom.ovr"
punch results last "limit_strom.rlt"
punch dr last "limit_strom.dr"
c
c limit_strom.in
c class limit
c ========================================
c
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
title secondary ionization dominated gas
c like SN envelope
c
c commands controlling continuum =========
c this continuum will be VERY faint
table agn
ionization parameter -25
c secondary ioinzations will dominate
set csupra -5
c
c commands for density & abundances =========
hden 5
abundances old solar 84
c
c commands controlling geometry =========
stop temperature 20
stop zone 1
set dr 0
c
c other commands for details =========
constant temperature 1000 K
iterate convergence
c
c commands controlling output =========
print ages
c check that no uninitialized DR rates are printed (r2757)
print arrays carbon only
punch heating "limit_supra.het"
punch ionizing continuum "limit_supra.ion" last
punch molecules "limit_supra.mol"
c
c
c limit_supra.in
c class limit
c ========================================
c
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
title compare with Van Blerkom and Hummer exact RT results
c
c commands controlling continuum =========
blackbody 50000 K
phi(h) 12.30103
c commands for density & abundances =========
hden 4
init "honly.ini"
abundances all -10
c
c commands controlling geometry =========
stop efrac -0.5
c
c other commands for details =========
diffuse ots
no level2 lines
constant temper 4
iterate
c
c commands controlling output =========
punch overview last "limit_vbhum.ovr"
punch dr last "limit_vbhum.dr"
c
c
c limit_vbhum.in
c
c class limit
c ========================================
c
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
title very fast simulation for Purify/valgrind
c
c commands controlling continuum =========
table agn
ionization parameter -2
c
no file opacity
set dr 0
c
c commands for density & abundances =========
hden 9
init file "hheonly.ini"
element oxygen on
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
no level 2
constant temperature 4
atom h-like levels very small
atom he-like levels very small
c
c commands controlling output =========
punch dr last "limit_veryveryfast.dr"
c
c
c limit_veryveryfast
c class limit
c ========================================
c
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
title NLR model for Lexington 2000 Meeting
c
c commands controlling continuum =========
phi(h) 12.47712
c shape of continuum is interpolated table
interpolate (0 -10) (0.08 -10) (0.1 1) (3676 -4.935) (4700 -11)
continue (4750 -20) (7.4e6 -30)
c
c commands controlling geometry =========
stop column 22
c
c commands for density & abundances =========
hden 4
init file="c84.ini"
abundances -1 c-3.52 n-4 o-3.097 ne-4 na-9
continue mg-4.523 al-8 si-4.523 s-4.824 a-9 ca-8 fe-8 ni-9
c
c other commands for details =========
iterate
c
c commands controlling output =========
* normalize to "totl" 4861 of 0.923
print line faint .01
print diffuse continuum
c add sum of these lines to printout for Stoy ratio
print line sum
TOTL 1216
He 1 5876
TOTL 1909
TOTL 1549
N 2 6584
N 2 6548
N 3 57.21m
totl 1750
totl 1486
o 1 6300
o 1 63.17m
TOTL 3727
totl 1665
O 3 51.80m
O 3 5007
O 3 4959
totl 1402
Ne 3 15.55m
Ne 3 3869
Ne 3 3968
Ne 4 2424
Ne 5 3426
Ne 5 3346
totl 2798
si 2 34.81m
s 2 6720
S 3 18.67m
S 3 9532
S 3 9069
S 4 10.51m
end of lines
c
punch overview last "nlr_lex00.ovr"
punch dr last "nlr_lex00.dr"
punch results last "nlr_lex00.rlt"
c
table lines "LineList_NLR.dat"
c nlr_lex00.in
c class nlr
c ========================================
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
title NLR liner model
c a constant pressure (gas+radiation) model of a nlr_liner cloud
c in the spirit of Ferland and Netzer 1983
c
c commands controlling continuum =========
table agn
ionization parameter -3
c
c commands for density & abundances =========
hden 6
init file "ism.ini"
abundances old solar 84
metals 0.3
c
c commands controlling geometry =========
stop thickness 16.3
stop column density 23
constant pressure
c
c other commands for details =========
iterate to convergence ;must iterate to get radiation pressure correctly
c
c commands controlling output =========
punch overview last "nlr_liner.ovr"
punch element nitrogen last "nlr_liner.nit"
punch dr last "nlr_liner.dr"
punch results last "nlr_liner.rlt"
c
c nlr_liner.in
c class nlr
c ========================================
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
title liner model with grains
c
c a constant pressure (gas+radiation) model of a liner cloud
c in the spirit of Ferland and Netzer 1983
c
c commands controlling continuum =========
ionization parameter -3
table agn
c
c commands for density & abundances =========
hden 6
c this turns on both grains and depleted abundances
abundances ism no grains
grains ism no qheat single
init file "ism.ini"
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
constant pressure
iterate to convergence ;must iterate to get radiation pressure correctly
c
c commands controlling output =========
punch overview last "nlr_liner_grains.ovr"
punch dr last "nlr_liner_grains.dr"
punch continuum last "nlr_liner_grains.con" units microns
punch results last "nlr_liner_grains.rlt"
c
c nlr_liner_grains.in
c class nlr
c ========================================
c
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
title Paris meeting NLR model
c
c commands controlling continuum =========
interpolate (0 -10) (0.073 -10) (0.074 1) (7352 -4)
continue (7400 -15) (7.353e6 -20)
ionization parameter -2
c
c commands controlling geometry =========
stop lyman continuum optical depth 4
c
c commands for density & abundances =========
hden 3
init file="c84.ini"
abund -1 C-3.5229 N-4. O-3.22185 ne-3.82391 na=-8 mg-4.5229 al=-8
continue si-4.5229 s-4.82391 ar-8 ca=-8 fe-7 ni-8
c
c other commands for details =========
c this large group of lines are turned off so that the model runs
c 30 percent faster - lines are mainly fuv and x-ray, which we will
c not track in this model
no level2
iterate
atom h-like element helium levels resolved 10
c
c commands controlling output =========
punch overview last "nlr_paris.ovr"
punch dr last "nlr_paris.dr"
punch results last "nlr_paris.rlt"
c
c nlr_paris.in
c class nlr
c ========================================
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
title cold nova shell
c Ferland et al. 1984 DQ Her
c model of room temperature ionized cloud arund old nova DQ Her
c roughly that of
c tests behaviour of code at very low temperatures
c
c commands controlling continuum =========
c flat continuum, followed by nu^-2 power law
interpolate (0 0) (0.3 0) (8.e6 -14.8)
luminosity total 34
c
c commands for density & abundances =========
hden = 2.
abundances nova
grains no qheat single
c
c commands controlling geometry =========
filling factor 0.667
covering factor 0.667
radius 16.5682 , thickness = 16.14613
c need this since gas is so cool
stop temp = 100
c
c other commands for details =========
# >>chng 06 aug 02, add cosmic rays, should always have been included
cosmic rays background
iterate
turbulence 300
age 70 years %it exploded in the 1930's
atom h-like element hydrogen levels resolved 15
atom h-like element helium levels resolved 15
c
c commands controlling output =========
normalize to 4861 label="CaBo" intensity 1.169
print line all
punch overview last "nova_dqher.ovr"
punch results last "nova_dqher.rlt"
punch dr last "nova_dqher.dr"
punch transmitted continuum "nova_dqher.trn" last
c
c nova_dqher.in
c class nova
c ========================================
c
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
title dense nova photosphere
c
c commands controlling continuum =========
c this is the result of this command
c table star kurucz 35000; use old atlas atmosphere
c and makes it possible to run sims without
c installing the stellar atmosphere files
c set SED of central star
table read "star_kurucz_35000.dat"
c set luminosity of central star
absolute bolometric magnitude -8.1
c
c commands for density & abundances =========
hden 10 ;log of total hydrogen density (cm-3) at illuminated face
abundances old solar 84 ; use old solar abundances for record keeping
c
c commands controlling geometry =========
sphere ; model is a full sphere covering the central star
radius 12 to 14; log of inner and outer radii (cm)
c
c other commands for details =========
iterate to convergence
c
c commands controlling output =========
print line faint -1
punch overview "nova_photos.ovr" last
punch results "nova_photos.rlt" last
punch dr "nova_photos.dr" last
punch heat "nova_photos.het" last
punch cool "nova_photos.col" last
c
c nova_photos.in
c class nova
c ========================================
c
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
title test phymir optimizers
c spectrum computed with hden 5, temp 4
c subplex, phymir, powell
c
c commands controlling continuum =========
black 40000 K
ionization par -3
c
c commands for density & abundances =========
hden 4 vary
init file "hheonly.ini"
element oxygen on
c
c commands controlling geometry =========
Case B
stop zone 1
c
c other commands for details =========
optimize tolerance 0.03
constant temper 4.3 vary
optimize phymir
optimize iteration 100
c the following spectrum was derived by running this sim at hden 5 and t=4
c resulting eden was 5.039 and T=4, which we shall assert that we find
c >>chng 06 apr 03, backdate to old [OII] As and rederive spectrum
optimize lines
o ii 3729 0.1432
o ii 3726 0.4055
o ii 7323 0.5281
o ii 7332 0.4257
o 3 5007 3.6189
totl 4363 0.0342
end of lines
c
c commands controlling output =========
print line faint -2
c
c
c optimize_phymir.in
c class optimizer
c ========================================
c
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
title test subplex optimizer
c spectrum computed with hden 5, temp 4
c subplex, phymir, amoeba, powell
c
c commands controlling continuum =========
black 40000 K
ionization par -3
c
c commands for density & abundances =========
hden 4 vary
init file "hheonly.ini"
element oxygen on
c
c commands controlling geometry =========
Case B
stop zone 1
c
c other commands for details =========
constant temper 4.3 vary
optimize subplex
optimize iteration 100
optimize tolerance 0.01
c the following spectrum was derived by running this sim at hden 5 and t=4
c resulting eden was 5.039 and T=4, which we shall assert that we find
c >>chng 06 apr 03, backdate to old [OII] As and rederive spectrum
optimize lines
o ii 3729 0.1432
o ii 3726 0.4055
o ii 7323 0.5281
o ii 7332 0.4257
o 3 5007 3.6189
totl 4363 0.0342
end of lines
c
c commands controlling output =========
print line faint -2
c
c
c optimize_subplex.in
c class optimizer
c ========================================
c
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
title conditions similar to Orion nebula blister
c orion hii region with open geometry
c
c commands controlling continuum =========
c SED of central star
table read "star_kurucz_39600.dat"
c its flux of H-ionizing photons
phi(h) 13.0
c
c this is to include velocity field in radiative transfer
turbulence 8 km/sec no pressure
c
c commands for density & abundances =========
hden 4
abundances hii region no grains
grains orion
c
c commands controlling geometry =========
cosmic rays, background
constant pressure
c this is the account for continued matter beyond i front
double optical depths
c
c other commands for details =========
iterate 2
c
c commands controlling output =========
print line faint -5
c print lines as surface brightness
print lines surface brightness arcsec
print line optical depths
print diffuse continuum
c want to print line intensities are surface brightness, per arcsec^2
print lines surface brightness arcsec
print diffuse continuum
punch overview last "orion_hii_open.ovr"
punch dr last "orion_hii_open.dr"
punch continuum last "orion_hii_open.con" units microns
punch transmitted continuum last "orion_hii_open.trn"
punch overview last "orion_hii_open.ovr"
punch fine opacity last "orion_hii_open.opc" range 0.7 0.9 ryd
punch element nitrogen last no hash "orion_hii_open.nit"
punch line emissivity "orion_hii_open.ems" last no hash emergent
totl 5199
o 1 6300
end of lines
punch linelist "orion_hii_open.lin" "LineList_HII.dat" last no hash emergent absolute
c
c orion_hii_open.in
c class hii
c ========================================
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
title constant pressure H+ region/pdr
c
c commands controlling continuum =========
c the incident continuum is two parts
c star and flux of photons striking it
c this is the photosphere of the OVI star, its temperature and Q(H)
c this is the result of this command
c table star kurucz 39600 K
c and makes it possible to run these orion sims without
c installing the stellar atmosphere files
table read "star_kurucz_39600.dat"
Q(H) 49
c this adds the observed hot brems, its temperature and the flux of
c photons striking the cloud
brems 6
phi(h) 10
c add cosmic rays, which are important in the pdr
cosmic rays, background
c
c commands controlling geometry =========
c this sets the separation from the star and the face of the cloud
radius 17.4507
c this turns off the stop temperature opption
c the sim will not stop due to temperature
stop temperature off
c this is typical of a gmc, larson 1981
stop total hydrogen column density 22
c this sets the thickness of the HII region & PDR
stop thickness 0.5 linear parsec
c assume constant pressure
c constant gas pressure
constant pressure
c this will result in a milli gauss B-field in molecular region
magnetic field -5 gauss
c the orion environment full covers the star, so turn on sphere
sphere
c we have a spherical geometry but want to simulate observing
c through a spectrometer's slit. use the aperture
c command for this
aperture beam
c
c other commands for details =========
c mimic existence of unmodeled molecular gas
double
c iterate since lines optically thick
iterate
c the observed microturbulence, partially a flow, so not included in pressure
turbulence 8 km/sec no pressure
c set the line width so lines appear on the punch continuum
set punchLwidth 10 km/s
c there should be no failures at all
failures 3
c
c this model goes quite deep, needs lots of zones
set nend 2200
c
c commands for density & abundances =========
c this is the log of the initial H density, cm-3
hden 4
c this will speed up the calculation a bit
init file="ism.ini"
c this uses HII region abundances, but no grains
abundances hii region no grains
c this turns on orion grains, but leaves quantum heating off to save time
grains orion no qheat
c turn on PAHs, with an abundance that depends on H0 fraction,
c as suggested by long-slit observations of Orion bar,
c with an abundance 3x larger than default built into the code
grains pah function 3 no qheat
c
c commands controlling output =========
normalize to "O 1" 63.17m
c print lots of faint CO lines
print line faint -4
punch overview last "orion_hii_pdr.ovr"
punch heating "orion_hii_pdr.het"
punch cooling "orion_hii_pdr.col"
punch dr last "orion_hii_pdr.dr"
punch results last "orion_hii_pdr.rlt"
punch continuum last "orion_hii_pdr.con" units microns
punch hydrogen 21 cm last "orion_hii_pdr.21cm"
punch hydrogen lya last "orion_hii_pdr.lya"
punch element silicon last "orion_hii_pdr.sil"
punch grain extinction last "orion_hii_pdr.grnext"
punch grain charge last "orion_hii_pdr.grnchr"
punch grain potential last "orion_hii_pdr.grnpot"
punch grain temperature last "orion_hii_pdr.grntem"
c
c
c orion_hii_pdr.in
c class hii pdr
c ========================================
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
title constant gas pressure H+ region/PDR
c much faster due to physics disabled by fast.ini
c
c commands controlling continuum =========
c the incident continuum is two parts
c star and flux of photons striking it
c this is the result of this command
c table star kurucz 39600 K
c and makes it possible to run these orion sims without
c installing the stellar atmosphere files
table read "star_kurucz_39600.dat"
Q(H) 49
c add cosmic rays, which are important at depth
cosmic rays, background
c plus hot brems
brems 6
phi(h) 10
c
c commands for density & abundances =========
hden 4
init file="fast.ini"
abundances hii region no grains
c single sized grain with no quantum heating
grains orion no qheat single
c
c commands controlling geometry =========
radius 17.4507
sphere
c let it go into the molecular cloud
stop temperature 10 linear
c this is roughly the thickness of OMC1
stop thickness 1 linear parsec
c mimic existence of unmodeled molecular gas with double command
double
c
c other commands for details =========
failures 3
iterate
c make constant gas pressure since fast turned off line radiation pressure
constant gas pressure
c the observed microturbulence
turbulence 8 km/sec
c we have a spherical geometry but want to simulate observing
c through a spectrometer's slit. use the aperture
c command for this
aperture beam
c
c commands controlling output =========
normalize to "CaBo" 4861
print line faint -4
punch overview last "orion_hii_pdr_fast.ovr"
punch heating "orion_hii_pdr_fast.het"
punch cooling "orion_hii_pdr_fast.col"
punch dr last "orion_hii_pdr_fast.dr"
punch results last "orion_hii_pdr_fast.rlt"
punch continuum last "orion_hii_pdr_fast.con" units microns
punch ionizing continuum last "orion_hii_pdr_fast.ion"
punch hydrogen 21 cm last "orion_hii_pdr_fast.21cm"
punch hydrogen lya last "orion_hii_pdr_fast.lya"
punch element silicon last "orion_hii_pdr_fast.sil"
punch element sulphur last "orion_hii_pdr_fast.sul"
c
c
c orion_hii_pdr_fast.in
c class hii pdr
c ========================================
c
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
title the Orion HII Region / PDR / Molecular cloud with an open geometry
c
c commands controlling continuum =========
c the incident continuum has two parts
c kurucz continuum with flux of photons striking cloud
c this is the the OVI star, its temperature and phi(H)
c this is the result of this command
c table star kurucz 39600 K
c and makes it possible to run these orion sims without
c installing the stellar atmosphere files
table read "star_kurucz_39600.dat"
phi(H) 13
c
c this adds the observed hot brems
c its temperature (as log of T) and the flux of
c photons striking the cloud
brems 6
phi(h) 10
c
c cosmic rays are important for pdr chemistry
cosmic rays, background
c
c commands controlling geometry =========
c this turns off the stop temperature option
c so the sim will not stop due to temperature
stop temperature off
c this sets the thickness of the HII region & PDR
stop thickness 0.5 linear parsec
c this is typical of a gmc, larson 1981
stop total hydrogen column density 22
c this will result in a milli gauss B-field in molecular region
magnetic field -5 gauss
c assume constant pressure
constant pressure
set nend 2000
c
c other commands for details =========
failures 3
c mimic existence of unmodeled molecular gas
double
c iterate since lines optically thick
iterate
c set microturbulence in equipartition with B field
turbulence equipartition
c set the line width so lines appear on the punch continuum
set punchLwidth 10 km/s
c
c commands for density & abundances =========
c this is the log of the initial H density, cm-3
hden 4
c this will speed up the calculation a bit
init file="ism.ini"
c this uses HII region abundances, but no grains
abundances hii region no grains
c this uses orion grains
grains orion
c turn on PAHs, with an abundance that depends on H0 fraction,
c as suggested by long-slit observations of Orion bar,
c with an abundance 3x larger than default built into the code
grains pah function 3
c
c commands controlling output =========
c print lots of faint CO lines
print line faint -6
c normalize to Ha
normalize to "H 1" 6563
punch overview last "orion_hii_pdr_pp.ovr"
punch temperature last "orion_hii_pdr_pp.tem"
punch overview "orion_hii_pdr_pp.ovr1"
punch molecules last "orion_hii_pdr_pp.mol"
punch molecules "orion_hii_pdr_pp.mol1"
punch heating "orion_hii_pdr_pp.het"
punch cooling "orion_hii_pdr_pp.col"
punch dr last "orion_hii_pdr_pp.dr"
punch results last "orion_hii_pdr_pp.rlt"
punch continuum last "orion_hii_pdr_pp.con" units microns
punch hydrogen 21 cm last "orion_hii_pdr_pp.21cm"
punch hydrogen lya last "orion_hii_pdr_pp.lya"
punch element silicon last "orion_hii_pdr_pp.sil"
punch pressure last "orion_hii_pdr_pp.pre"
punch pressure "orion_hii_pdr_pp.pre1"
punch grain extinction last "orion_hii_pdr_pp.grnext"
punch grain charge last "orion_hii_pdr_pp.grnchr"
punch grain potential last "orion_hii_pdr_pp.grnpot"
punch grain temperature last "orion_hii_pdr_pp.grntem"
punch grain temperature "orion_hii_pdr_pp.grntem1"
c
c
c orion_hii_pdr_pp.in
c class hii pdr
c ========================================
similar to orion_hii_pdr except for plane parallel geometry
pdr_co_fully.in H2 and CO in fully molecular limit
title H2 and CO in fully molecular limit
c this is a pair with pdr_co_fully_noneq - that tests non equilibrium chem
c
c commands controlling continuum =========
blackbody 5000
luminosity total solar linear 2
brems 6
luminosity total solar log -2.7
c
c commands for density & abundances =========
c set the density and composition, ism with grains
hden 10
abundances ism no qheat
c
c other commands for details =========
c this is an important ionization source
cosmic ray background
c code will stop at 4000 K by default, lower this temp so we
c can do fully molecular gas
stop temperature 10K linear
c
c commands controlling geometry =========
c the radius and thickness
radius 15.8
stop thickness 6
turbulence 3 km / s
c
c commands controlling output =========
punch overview "pdr_co_fully.ovr"
punch molecules "pdr_co_fully.mol"
punch dr "pdr_co_fully.dr"
punch heating "pdr_co_fully.het"
punch cooling "pdr_co_fully.col"
punch grain charge "pdr_co_fully.grnchr"
punch grain drift "pdr_co_fully.grndft"
punch grain temperature "pdr_co_fully.grntem"
c
c
c gas has more he++ than He+ due to fast charge transfer with co
c neutralizing he+
c pdr_co_fully.in
c class pdr
c ========================================
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
title H2 and CO are fully molecular, non-equilibrium case
c this is a pair with pdr_co_fully.in, which does not include non-equil chem
c
c commands controlling continuum =========
blackbody 5000
luminosity total solar linear 2
brems 6
luminosity total solar log -2.7
c
c commands for density & abundances =========
c set the density and composition, ism with grains
hden 10
abundances ism no qheat
c
c other commands for details =========
c this is an important ionization source
cosmic ray background
c code will stop at 4000 K by default, lower this temp so we
c can do fully molecular gas
stop temperature 10K linear
c
c commands controlling geometry =========
c the radius and thickness
radius 15.8
stop thickness 6
turbulence 3 km / s
c this turns on non-equilibrium chemistry as suggested by Federman et al. 1996
set chemistry non equilibrium
c
c commands controlling output =========
punch overview "pdr_co_fully_noneq.ovr"
punch molecules "pdr_co_fully_noneq.mol"
punch dr "pdr_co_fully_noneq.dr"
punch heating "pdr_co_fully_noneq.het"
punch cooling "pdr_co_fully_noneq.col"
punch grain charge "pdr_co_fully_noneq.grnchr"
punch grain drift "pdr_co_fully_noneq.grndft"
punch grain temperature "pdr_co_fully_noneq.grntem"
c
c
c gas has more he++ than He+ due to fast charge transfer with co
c neutralizing he+
c pdr_co_fully_noneq.in
c class pdr
c ========================================
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
title illumination by cool STE blackbody
c gasis fully molecular, grains should be in STE
c
c commands controlling continuum =========
c illuminate with 120 blackbody in thermodynamic equilibrium
blackbody 120 STE
CMB
c
c commands for density & abundances =========
c density
hden 7
c ism dust and grains
abundances ISM no grains
c dust to gas ratio is 10x standard
grains 1.0
c lowers metals and grains to 1/10 standard, so metals are
c 1/10 solar while dust to gas ratio is galactic
metals and grains 0.1
c
c other commands for details =========
c set background cosmic rays to allow chemistry
cosmic ray background
iterate
c
c commands controlling geometry =========
radius 17.5
sphere
stop temperature 20K linear
stop column density 25.5
c
c commands controlling output =========
punch overview "pdr_coolbb.ovr"
punch molecules "pdr_coolbb.mol"
punch heating "pdr_coolbb.het"
punch cooling "pdr_coolbb.col"
punch grain temperature "pdr_coolbb.grntem"
c
c
c pdr_coolbb.in
c class pdr
c ========================================
This is a dense ISM exposed to a cool blackbody. This tests the
ability to converge onto a VERY molecular environment. Nearly all
C and H are in CO and H2.  This is our attempt at reproducing their calculation.
This is the dense molecular phase, not the phase that produces H3+
// >>refer model pdr Le Petit, F., Roueff, E., & Herbst, E. 2004,
// >>refercon A&A, 417, 993
If you do a thermal equilibrium calculation by removing the constant temperature
command the kinetic temperature will be about three times larger than
assumed in their paper.
pdr_HTT91.in low-density PDR from HTT91
title low-density PDR from HTT91
c >>refer test model Hollenbach, D., Takahashi, T., &
c >>refcon Tielens, A.G.G.M., 1991, ApJ,377, 192-209
c
c commands controlling continuum =========
c first continuum is FIR hot grain continuum produced in
c unmodeled HII Region
c this is hot star continuum
black 30000
intensity 0.2 range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
cosmic rays, background
c
c commands for density & abundances =========
hden 3
init file="ism.ini"
abundances he -1.01 c -3.52 n-8 o-3.30 ne-8 mg-5.89
continue si -6.10 s -5.10 cl-7 ar-8 fe -6.60
grains orion, abundance log 0.16 no qheat
c
c commands controlling geometry =========
sphere
c stop when gas is fully neutral
stop efrac -10
c this is to stop at an intended place, since results would be
c very dependent on details if we stop on temperature
stop thickness 18.954
c stop when gas is cold
stop temperature 10 linear
c add this to mimic unmodelled neutral gas
double optical depths
c
c other commands for details =========
iterate 2
case b
turbulence 1.5 km/sec
c
c commands controlling output =========
normalize to 157.6m "C 2"
c uv lines are strongly pumped by stellar continuum, break out contribution
print line pump
print line optical depths
print ages
punch overview last "pdr_HTT91.ovr"
punch dr "pdr_HTT91.dr"
punch molecules last "pdr_HTT91.mol"
punch results last "pdr_HTT91.rlt"
punch continuum units microns last "pdr_HTT91.con"
punch heating last "pdr_HTT91.het"
punch cooling last "pdr_HTT91.col"
c
c pdr_HTT91.in
c class pdr
c ========================================
c
This is the Hollenbach et al 1991 Low-density PDR
The case b command appears because the Lyman lines are
vastly optically thick in this environment.
If the command is removed the Lyman lines will be optically thin,
which will result in fast fluorescent excitation of the
(nearly totally neutral) hydrogen atom.
there is very little CO in this model since it is not thick enough
for the UV pumping lines to become optically thick
pdr_leiden_f1.in Leiden meeting model 1
title Leiden meeting model 1
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 5
extinguish 24
c
c commands for density & abundances =========
c hydrogen density
hden 3.
grains ism 1.16 no qheat
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden.ini"
c This command defines the grain temperature to be a constant 20 Kelvin
constant grain temperature 20
c This sets the temperature to a constant 50 Kelvin
constant temperature 50 linear
c
c commands controlling output =========
print line optical depths
punch overview "pdr_leiden_f1.ovr"
punch continuum "pdr_leiden_f1.con"
punch leiden lines "pdr_leiden_f1.lin"
punch leiden "pdr_leiden_f1.lei"
punch dr "pdr_leiden_f1.dr"
punch molecules "pdr_leiden_f1.mol"
punch grain physical conditions "pdr_leiden_f1.grn"
punch chemistry rates CO "pdr_leiden_f1.rat"
punch H2 destruction "pdr_leiden_f1.H2d"
punch H2 creation "pdr_leiden_f1.H2c"
punch secondaries "pdr_leiden_f1.sec"
c
c
c pdr_leiden_f1.in
c class pdr
c ========================================
c
This sim has some interesting properties. The grain temp is so low that
O freezes onto grains as H2O. This is so efficient that CO does not become
well formed - the CO/C ratio only reaches 0.3.
This is one of the tests in Rollig et al. 2007, A&A, 467, 187
pdr_leiden_f2.in Leiden meeting model 2
title Leiden meeting model 2
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use
c half the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 50000
extinguish 24
c
c commands for density & abundances =========
grains ism 1.16 no qheat
c hydrogen density
hden 3.
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden.ini"
c This command defines the grain temperature to be a constant 20 Kelvin
constant grain temperature 20
c This sets the temperature to a constant 50 Kelvin
constant temperature 50 linear
c
c commands controlling output =========
punch overview "pdr_leiden_f2.ovr"
punch continuum "pdr_leiden_f2.con"
punch molecules "pdr_leiden_f2.mol"
punch leiden lines "pdr_leiden_f2.lin"
punch leiden "pdr_leiden_f2.lei"
punch dr "pdr_leiden_f2.dr"
punch grain physical conditions "pdr_leiden_f2.grn"
c
c
c pdr_leiden_f2.in
c class pdr
c ========================================
c
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
pdr_leiden_f3.in Leiden meeting model 3
title Leiden meeting model 3
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 5
extinguish 24
c
c commands for density & abundances =========
grains ism 1.16 no qheat
c hydrogen density
hden 5.5
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden.ini"
c This command defines the grain temperature to be a constant 20 Kelvin
constant grain temperature 20
c This sets the temperature to a constant 50 Kelvin
constant temperature 50 linear
c
c commands controlling output =========
punch overview "pdr_leiden_f3.ovr"
punch continuum "pdr_leiden_f3.con"
punch leiden lines "pdr_leiden_f3.lin"
punch leiden "pdr_leiden_f3.lei"
punch dr "pdr_leiden_f3.dr"
punch grain physical conditions "pdr_leiden_f3.grn"
c
c
c pdr_leiden_f3.in
c class pdr
c ========================================
c
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
pdr_leiden_f4.in Leiden meeting model 4
title Leiden meeting model 4
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c
c commands for density & abundances =========
grains ism 1.16 no qheat
c
c commands controlling geometry =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 50000
extinguish 24
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden.ini"
c This command defines the grain temperature to be a constant 20 Kelvin
constant grain temperature 20
c This sets the temperature to a constant 50 Kelvin
constant temperature 50 linear
c hydrogen density
hden 5.5
c
c commands controlling output =========
punch overview "pdr_leiden_f4.ovr"
punch continuum "pdr_leiden_f4.con"
punch leiden lines "pdr_leiden_f4.lin"
punch leiden "pdr_leiden_f4.lei"
punch dr "pdr_leiden_f4.dr"
punch grain physical conditions "pdr_leiden_f4.grn"
c
c
c pdr_leiden_f4.in
c class pdr
c ========================================
c
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
pdr_leiden_hack_f1.in Leiden meeting model 1 with hacks
title Leiden meeting model 1 with hacks
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 5
extinguish 24
c
c commands for density & abundances =========
c hydrogen density
hden 3.
grains ism 1.16 no qheat
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden_hack.ini"
c This command defines the grain temperature to be a constant 20 Kelvin
constant grain temperature 20
c This sets the temperature to a constant 50 Kelvin
constant temperature 50 linear
c
c commands controlling output =========
punch leiden lines "pdr_leiden_hack_f1.lin"
punch leiden "pdr_leiden_hack_f1.lei"
punch dr "pdr_leiden_hack_f1.dr"
punch grain physical conditions "pdr_leiden_hack_f1.grn"
punch overview "pdr_leiden_hack_f1.ovr"
c
c
c
c
c pdr_leiden_f1_hack.in
c class pdr
c ========================================
c
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
this includes hacks to get "standard answer"
pdr_leiden_hack_f2.in Leiden meeting model 2 with hacks
title Leiden meeting model 2 with hacks
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use
c half the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 50000
extinguish 24
c
c commands for density & abundances =========
grains ism 1.16 no qheat
c hydrogen density
hden 3.
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden_hack.ini"
c This command defines the grain temperature to be a constant 20 Kelvin
constant grain temperature 20
c This sets the temperature to a constant 50 Kelvin
constant temperature 50 linear
c
c commands controlling output =========
punch leiden lines "pdr_leiden_hack_f2.lin"
punch leiden "pdr_leiden_hack_f2.lei"
punch dr "pdr_leiden_hack_f2.dr"
punch grain physical conditions "pdr_leiden_hack_f2.grn"
punch overview "pdr_leiden_hack_f2.ovr"
c
c
c pdr_leiden_hack_f2.in
c class pdr
c ========================================
c
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
includes hacks to get standard answer.
pdr_leiden_hack_f3.in Leiden meeting model 3 with hacks
title Leiden meeting model 3 with hacks
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 5
extinguish 24
c
c commands for density & abundances =========
grains ism 1.16 no qheat
c hydrogen density
hden 5.5
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden_hack.ini"
c This command defines the grain temperature to be a constant 20 Kelvin
constant grain temperature 20
c This sets the temperature to a constant 50 Kelvin
constant temperature 50 linear
c
c commands controlling output =========
punch leiden lines "pdr_leiden_hack_f3.lin"
punch leiden overview "pdr_leiden_hack_f3.ovr"
punch leiden "pdr_leiden_hack_f3.lei"
punch dr "pdr_leiden_hack_f3.dr"
punch grain physical conditions "pdr_leiden_hack_f3.grn"
c
c
c pdr_leiden_hack_f3.in
c class pdr
c ========================================
c
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
include hacks to get standard answer.
pdr_leiden_hack_f4.in Leiden meeting model 4 with hacks
title Leiden meeting model 4 with hacks
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c
c commands for density & abundances =========
grains ism 1.16 no qheat
c
c commands controlling geometry =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 50000
extinguish 24
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden_hack.ini"
c This command defines the grain temperature to be a constant 20 Kelvin
constant grain temperature 20
c This sets the temperature to a constant 50 Kelvin
constant temperature 50 linear
c hydrogen density
hden 5.5
c
c commands controlling output =========
punch leiden lines "pdr_leiden_hack_f4.lin"
punch leiden "pdr_leiden_hack_f4.lei"
punch dr "pdr_leiden_hack_f4.dr"
punch grain physical conditions "pdr_leiden_hack_f4.grn"
punch overview "pdr_leiden_hack_f4.ovr"
c
c
c pdr_leiden_hack_f4.in
c class pdr
c ========================================
c
This is one of the tests in Rollig et al. 2007, A&A, 467, 187
includes hacks needed to get standard answer.
pdr_leiden_hack_v1.in Leiden meeting model 5 with hacks
title Leiden meeting model 5 with hacks
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c is half the requested value
c they want for the model is actually twice the value below
table draine 5
extinguish 24
c
c commands for density & abundances =========
c hydrogen density
hden 3.
grains ism 1.16 no qheat
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden_hack.ini"
* element nitrogen on
* element nitrogen scale -1
* element silicon on
* element silicon scale -1
* element sulphur on
* element sulphur scale -1
* element chlorine on
* element chlorine scale -1
c Define the abundance of PAHs so we can reproduce the same photoelectric
c heating curve as BT94
c We have also scaled the grain abundance to achieve the desired AV/NH ratio
* grains PAH no qheat 8
c
c commands controlling output =========
punch leiden lines "pdr_leiden_hack_v1.lin"
punch leiden "pdr_leiden_hack_v1.lei"
punch dr "pdr_leiden_hack_v1.dr"
punch grain temperature "pdr_leiden_hack_v1.grn"
punch overview "pdr_leiden_hack_v1.ovr"
c
c
c pdr_leiden_hack_v1.in
c class pdr
c ========================================
c
This is one of the tests in Rollig et al. 2007, A&A, 467, 187
includes hacks to get standard answer.
pdr_leiden_hack_v2.in Leiden meeting model 6 with hacks
title Leiden meeting model 6 with hacks
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 50000
extinguish 24
c
c commands for density & abundances =========
c Define the abundance of PAHs so we can reproduce the same photoelectric
c heating curve as BT94
c We have also scaled the grain abundance to achieve the desired AV/NH ratio
* grains PAH no qheat 40
grains ism 1.16 no qheat
c hydrogen density
hden 3.
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden_hack.ini"
c
c commands controlling output =========
punch leiden lines "pdr_leiden_hack_v2.lin"
punch leiden "pdr_leiden_hack_v2.lei"
punch dr "pdr_leiden_hack_v2.dr"
punch grain temperature "pdr_leiden_hack_v2.grn"
punch overview "pdr_leiden_hack_v2.ovr"
punch heating "pdr_leiden_hack_v2.het"
punch cooling "pdr_leiden_hack_v2.col"
punch h2 rates "pdr_leiden_hack_v2.h2rat"
c
c
c pdr_leiden_hack_v2.in
c class pdr
c ========================================
c
This is one of the tests in Rollig et al. 2007, A&A, 467, 187
includes hacks to get standard answer.
pdr_leiden_hack_v3.in Leiden meeting model 7 with hacks
title Leiden meeting model 7 with hacks
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 5
extinguish 24
c
c commands for density & abundances =========
c Define the abundance of PAHs so we can reproduce the same photoelectric
c heating curve as BT94
c We have also scaled the grain abundance to achieve the desired AV/NH ratio
* grains PAH no qheat 5.7
grains ism 1.16 no qheat
c hydrogen density
hden 5.5
c
c commands controlling geometry =========
c
c other commands for details =========
c this sim has more than one thermal solution - force into lowest one,
c the one found by the rest of the group - without this we will find a
c soln at 1400 K
force temperature to 60K
failures 3
c use leiden initialization file
init file="pdr_leiden_hack.ini"
c
c commands controlling output =========
punch leiden lines "pdr_leiden_hack_v3.lin"
punch leiden "pdr_leiden_hack_v3.lei"
punch dr "pdr_leiden_hack_v3.dr"
punch grain temperature "pdr_leiden_hack_v3.grn"
punch overview "pdr_leiden_hack_v3.ovr"
punch heating "pdr_leiden_hack_v3.het"
punch cooling "pdr_leiden_hack_v3.col"
c
c
c pdr_leiden_hack_v3.in
c class pdr
c ========================================
c
This is one of the tests in Rollig et al. 2007, A&A, 467, 187
includes hacks to get standard answer
pdr_leiden_hack_v4.in Leiden meeting model 8 with hacks
title Leiden meeting model 8 with hacks
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 50000
extinguish 24
c
c commands for density & abundances =========
c Define the abundance of PAHs so we can reproduce the same photoelectric
c heating curve as BT94
c We have also scaled the grain abundance to achieve the desired AV/NH ratio
* grains PAH no qheat 40
* grains ism 0.936 no qheat
grains ism 1.16 no qheat
set PAH Bakes
c hydrogen density
hden 5.5
c
c commands controlling geometry =========
c
c other commands for details =========
* failures 3
c use leiden initialization file
init file="pdr_leiden_hack.ini"
c
c commands controlling output =========
punch leiden lines "pdr_leiden_hack_v4.lin"
punch leiden "pdr_leiden_hack_v4.lei"
punch dr "pdr_leiden_hack_v4.dr"
punch grain temperature "pdr_leiden_hack_v4.grn"
punch overview "pdr_leiden_hack_v4.ovr"
punch heating "pdr_leiden_hack_v4.het"
punch cooling "pdr_leiden_hack_v4.col"
punch transmitted continuum "pdr_leiden_hack_v4.con"
c
c
c pdr_leiden_hack_v4.in
c class pdr
c ========================================
c
This is one of the tests in Rollig et al. 2007, A&A, 467, 187
includes hacks to get standard answer.
pdr_leiden_v1.in Leiden meeting model 5
title Leiden meeting model 5
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c is half the requested value
c they want for the model is actually twice the value below
table draine 5
extinguish 24
c
c commands for density & abundances =========
c hydrogen density
hden 3.
grains ism 1.16 no qheat
c add PAHs
grains PAH no qheat 3 function
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden.ini"
c
c commands controlling output =========
punch overview "pdr_leiden_v1.ovr"
punch leiden lines "pdr_leiden_v1.lin"
punch leiden "pdr_leiden_v1.lei"
punch dr "pdr_leiden_v1.dr"
punch grain temperature "pdr_leiden_v1.grn"
c
c
c
c pdr_leiden_v1.in
c class pdr
c ========================================
c
This is one of the tests in Rollig et al. 2007, A&A, 467, 187
pdr_leiden_v2.in Leiden meeting model 6
title Leiden meeting model 6
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 50000
extinguish 24
c
c commands for density & abundances =========
c add PAHs and grains
grains PAH no qheat 3 function
grains ism 1.16 no qheat
c hydrogen density
hden 3.
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden.ini"
c
c commands controlling output =========
punch overview "pdr_leiden_v2.ovr"
punch leiden lines "pdr_leiden_v2.lin"
punch leiden "pdr_leiden_v2.lei"
punch dr "pdr_leiden_v2.dr"
punch grain temperature "pdr_leiden_v2.grn"
c
c
c pdr_leiden_v2.in
c class pdr
c ========================================
c
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
pdr_leiden_v3.in Leiden meeting model 7
title Leiden meeting model 7
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 5
extinguish 24
c
c commands for density & abundances =========
c add PAHs and grains
grains PAH no qheat 3 function
grains ism 1.16 no qheat
c hydrogen density
hden 5.5
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden.ini"
c
c commands controlling output =========
punch overview "pdr_leiden_v3.ovr"
punch leiden lines "pdr_leiden_v3.lin"
punch leiden "pdr_leiden_v3.lei"
punch dr "pdr_leiden_v3.dr"
punch grain temperature "pdr_leiden_v3.grn"
punch heating "pdr_leiden_v3.het"
punch cooling "pdr_leiden_v3.col"
c
c
c pdr_leiden_v3.in
c class pdr
c ========================================
c
pdr_leiden_v4.in Leiden meeting model 8
title Leiden meeting model 8
c This is one of the tests in Rollig et al. 2007, A&A, 467, 187
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 50000
extinguish 24
c
c commands for density & abundances =========
grains PAH no qheat 3 function
grains ism 1.16 no qheat
c hydrogen density
hden 5.5
c
c commands controlling geometry =========
c
c other commands for details =========
failures 3
c use leiden initialization file
init file="pdr_leiden.ini"
c
c commands controlling output =========
punch overview "pdr_leiden_v4.ovr"
punch leiden lines "pdr_leiden_v4.lin"
punch leiden "pdr_leiden_v4.lei"
punch dr "pdr_leiden_v4.dr"
punch grain temperature "pdr_leiden_v4.grn"
punch transmitted continuum "pdr_leiden_v4.con"
c
c
c pdr_leiden_v4.in
c class pdr
c ========================================
c
pdr_orion_veil.in Orion's veil
title Orion's veil
c
c commands controlling continuum =========
q(h) 50.000000
table star rubin
c AGN & CMB background
background z=0
cosmic rays background
c as a test this was tried - atomic temperature raised fm 100 to 140
c but nothing really wrong
* cosmic rays equipartition
c the observed magnetic field, roughly 100 micro Gauss
magnetic field -4
c
c commands for density & abundances =========
hden 3.1
init "ism.ini"
abundances orion no grains
grains orion no qheat
c
c commands controlling geometry =========
stop neutral hydrogen column density 21.6
radius 19.1
stop temperature linear 5
c this will not be hit, but put it in to insure that we stop if
c gas becomes totally molecular
stop av 10
c
c other commands for details =========
failures 3
* uncomment to include large H2 molecule - results will CHANGE!
* atom h2
turbulence 0.5 km/sec
sphere
c c this simulates Lyman lines in the stellar continuum
c atom h-like lyman pumping off
c
c commands controlling output =========
print line optical depths
punch PDR "pdr_orion_veil.pdr"
punch feii column densities "pdr_orion_veil.fe2col"
punch hydrogen 21 cm "pdr_orion_veil.21cm"
punch molecules "pdr_orion_veil.mol"
punch overveiw "pdr_orion_veil.ovr"
punch column densities "pdr_orion_veil.col"
punch heating "pdr_orion_veil.het"
punch cooling "pdr_orion_veil.col"
punch dr "pdr_orion_veil.dr"
punch H2 rates "pdr_orion_veil.h2rat"
punch pressure "pdr_orion_veil.pre"
punch wind "pdr_orion_veil.wnd"
print line optical depths
punch continuum units microns "pdr_orion_veil.con" last
c
c pdr_orion_veil.in
c class pdr
c ========================================
c
This is Abel et al 2004 model of Orion's veil, the layer of gas in front
of the Orion Nebula.
>>refer Orion Veil Abel, N. P., Brogan, C. L., Ferland, G. J.,
>>refercon O'Dell, C. R., Shaw, G., & Troland, T. H. 2004
pdr_th85ism.in TH85 PDR with ISM grains
title TH85 PDR with ISM grains
c
c commands controlling continuum =========
c cosmic radiation background
background z=0
c cosmic ray background ionization and heating
cosmic rays, background
c first continuum is FIR hot grain continuum produced in
c unmodeled HII Region
blackbody, t = 75 K
intensity 2.7 (total)
c this is the attenuated hot stellar continuum
black 30000
intensity 2.204 range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
c
c commands controlling geometry =========
c simulate effects of gas we do not model
double
c their turbulence
turbulence 2.7 km/sec
c stopping criteria
c this should be the one actually used
stop AV 33.2 extended
c stop when gas is fully neutral
stop efrac -10
c stop when gas is cold
stop temperature 10 linear
c stop at thickness of 16.5 so that mole limit does not
c stop this calculation - that would make results very
c detail dependent
stop thickness 19
c
c commands for density & abundances =========
hden 5.362
c this turns off some elements, and processes we don't need
c so needs to come before the elements
init file="ism.ini"
abundances he -1.01 c -3.52 n-8 o-3.30 ne-8 mg-5.89
continue si -6.10 s -5.10 cl-7 ar-8 fe -6.60
c use ism abundances but turn of quantum heating
grains ism, abundance log 0.16 no qheat
c
c other commands for details =========
c must iterate since many FIR MIR lines are optically thick
iterate
c this is a closed geometry, in Orion, veil covers 2pi sr
sphere
c make Lyman lines very optically thick, which stops pumping by
c Balmer continuum
case b
c this should run cleanly - turn down number of allow conv fails
failures 3
c
c commands controlling output =========
normalize to "C 2" 157.6m
c want the spectrum to be relative to this [C II] line
c uv lines are strongly pumped by stellar continuum, break out contribution
print line pump
print line optical depths
print ages
punch overview last "pdr_th85ism.ovr"
punch pdr last "pdr_th85ism.pdr"
punch molecules last "pdr_th85ism.mol"
punch dr last "pdr_th85ism.dr"
punch hydrogen physical conditions last "pdr_th85ism.hyd"
punch results last "pdr_th85ism.rlt"
punch continuum units microns last "pdr_th85ism.con"
punch heating last "pdr_th85ism.het"
punch cooling last "pdr_th85ism.col"
punch hydrogen 21 cm last "pdr_th85ism.21cm"
punch element magnesium last "pdr_th85ism.mag"
punch grain extinction last "pdr_th85ism.grnext"
punch grain potential last "pdr_th85ism.grnpot"
punch grain temperature last "pdr_th85ism.grntem"
punch grain charge last "pdr_th85ism.grnchr"
c
table lines "LineList_PDR.dat"
c pdr_th85ism.in
c class pdr
c ========================================
c
This is the Tielens and Hollenbach (1985a, b) standard model of
the Orion photodissociation region (PDR). Specifically,
this is my attempt at their Table 2 of paper 2, ApJ 291, p749.
The case b command appears because the Lyman lines are
vastly optically thick in this environment.
If the command is removed the Lyman lines will be optically thin,
which will result in fast fluorescent excitation of the
(nearly totally neutral) hydrogen atom.
// >>refer model pdr Tielens, A. G. G. M., & Hollenbach, D. 1985a, ApJ, 291, 722
// >>refer model pdr Tielens, A. G. G. M., & Hollenbach, D. 1985b, ApJ, 291, 746
pdr_th85ism_cgto.in TH85 pdr with ISM grains and C > O
title TH85 pdr with ISM grains and C > O
c
c commands controlling continuum =========
c cosmic radiation background
background z=0
c cosmic ray background ionization and heating
cosmic rays, background
c first continuum is FIR hot grain continuum produced in
c unmodeled HII Region
blackbody, t = 75 K
intensity 2.7 (total)
c this is the attenuated hot stellar continuum
black 30000
intensity 2.204 range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
c
c commands controlling geometry =========
c simulate effects of gas we do not model
double
c their turbulence
turbulence 2.7 km/sec
c stopping criteria
c this should be the one actually used
stop AV 33.2 extended
c stop when gas is fully neutral
stop efrac -10
c stop when gas is cold
stop temperature 10 linear
c stop at thickness of 16.5 so that mole limit does not
c stop this calculation - that would make results very
c detail dependent
stop thickness 19
c
c commands for density & abundances =========
hden 5.362
c this turns off some elements, and processes we don't need
c so needs to come before the elements
init file="ism.ini"
c this is the TH85 mix except C is raised by 0.2 dex,
c and O lowered byt his amount, so that C/O > 1
abundances he -1.01 c -3.4 n-8 o-3.50 ne-8 mg-5.89
continue si -6.10 s -5.10 cl-7 ar-8 fe -6.60
c use ism abundances but turn of quantum heating
grains ism, abundance log 0.16 no qheat
c
c other commands for details =========
c must iterate since many FIR MIR lines are optically thick
iterate
c this is a closed geometry, in Orion, veil covers 2pi sr
sphere
c make Lyman lines very optically thick, which stops pumping by
c Balmer continuum
case b
c this should run cleanly - turn down number of allow conv fails
failures 3
c
c commands controlling output =========
normalize to "C 2" 157.6m
c want the spectrum to be relative to this [C II] line
c uv lines are strongly pumped by stellar continuum, break out contribution
print line pump
print line optical depths
print ages
punch overview last "pdr_th85ism_cgto.ovr"
punch pdr last "pdr_th85ism_cgto.pdr"
punch molecules last "pdr_th85ism_cgto.mol"
punch dr last "pdr_th85ism_cgto.dr"
punch hydrogen physical conditions last "pdr_th85ism_cgto.hyd"
punch results last "pdr_th85ism_cgto.rlt"
punch continuum units microns last "pdr_th85ism_cgto.con"
punch heating last "pdr_th85ism_cgto.het"
punch cooling last "pdr_th85ism_cgto.col"
punch hydrogen 21 cm last "pdr_th85ism_cgto.21cm"
punch element magnesium last "pdr_th85ism_cgto.mag"
punch grain extinction last "pdr_th85ism_cgto.grnext"
punch grain potential last "pdr_th85ism_cgto.grnpot"
punch grain temperature last "pdr_th85ism_cgto.grntem"
punch grain charge last "pdr_th85ism_cgto.grnchr"
c
c pdr_th85ism_cgto.in
c class pdr
c ========================================
c
This is the Tielens and Hollenbach (1985a, b) standard model of
the Orion photodissociation region (PDR) but with the C abundance
increased by 0.2 dex, and O lowered by this amount, so that C/O>1.
Specifically, this is their Table 2 of paper 2, ApJ 291, p749.
The case b command appears because the Lyman lines are
vastly optically thick in this environment.
If the command is removed the Lyman lines will be optically thin,
which will result in fast fluorescent excitation of the
(nearly totally neutral) hydrogen atom.
// >>refer model pdr Tielens, A. G. G. M., & Hollenbach, D. 1985a, ApJ, 291, 722
// >>refer model pdr Tielens, A. G. G. M., & Hollenbach, D. 1985b, ApJ, 291, 746
pdr_th85orion.in TH85 PDR with Orion grains
title TH85 PDR with Orion grains
c
c commands controlling continuum =========
c cosmic background
background
c galactic cosmic ray background
cosmic rays, background
c first continuum is FIR hot grain continuum produced in
c unmodeled HII Region
blackbody, t = 75 K
intensity 2.7 (total)
c this is the attenuated hot stellar continuum
black 30000
intensity 2.204 range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
c
c commands for density & abundances =========
hden 5.362
init file="ism.ini"
grains orion, abundance log 0.16 no qheat
abundances he -1.01 c -3.52 n-8 o-3.30 ne-8 mg-5.89
continue si -6.10 s -5.10 cl-7 ar-8 fe -6.60
c
c commands controlling geometry =========
c simulate effects of gas we do not model
double
sphere
c stopping criteria
c this should be the one actually used
c >>chn 04 mar 13, from 10 to 36.3, bug in AV had stopped at this depth,
c so change it to this to keep model the same
stop AV 36.3 extended
c stop when gas is fully neutral
stop efrac -10
c stop when gas is cold
stop temperature 10 linear
c stop at thickness so that would make results very
c detail dependent
stop thickness 19
c
c other commands for details =========
turbulence 2.7 km/sec
iterate
failures 3
c
c this is done to not allow pumping and subsequent photoionization
c of H by Balmer continuum in keeping with std pdr assumptions
case b
c
c commands controlling output =========
normalize to "C 2" 157.6m
c uv lines are strongly pumped by stellar continuum, break out contribution
print line pump
print line optical depths
print ages
c
punch overview "pdr_th85orion.ovr" no hash
punch pdr last "pdr_th85orion.pdr"
c this only outputs major molecules
punch molecules last "pdr_th85orion.mol"
punch dr "pdr_th85orion.dr"
c this is to get all of H molecules
punch hydrogen physical conditions last "pdr_th85orion.hyd"
punch results last "pdr_th85orion.rlt"
punch continuum units microns last "pdr_th85orion.con"
punch ionizing continuum last "pdr_th85orion.ion"
punch heating last "pdr_th85orion.het"
punch cooling last "pdr_th85orion.col"
punch hydrogen 21 cm last "pdr_th85orion.21cm"
c these are for the grains
punch grain extinction last "pdr_th85orion.grnext"
punch grain potential last "pdr_th85orion.grnpot"
punch grain temperature last "pdr_th85orion.grntem"
punch grain charge last "pdr_th85orion.grnchr"
c
c
c pdr_th85orion.in
c class pdr
c ========================================
This is the Tielens and Hollenbach (1985a, b) standard model of
the Orion photodissociation region (PDR). Specifically,
this is my attempt at their Table 2 of paper 2, ApJ 291, p749.
The case b command appears because the Lyman lines are
vastly optically thick in this environment.
If the command is removed the Lyman lines will be optically thin,
which will result in fast fluorescent excitation of the
(nearly totally neutral) hydrogen atom.
// >>refer model pdr Tielens, A. G. G. M., & Hollenbach, D. 1985a, ApJ, 291, 722
// >>refer model pdr Tielens, A. G. G. M., & Hollenbach, D. 1985b, ApJ, 291, 746
pn_fluc.in Paris PN with density fluctuations
title Paris PN with density fluctuations
c
c commands for density & abundances =========
fluctuations 16.5 4 3
c this sets up the code like version c84, with fewer chemical elements
init file="c84.ini"
c this sets the abundances of the elements that we will use
abund -1 C-3.523 N-4. O-3.222 ne-3.824 na=-10 mg-4.523 al=-10
continue si-4.523 s-4.824 ar-10 ca=-10 fe-10 ni=-10
c
c commands controlling continuum =========
black body, T = 150000 K, radius = 10
black 5
luminosity total 38
c
c commands controlling geometry =========
sphere
radius 17
c
c other commands for details =========
c
c commands controlling output =========
punch overview last "pn_fluc.ovr"
punch element nitrogen last "pn_fluc.nit"
punch dr last "pn_fluc.dr"
punch results last "pn_fluc.rlt"
c
c pn_fluc.in
c class pn function
c ========================================
The boundary conditions are similar to those for the Paris meeting PN,
a homogeneous grain-free PN. This model has density fluctuations,
with values chosen so that the mean ne np V are the same
for the nebulae with and without fluctuations.
Checks:
- Check that the fluctuations command works.
- How do results compare with homogeneous Paris pn?
pn_ots.in Paris PN with ots
title Paris PN with ots
c recompute "standard" PN model of the Pequignot Meudon Conferance
c
c commands controlling continuum =========
black body, T = 150000 K, radius = 10
c
c commands for density & abundances =========
hden = 3.4771213
init file="c84.ini"
abund -1 C-3.523 N-4. O-3.222 ne-3.824 na=-10 mg-4.523 al=-10
continue si-4.523 s-4.824 ar-10 ca=-10 fe-10 ni=-10
c
c commands controlling geometry =========
radius = 17
sphere
c
c other commands for details =========
diffuse ots
no level2
iterate
atom h-like element hydrogen levels resolved 10
atom h-like element helium levels resolved 15
c
c commands controlling output =========
punch overview last "pn_ots.ovr"
punch element nitrogen last "pn_ots.nit"
punch results last "pn_ots.rlt"
punch dr last "pn_ots.dr"
c
c pn_ots.in
c class pn
c ========================================
c
This is the on-the-spot version of the Paris Planetary Nebula.
Checks:
- Q(H) total 4861 luminosity is close to expected value
- Line spectrum similar to that predicted by default conditions.
pn_paris.in Paris meeting PN
title Paris meeting PN
c standard" PN model of the Pequignot Meudon Conferance
c
c commands controlling continuum =========
black body, T = 150000 K, radius = 10
c
c commands for density & abundances =========
hden = 3.4771213
init file="ism.ini"
abund he -1 C-3.523 N-4. O-3.222 ne-3.824 mg-4.523
continue si-4.523 s-4.824 cl-7 ar-10 fe-10
c
c commands controlling geometry =========
radius = 17
sphere
c
c other commands for details =========
age 10000 years
c
c commands controlling output =========
normalize to "Ca b" 4861
print line optical depths
print ages
print column densities
punch overview "pn_paris.ovr"
punch transmitted continuum "pn_paris.trn"
punch continuum units microns "pn_paris.con"
punch element carbon "pn_paris.car"
punch physical conditions "pn_paris.phy"
punch element nitrogen "pn_paris.nit"
punch dr "pn_paris.dr"
punch temperature "pn_paris.tem"
punch lines emissivity "pn_paris.ems"
h 1 6563
s 2 6720
end of lines
punch averages "pn_paris.avr" last
temperature hydrogen 1
end of averagers
c
c pn_paris.in
c class pn
c ========================================
c
This is one of the "standard" models computed at the Paris meeting on
photoionization and shock calculations. A table in Hazy compares the
predictions of the current version of CLOUDY with predictions of a
few of the other codes.
The model is meant to represent a planetary nebula ionized by a very
hot central object. As a result there is a great deal of He++ and
the associated line and continuum emission is very important.
An age of 10000 years was set. This tests logic in the age command.
pn_paris_fast.in Paris PN, fast version
title Paris PN, fast version
c standard" PN model of the Pequignot Meudon Conferance
c
c commands controlling continuum =========
black body, T = 150000 K, radius = 10
c
c commands for density & abundances =========
hden = 3.4771213
init file="fast.ini"
abund he -1 C-3.523 N-4. O-3.222 ne-3.824 mg-4.523
continue si-4.523 s-4.824 ar-10
c
c commands controlling geometry =========
sphere
radius = 17
c
c other commands for details =========
c
c commands controlling output =========
normalize to "Ca b" 4861
punch overview "pn_paris_fast.ovr"
punch physical conditions "pn_paris_fast.phy"
punch element nitrogen "pn_paris_fast.nit"
punch dr "pn_paris_fast.dr"
c
c pn_paris_fast.in
c class pn
c ========================================
c
This is one of the "standard" models computed at the Paris meeting on
photoionization and shock calculations. A table in Hazy compares the
predictions of the current version of CLOUDY with predictions of a
few of the other codes.
The model is meant to represent a planetary nebula ionized by a very
hot central object. As a result there is a great deal of He++ and
the associated line and continuum emission is very important.
pn_sqrden.in PN with density propt R^-2 and filling factor
title PN with density propt R^-2 and filling factor
c this is an optically thin model, which will have a broad range
c of density but the same ionization parameter across the model.
c the physical condtions should not vary by much across the structure
c
c commands controlling continuum =========
c continuum is hot blackbody at ~Ledd for solar mass
blackbody, t=5 luminosity=38
c
c commands for density & abundances =========
c the density will fall off as the inverse square of the radius, hence the name
hden 5 -2
init file "ism.ini"
c use default PN abundances but turn off quantum heating since
c we are not going to save the predicted near IR continuum
abundances planetary no qheat
c
c commands controlling geometry =========
c small filling factor so that region will be optically thin
filling factor -2
c set inner and outer radius
radius 16 18
sphere
c
c other commands for details =========
iterate
c
c commands controlling output =========
print line faint 1
punch overview "pn_sqrden.ovr" last
punch dr "pn_sqrden.dr" last
c
c pn_sqrden.in
c class pn
c ========================================
Checks:
- Zone thickness budgeting handled OK.
- physical conditions nearly constant across computed structure
stars_atlas.in Atlas stellar atmosphere
title Atlas stellar atmosphere
c
c commands controlling continuum =========
c Approximate model of a hot star ionizing its surroundings.
c Assume H density of 1e+6 per cc. This run tests the new Kurucz model option.
c I choose the T_eff and log(g) values arbitrarily. It implies a star
c with luminosity 32300 L_sun, radius 6.4745 R_sun, and mass 3.745 M_sun.
table star atlas 30400.0 4.2
luminosity 4.509202522 solar
c
c commands for density & abundances =========
abundances old solar 84
hden 6.0
grains ism
c
c commands controlling geometry =========
radius -3.0 parsec
sphere
stop zone 1
set dr 0
c
c other commands for details =========
constant temperature 4
c
c commands controlling output =========
print continuum
c
punch overview last "stars_atlas.ovr"
punch results last "stars_atlas.rlt"
punch transmitted continuum last "stars_atlas.trn" no header
punch continuum last "stars_atlas.con" units microns
c
c stars_atlas.in
c class stars
c ========================================
This is a test that the code can correctly access the
large block of Atlas model atmosphere continua described by Kurucz (1991).
Kevin Volk provided it as part of his original coding of these
stellar atmosphere files.
Constant temperature is assumed since this tests shape of stellar continuum
rather than thermal physics.
Checks:
table star atlas command works.
stars_atlas_3d.in Atlas stellar atmosphere, 3D interpolation
title Atlas stellar atmosphere, 3D interpolation
c
c commands controlling continuum =========
c Approximate model of a hot star ionizing its surroundings.
c Assume H density of 1e+6 per cc. This run tests the atlas 3dim model option.
c I choose the T_eff and log(g) values arbitrarily.
table star atlas 3-dim 38400.0 4.82 -1.42
luminosity 4.509202522 solar
table star atlas odfnew 3-dim 38400.0 4.82 0.42
luminosity 4.509202522 solar
c
c commands for density & abundances =========
abundances old solar 84
hden 6.0
grains ism
c
c commands controlling geometry =========
radius -3.0 parsec
sphere
stop zone 1
set dr 0
c
c other commands for details =========
constant temperature 4
c
c commands controlling output =========
c
punch overview last "stars_atlas_3d.ovr"
punch results last "stars_atlas_3d.rlt"
punch transmitted continuum last "stars_atlas_3d.trn" no header
punch continuum last "stars_atlas_3d.con" units microns
c
c stars_atlas_3d.in
c class stars
c ========================================
This is a test that the code can correctly access the
large 3-dim block of Atlas model atmosphere continua.
Checks:
table star atlas 3dim command works.
stars_atlas_all.in interpolate on Atlas grids
title interpolate on Atlas grids
c
c commands controlling continuum =========
c Include stars with a wide range of metallicities to test access to these grids.
table star atlas Z+1.0 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z+0.5 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z+0.3 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z+0.2 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z+0.1 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z+0.0 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-0.1 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-0.2 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-0.3 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-0.5 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-1.0 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-1.5 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-2.0 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-2.5 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-3.0 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-3.5 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-4.0 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-4.5 38400.0 4.82
luminosity 4.509202522 solar
table star atlas Z-5.0 38400.0 4.82
luminosity 4.509202522 solar
c
c commands for density & abundances =========
abundances old solar 84
hden 6.0
grains ism
c
c commands controlling geometry =========
radius -2.0 parsec
sphere
stop zone 1
set dr 0
c
c other commands for details =========
constant temperature 4
c
c commands controlling output =========
c
punch overview last "stars_atlas_all.ovr"
punch results last "stars_atlas_all.rlt"
punch transmitted continuum last "stars_atlas_all.trn" no header
punch continuum last "stars_atlas_all.con" units microns
c
c stars_atlas_all.in
c class stars
c ========================================
This is a test that the code can correctly access the
2D grids of various metallicity of Atlas model atmosphere continua.
Checks:
access to the various atlas grids
stars_atlas_odfnew_all.in access various Atlas ODFNEW grids
title access various Atlas ODFNEW grids
c
c commands controlling continuum =========
c Include stars with a wide range of metallicities to test access to these grids.
table star atlas odfnew Z+0.5 38400.0 4.82
luminosity 4.509202522 solar
table star atlas odfnew Z+0.2 38400.0 4.82
luminosity 4.509202522 solar
table star atlas odfnew Z+0.0 38400.0 4.82
luminosity 4.509202522 solar
table star atlas odfnew Z-0.5 38400.0 4.82
luminosity 4.509202522 solar
table star atlas odfnew Z-1.0 38400.0 4.82
luminosity 4.509202522 solar
table star atlas odfnew Z-1.5 38400.0 4.82
luminosity 4.509202522 solar
table star atlas odfnew Z-2.0 38400.0 4.82
luminosity 4.509202522 solar
table star atlas odfnew Z-2.5 38400.0 4.82
luminosity 4.509202522 solar
c
c commands for density & abundances =========
abundances old solar 84
hden 6.0
grains ism
c
c commands controlling geometry =========
radius -2.0 parsec
sphere
stop zone 1
set dr 0
c
c other commands for details =========
constant temperature 4
c
c commands controlling output =========
c
punch overview last "stars_atlas_odfnew_all.ovr"
punch results last "stars_atlas_odfnew_all.rlt"
punch transmitted continuum last "stars_atlas_odfnew_all.trn" no header
punch continuum last "stars_atlas_odfnew_all.con" units microns
c
c stars_atlas_odfnew_all.in
c class stars
c ========================================
This is a test that the code can correctly access the
Atlas ODFNEW model atmosphere continua.
Checks:
access to the various atlas odfnew grids
stars_bstar2006.in tlusty bstar grid
title tlusty bstar grid
c
c commands controlling continuum =========
c Approximate model of a B star ionizing its surroundings.
c Assume H density of 1e+6 per cc. This run tests the new Tlusty model option.
c I choose the T_eff and log(g) values arbitrarily.
table star tlusty bstar 20400.0 4.2
luminosity 4.509202522 solar
c
c commands for density & abundances =========
abundances old solar 84
hden 6.0
grains ism
c
c commands controlling geometry =========
radius -3.0 parsec
sphere
stop zone 1
set dr 0
c
c other commands for details =========
c
c in this model the Lyman lines are pumped significantly by the stellar continuum;
c disable this process to avoid critical dependence on the precise shape of the continuum.
no induced processes
constant temperature 4
c
c commands controlling output =========
c
punch overview last "stars_bstar2006.ovr"
punch results last "stars_bstar2006.rlt"
punch transmitted continuum last "stars_bstar2006.trn" no header
c
c stars_bstar2006.in
c class stars
c ========================================
This is a test that the code can correctly access the
large block of Tlusty B-star model atmosphere continua.
Checks:
table star tlusty bstar command works.
stars_bstar2006_3d.in tlusty bstar grid
title tlusty bstar grid
c
c commands controlling continuum =========
c Approximate model of a B star ionizing its surroundings.
c Assume H density of 1e+6 per cc. This run tests the new Tlusty model option.
c I choose the T_eff, log(g) and log(Z) values arbitrarily.
table star tlusty bstar 3-dim 20400.0 4.2 -0.573
luminosity 4.509202522 solar
c
c commands for density & abundances =========
abundances old solar 84
hden 6.0
grains ism
c
c commands controlling geometry =========