DISPGEN OPTIONS
Multi-frequency continuum
options
Ionization state
specifiers (i.e., *)
Options are ordered under
subject. Associated with each option are requested inputs. Some inputs are not
prompted for, and can only be changed from their default values by specifying
them in the call. eg.
CJBB(JONS=T)
In this documentation, such
input are placed in [ ]. If you see a hidden option
which is not described, check $cmfdist/disp/maingen.f. The option use
should be obvious.
Many options, e.g., DC
(departure coefficients) operate on many species. The
species is specified by direct attachment to the option call. For example to
plot departure coefficient for C2, issue the command
DC_C2
Options that require species
addenda are specified by a * --- eg DC_*.
All logs are base 10, unless
specifically noted otherwise.
SVE and BOX file
Default
is to write file MAIN_OPT_STR.sve
Append
sve=filename to write a new .sve
file (no brackets)
Type
box=filename to write a .box file containing several .sve
files
Type .filename to
read .sve file
Type
#filename to read .box file
Options fall into different
classes: X-axis options, Y-axis options, and output. X-axis options simply set
the default X-axis for subsequent plots, although users should be aware that
not all plot options use the default X-axis. Y-axis options set the Y-axis.
Generally multiple Y-axis options can be executed before a call to the plotting
routine (PGPLOT subroutines). Some Y-axis options initiate a call to the plot
routine immediately.
XLOGR |
Set X axis to log(r/R*). |
XLINR |
Set X axis to r/R*. |
XARC |
Set X axis to arcseconds
[LIN=T] gives linear axis |
XAU |
Set X axis to units of AU
[LIN=T] give linear axis |
XRSUN |
Set X axis to units of Rsun
[LIN=T] gives linear axis |
XED |
Set X axis to log(Ne). |
XROSS |
Set X axis to log(Tau(Ross)). |
SXROSS |
Set X axis to spherical Rosseland
optical depth scale. |
XCOLD |
Set X axis to log(column density). |
XATOM |
Set X axis to log(Ni) where Ni is the
atom/ion density. |
XMASS |
Set X axis to mass exterior to grid point. |
XN |
Set X axis to vector index I |
XTEMP |
Set X axis to Temperature (units 104 K). |
XVEL |
Set X axis to vector index Vel(km/s) |
XLOGV |
Set X axis to vector index Log( Vel(km/s) ) |
XTAUC |
Set X axis to Log(Tau) [Continuum
wavelength requested] |
XCAKT |
Set X axis to CAK (Castor, Abbott, & Kelin
1975) t. The default Doppler velocity is 10km/s. Note that the CAK t
parameter is generally not a monotonic function of r.
[VTH] : hidden --- sets the Doppler velocity. |
TIT |
Allows
title (or revised) TITLE to be set. Note that inputing
"" will generally set the string to blanks. |
GR |
General
purpose Graphing routine. |
GRNL |
General
purpose Graphing routine. As for GR but ignores labels. |
GRED |
Plots
electron density on top axis. Assumes default X-axis. Ne is matched to X-axis
using monotonic interpolation. |
GROSS |
Plots Rosseland optical depth on top axis. Assumes default
X-axis. The Rosseland optical depth is matched to
X-axis using monotonic interpolation. |
SET-ATM |
Sets
atmosphere to wind or exponential. For use in calculating Tau at outer
boundary. |
SET-METH |
Sets the
method for evaluating derivatives for use when computing the optical depth
scale. Options LOGMON, LOGLOG, and ZERO. |
SET-IBC |
Sets
inner boundary condition: DIFFUSION, SCHUSTER, ZERO_FLUX,
HOLLOW. Default is DIFFUSION approximation for stars, and ZERO_FLUX for SN. |
WRFREQ
|
Output
frequencies (in units of 1015 Hz), corresponding to the bound-free
edges of all levels, to EDGE_FREQ.` |
WRN |
Output
summary of model atoms to screen (species & number of levels). |
WRID_* |
Output
summary of levels to screen [LIMS] --- from level LIM(1)
to level LIM(2) Lists level and level name. |
WRTRANS |
Outputs
a summary of all bound-bound wavelengths between 2 wavelength limits (format
as in CMFGEN). |
WRTAB |
Outputs
R, Atom density, T and Tau(Ross) to NEW_TAB |
LNID |
Creates
a line ID file for stars with weak winds. Option selects line for which the
optical depth exceeds some limiting values at tauc=2/3.
Can be read in by PLT_SPEC to identify spectral lines. |
PLNID |
Create
line ID file for plane-parallel models. The list is created based on an
estimate of the central line intensity. The procedure may also work for most
O stars -- especially those with weak winds. It generally does a better job
of identifying lines than does LNID. |
YLOGR |
Plots
log(r/R*) |
CLUMP |
Plots
clumping factor or reciprocal of the clumping factor. [RECIP=T] |
DIFFT |
Plots an
estimate of the diffusion time to the outer boundary (DB=T), or the diffusion
time between grid points (DB=F). |
ED |
Plots log(Electron density). |
T |
Plots T(104 K). |
LOGT |
Plots log(T[104 K]). |
|
|
|
|
DTDP |
Plots dlnT/dlnP |
PGONP |
Plots P(gas)/P(Radiation) as a function of depth (optically
thick approximation). |
DPDR |
Computes 1/ρ dP(gas)/dR. |
DERAD |
Plots
integrated nuclear decay energy as a function of depth. |
EK |
Computes
and plots kinetic energy of outflow (in Lsun). |
EI |
Computes
and plots internal energy of outflow (in Lsun). |
ISOC |
Plots
the isothermal sound speed. |
BEK |
Computes
the bulk kinetic energy of the flow. Useful for SN. It also comoute
VRMS (i.e., the root mean square velocity) in km/s. |
|
|
VEL |
Plots V(km/s)'). |
LOGV |
Plots Log(V(km/s)). |
SIGMA |
Plots Log(dlnv/dlnr)
[log(sigma+1)]. |
|
|
YDEN |
Plots
density (gm/cm^3) |
YCOLD |
Plots log(column density). |
YATOM |
Plots log(N) where N is the (total) atom density. |
YION |
Plots log(Ni) where Ni is the (total) ion density. |
HMIN |
Plots
the LTE population of H-. |
|
|
YROSS |
Plot log(Tau(Ross)). |
SYROSS |
Plot
spherical Rosseland optical depth scale. |
DIEROP |
Plots
the Rosseland mass absorption coefficient against
ρ /T3 . Scaling often used with
opacity tables. |
THOP |
Compute
and plot T computed using the spheric Hopf function. |
|
|
TCMF |
Plot
grey temperature scale computed by CMFGEN *(useful for SN models). |
GREY |
Evaluate
grey temperature structure after first computing Rosseland
mean opacity. X-axis setting is ignored, and T(grey)
is plotted against log(Tauross). You will generally
need to reset the default X-axis after using this option. [ELEC] Plots log(T[grey]). |
TRAT |
Plots
T/TGREY (assumes grey temperature distribution has been created). |
|
|
FONR |
Plots
Flux mean opacity / Rosseland mean opacity. |
CAKT |
Plots
the Castor, Abbott, Klein (1975) t parameter. |
MT |
Plots
the force multiplier. By definition it does not include the force
contribution by electron scattering. However, in the implementation here the
contributions by bound-free and free-free opacities (important at depth), are included. |
YMDOT |
Plot
mass-loss rate at each depth. Useful for model with time dependent mass loss.
|
YAVMODT |
Plots
smoothed mass-loss rate. This is useful for a shell model .
The averaging scale is a free parameter. |
YF |
Plots
volume-filling factor as a function of depth (similar to CLUMP). |
YAVF |
Plots
smoothed volume-filling factor as a function of radius. This is useful for
a shell model. |
YMASS |
Plots
mass (in Msun) of envelope exterior to x(i). |
These
options were more useful in an earlier version, and are generally no longer
used.
HZ_IN |
Switches
frequency input units to 1015 Hz (def) |
KEV_IN |
Switches
frequency input units to KeV |
ANG_IN |
Switches
frequency input units to Angstrom |
XRAY |
Switches
on/off K-shell X ray opacities. |
DIS |
Switches
on/off level dissolution. This option is only for experimenting and testing
--- it generally does not need to be used. Default is set when model is read
in. |
METHOD |
Allows
you to change the method for computing the derivatives (ZERO, LOGLOG, LOGMON)
for use with Euler-McLaurin summation formula. |
LAM |
Wavelength
(Ang) or if neg in units
of 1015 Hz. |
ELEC |
Include
electron scattering opacity? |
|
|
OP |
Plots
the continuum opacity [cm-1] [NOT program units]. |
KAPPA |
Plots
the mass absorption coefficient (cm2/g) |
ETA |
Plots
the continuum emissivity [ergs/cm3/s/Hz]. |
TAUC |
Plots
the continuum optical depth. |
DTAUC |
Plots
the continuum optical depth increments (/\Tau). |
MEANOPAC |
Outputs
opacities, optical depth scales and optical depth increments to file in an
identical format to MEANOPAC created by CMFGEN. |
RAY |
Plots
the Rayleigh scattering opacity due to Hydrogen as a function of depth. |
RAYL |
Plots
the Rayleigh scattering cross section as a function of wavelength. It is
normalized by N(g.s). times the Thompson electron scattering cross-section. |
|
|
CJBB |
Plots
J/BB for continuum against current X axis (def). [TPLT] Set X
axis to log(Tau[continuum]) - X label corrupted. [JONS]
Plot J/S for continuum (F). [JONLY] Plot J |
JEXT |
Allows comparison between J computed using ray-by-ray solution
(NEWJSOLD) on ND grid, and J computed using Eddington
factors (JFEAUNEW) on a more refined depth grid: (ND-1)+1
if ND < 50
2(ND-1)+1 if ND < 80
ND otherwise. The error is defined by: 200(J[E]-J([R]))/(J[e]+J[R])). [LOGE] -
Plots log of absolute value of the error. |
TAUGAM |
Plot the effective absorption optical depth to gamma rays. |
GAMABS |
Plots and compares the gamma-ray energy absorbed as a function
of depth. Requires current_nonlocal_decay_energy.dat. Also plotted is the
energy absorbed assuming a pure absorption approach. |
RTAU |
Computes
R at the given continuum TAU value for a set of user provided frequencies. [LINX] : Determines whether to plot a linear X axis. [LINY] : Determines whether to plot a linear Y axis |
VTAU |
Computes
V at the given continuum TAU value for a set of user provided frequencies |
EDTAU |
Computes
Ne at the given continuum TAU value for a set of user provided frequencies |
ALBEDO |
Plots
the albedo at given continuum TAU. |
TAUR |
Computes
TAU at the given R value for a set of user provided
frequencies. [LINX] : Determines whether to plot a linear X axis. [LINY] : Determines whether to plot a linear Y axis. |
CHIR |
Computes
CHI (cm-1) at a given value of R for a set of user provided
frequencies. |
KAPR |
Computes
KAPPA (cm2/g) at a given value of R for a set of user provided
frequencies. |
ETAR |
Computes
ETA (ergs/cm2/s/Hz) at a given value of R for a set of user
provided frequencies. |
TWOOP |
Plot two
photon opacity or emissivity. |
WRDC |
Output
departure coefficients in CMFGEN format for all species present. These files
may be used as input for CMFGEN. [OWIN] Indicates depths at which
populations are not output. Up to 5 pairs [EXT]
Indicates file extension. For example, EXT=_IN will yield HI_IN, C2_IN
etc. The output files must not exist. |
|
Output
populations for all species present. Same file format and options as for
WRDC. |
WRTX |
Outputs
excitation temperature (relative to ion) for all species. Same file format
and options as for WRDC. Can be read by WR_F_TO_S to create an input
departure file for a new, higher, ionization stage. |
WRLTE |
Writes LTE
populations for all species present in the model. Same file format and
options as for WRDC. |
WRC |
Output
R, T, SIGMA, V, ETA, CHI_TH, ESEC to old format file
(i.e. column format). CHIL and ETAL are set to 1.0E-10. |
WRL_* |
Output
line data for computation of line profiles by other programs. R, T, V, SIGMA,
ETA, CHI, ESEC, ETAL and CHIL are output. Two data formats are available: A
column format for single lines, and a row format for multiple lines. |
I |
2 |
III |
IV |
V |
SIX |
SEV |
VIII |
IX |
X |
XI |
XII |
XIII |
XIV |
XV |
XSIX |
H : HYD |
He : HE |
C : CARB |
N : NIT |
O : OXY |
F :
FLU |
Ne : NEON |
|
Na : SOD |
Mg : MAG |
Al : ALUM |
Sx : SIL |
P : PHOS |
S
: SUL |
Cl : CHL |
Ar : ARG |
K : POT |
Ca : CAL |
Sc : SCAN |
Tx : TIT |
V : VAN |
Cr : CHRO |
Mn : MAN |
Fe : IRON |
Co : COB |
Nk : NICK |
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HI |
H2 |
HeI |
He2 |
HeIII |
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CI |
C2 |
CIII |
CIV |
CV |
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NI |
N2 |
NIII |
NIV |
NV |
NSIX |
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OI |
O2 |
OIII |
OIV |
OV |
OSIX |
OSEV |
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FeI |
Fe2 |
FeIII |
FeIV |
FeV |
FeSIX |
FeSEV |
FeVIII |
FeIX |
FeX |
FeXI |
FeXII |
ALL can
also be used with SOME options.
IF_* |
Plots
the ratio of the population relative to total ion population for each
ionization state. [SPEC_FRAC=T] Plots relative to total species abundance. |
SCL_* |
Scales a
given population by a set factor for all depths beyond some depth K (i.e. for
depths 1 to K). NB: Scale factor should generally be less than unity. To scale
populations between depths L and K only do the following: SCL(SCL_FAX=X,Depth=K) SCL(SCL_FAX=1/X,Depth=L) Option
available to adjust populations for input to CMFGEN. An LTE option should be
issued before calling WRDC. |
YSPEC |
Plots
species population, or log (species_pop/atom_pop). The latter requires [ELEC]=T. |
IMASS |
Plots
mass of a given species, exterior to depth I, against current X coordinate. |
WRID_* |
Output
summary of levels to screen [LIMS] --- from level LIM(1)
to level LIM(2) Lists level and level name. |
DC_* |
Plots
departure coefficients for specified levels. Levels specified as 1,2,3,4,6 or
1:4,6. A maximum of 10 levels can be input. |
DCS |
Plots
departure coefficients of each level as a function of depth. Departure
coefficients at each depth make a single curve --- use symbol option in gramon_pgplot. |
LDC |
Plots
departure coefficient as a function of level at a given depth. |
LPOP |
Plots
population as a function of level at a given depth. |
TPOP |
Plots
radial Sobolev optical depth as function of level
at a given depth (assuming f=1 and no correction for stimulated emission). |
POP_* |
Plots
populations for specified levels. |
RAT_* |
Plots
summed population of species. Can also be used for highest ionization state.
Then Equivalent to D*/. Can be used to indicate in which region a particular
ion is dominant. |
ION_* |
Plots
ionization ratio. Population for any species is summed over all levels in
that species. ION* refers to the * species, and the next ionization stage. |
QF_* |
Computes
the column density for all ionization stages belonging, to a species and for
the atom. If XV is the column density for species XzV,
the program returns XV/X where X is the species column density. Inserted for
comparison with SETI results. |
DION_* |
Plots
the population of highest ionization stage.
e.g., DION_He2 plots He++ |
RR_* |
Computes
integrated recombination coefficient, which can be plotted. Units are such that
the line flux is RR*α/d2/λ
ergs/cm^2/sec. Alpha (α) is the effective recombination rate in units of
10-12, d is the distance
in kpc, and λ is the transition wavelength in μm. [TVAR] Assume recombination rate varies with
T (F). Computed recombination rate is normalized to 104 K. [EXP] Exponent for T variation
(Recombination assumed to vary as T-0.8). |
WLD_* |
Plots
occupation probabilities as a function of depth. |
SOBR_* |
Computes
net rate using Sobolev approximation. |
NETR_* |
Computes
net rate using full CMF solution. If the FORM method is adopted (see below)
J, H, CHI{L}. H, and M {force multiplier} can be
plotted at selected depths. [COL_OPT] Solution method: FORM,
FG, HAM. The FORM method has a large number of
options designed for testing the radiative
transfer. [HAM] Use second order frequency
differencing (F) [SKIPEW] Skip Equivalent Width computation (F).
[EWACC] Required % accuracy of WE
computation (0.05%). If the FG or HAM option is specified, the atomic mass is
taken as 4 for all species. |
MOMR_* |
Similar
to NETR* but use Eddington factors for solution. [HAM] Use second order frequency differencing (F). [FULESS] Include line photons scattered in
resonance zone? (T) [EWACC] Required % accuracy of WE
computation (0.05%). |
|
|
BETA_* |
Computes
Sobolev Escape Probability. |
EW_* |
Computes
the line EW, and plots line formation region or the force multiplier, M(t). EW and line formation region. Options are only
useful for W-R
stars and LBVs. EW takes into account absorption of continuum
radiation by the line when indicating the line formation region -- EP* (an
older option) does not. The parameter plotted on the y-axis is normalized
such that Y.dlogr is the relative contribution to
the EW by the interval dlogr. Thus the formation
zone /EW should generally be plotted against log r. Other x-axis variables
will cause distortion. |
EP_* |
Plots
line formation region.[ELEC] Ignores electron
scattering opacity (T). Preferred option as electron scattering does not
destroy photons. [NEW] Includes
continuum absorption of line photons (T).
[LINV] Plot against linear R scale ? (F) |
DIE_* |
Computes
EW for a dielectronic line (parameters input) |
PROF |
Plot
intrinsic line profiles for a range of temperatures and densities.
FULL_STRK_LIST and Stark files must be linked for the routine to work. |
|
|
SRCE_* |
Plots log(SL) --- SL is the line source function. |
SRCEBB_* |
Plots log(SL/BB) where BB is black body. |
SRCEJC_* |
Plots log(SL/Jc) where Jc is mean continuum intensity. |
CHIL_* |
Line
opacity at line core. Assume a Doppler velocity of 10km/s. |
TAUL_* |
Plots
the Sobolev optical line depth.
[STAT] Computes stationary line optical depth (assuming a Doppler
velocity
of
10km/s and that the macroscopic velocity field is zero). |
CAKT |
Plots
the CAK (Castor, Abbot, and Klein) parameter. |
TAUSOB |
Plots
the Sobolev optical depth scale. Assumes fg=1, and uses the atom density for the level population. |
GF_* |
Plots gf values in a fixed wavelength interval as a function of
wavelength. |
DIST_* |
Plots
the logarithmic Sobolev optical depth (radial or angle
averaged) for every line in a given wavelength interval as a function of the
line wavelength. Lines with a negative optical depth are set to -20. |
NV_ |
Plot the
number of lines with optical depth > TAU_MIN in a given velocity interval
at a specified depth. |
LTAU_* |
Computes
the optical depth of lines of a given ionization stage and species at a given
depth in the atmosphere. Either the radial or tangential Sobolev
optical depth is used. When plotting, use the V mode with the C(onnect) option. Alternatively
it is possible to plot a line strength defined by 10-15 . CHI{Line}
. (10 kms/C) / (sigma Ne). This is a
"mean" line opacity normalized by the electron scattering opacity. |
VLTAU |
Plots a
vertical line, at each line frequency, showing the rang
of velocities over which a line has an optical depth larger than unity.
Currently plots for all species. |
POW_* |
Plots
the number of lines in Log τ or Log (Line strength) space at a given
depth. Each uniform logarithmic bin is 0.25 wide in LOG10 space. For Log
τ space, the line optical depth is normalized by the electron scattering
opacity. |
DCHI |
Creates
an image of the partial opacities (i.e., the opacities due to each ionization
stage) at a given frequency as a function of depth. The images are scaled by
the TOTAL opacity at that depth. |
LCHI |
Creates
an image of the fractional contribution to the opacity as a function of
species and wavelength. |
MCHI_* |
Does one
of two things: 1. Creates an image of the fractional contribution to the
opacity and emissivity of a single species as a function of depth and
wavelength. 2. When no species is specified, the maximum fractional contribution
of each species at ANY depth is output to the terminal. |
ARAT |
Computes
the optical depth of lines of a given ionization stage and species at a given
depth in the atmosphere. Either the radial or tangential Sobolev
optical depth is used. Lines with different A/SUM ranges are plotted in
different colors. |
Designed to fudge populations and temperatures. These fudged
values can be output, and used to restart a model which
is failing to converge.
AV_* |
Replaces
population at a given depth by average population at adjacent depths. |
REP_* |
Replaces
population at a given depth by population at another depth. |
FIXT2 |
Computes
new T distribution based on GREY temperature distribution. GREY option must
be called first. Populations are adjusted under the assumption that the
departure coefficients are constant. The electron density is self-
consistently estimated. Needs to be iterated.
[SCALE] - Optical depth below T remains approximately fixed. |
FIXT |
Old temperature
correction procedure. No adjustment to ED. Must do GREY, FIXT, and finally
LTE option.
[SCALE] - Optical depth below T remains approximately fixed. |
EXTRAP |
Set T(I:J)=T(I:J+1). Over the same range, the populations are
determined assuming the ionization is constant. The LTE populations are
updated. |
LTE |
Re-computes
LTE populations. |
NEWRG |
Creates
a new R grid, equally spaced on some Log τ scale. |
WRRVSIG |
Creates
an RVSIG_COL file. |
SCL_# |
Scales the populations of all levels belonging to a species below some depth (see
under species options). |
TST |
Allows
velocity law to be plotted for different input parameters (e.g, β, Vcore etc). Useful for checking effect of parameters,
smoothness of velocity law etc. |
CHKV |
Estimates
V at some inner radius (r <R*) for the current V(r). |
SM_ |
Smooths
the level populations (or departure coefficients) over depth. Not very
sophisticated. |
MODSUM |
Corrects
the MOD_SUM file for CMFGEN which was corrupted in
versions prior to 01-Sep-199? |
GNTFF |
Computes
free-free gaunt factor for Hydrogenic ion. |
GNTBF |
Computes
bound-free gaunt factor for Hydrogenic ion. |
COL_* |
Computes
and outputs average collision strength, OMEGA(I,J) |
COLR_* |
Computes
collision rates at a specified depth. Net rates, downward rate, of cooling
rate can be output. |
PHOT_* |
Outputs the
photoionization cross-sections at a given frequency, or at the ionization
edge (nu=0). |
PLTPHOT_* |
Plots
the photoionization cross-section for a given level, as a function of λ,
frequency (ν), or normalized frequency (ν/νo).
The differential recombination rate can also be plotted. It can
also plot all cross-sections for the ground state of a given species (e.g., CARB)
as a function of Hz or EV. |
RDDIE_* |
Read in dielectronic lines for resonances not included in the
photoionization cross-section. These will then be included with the
photoionization cross-sections. [DIE_REG] Includes dielectronic
lines from levels permitted to autoionize in LS
coupling? [DIE_WI] Includes dielectronic lines from levels NOT permitted to autoionize in LS coupling? [VSM]
Smoothing width in km/s. |
NRR_* |
Compute
recombination rate for a given species. [PHOT_ID] Photoionization route (1 is normal
default) [EXC_EN] Excitation energy of
final state (cm^-1) [GION]
Statistical weight of lower level. |
RR_* |
Computes
approximate integrated recombination rate (i.e., an emission measure). d=1kpc, and α =10-12 is assumed. Units are
ergs/cm2/s.
[TVAR]
Allow for variation of T [EXP]
Exponent for T variation (generally +ve). (alpha varies as 1/TEXP) |
LAM |
Computes
Lambda for current line frequency. In vacuum for λ < 2000, otherwise
in air. [FREQ]: Frequency for
which lambda required. |
INTERP |
Routine
interpolates and sets Y axis for the last plotted
variable against R (crude). |
CHKV |
Determines
radius (and velocity) where Rosseland optical depth
is τ. [TAU] : Rosseland optical depth at which R and V are to be
determined
(default=100). |
EXIT |
Exit
from display package |
EX |
Exit
from display package |