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VI/89A Radiative forces for stellar envelopes (Seaton, 1997)
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drwxr-xr-x 141 cats archive 4096 Sep 6 2023 [Up]
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Beginning of ReadMe :VI/89A Radiative forces for stellar envelopes (Seaton, 1997)
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Opacities for stellar envelopes
Seaton M.J., Yan Y., Mihalas D., Pradhan A.K.
<Mon. Not. R. Astron. Soc. 266, 805 (1994)>
=1994MNRAS.266..805S (SIMBAD/NED BibCode) (SYMP)
Fitting and smoothing of opacity data
Seaton M.J.
<Mon. Not. R. Astron. Soc. 265, L25 (1993)> (OPF)
=1993MNRAS.265L..25S (SIMBAD/NED BibCode)
Atomic data for opacity calculations: XXII. Computations for 2472790
multiplet gf-values in Fe VIII to Fe XIII
Lynas-Gray A.E., Seaton M.J., Storey, P.J.
<J. Phys. B, 28-14, 2817 (1995)>
=1995JPhB...28.2817L
Interpolation of Rosseland-mean opacities for variable X and Z
Seaton, M.J.
<Mon. Not. R. Astron. Soc. 279, 95 (1996)> (IXZ)
=1996MNRAS.279...95S
Radiative forces in stellar envelopes
Seaton M.J.
<Mon. Not. R. Astron. Soc. 289, 700, (1997)>
=1997MNRAS.289..700S
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ADC_Keywords: Atomic physics ; Models, atmosphere
Keywords: Opacities, radiative accelerations, stellar envelopes, diffusion
References:
Opacities from the Opacity Project. For general description see
M.J. Seaton, Yu Yan, D. Mihalas and Anil K. Pradhan,
1994MNRAS.266..805S . This paper will be referred to as SYMP.
For interpolation of opacities as functions of temperature
and density see M.J. Seaton, 1993MNRAS.265L..25S .
This paper will be referred to as OPF.
For interpolations of opacities as functions of X (hydrogen mass-
fraction) and Z (metals mass-fraction), for fixed relative
abundances of metal atoms, see M.J. Seaton, 1996MNRAS.279...95S .
This paper will be referred to as IXZ.
For the calculation of forces on atoms of individual elements due
to radiation pressure, calculated using atomic data from the
Opacity Project. see M.J. Seaton, 1997MNRAS.289..700S
This paper will be referred to as ACC.
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Description:
(1) Primary data files, stages.zz
These files give data for the calculation of radiative accelerations,
GRAD, for elements with nuclear charge zz.
Data are available for zz=06, 07, 08, 10, 11, 12, 13, 14, 16, 18, 20,
24, 25, 26 and 28. Calculations are made using data from the Opacity
Project (see papers SYMP and IXZ).
The data are given for each ionisation stage, j.
They are tabulated on a mesh of (T, Ne, CHI) where
T is temperature, Ne electron density and CHI is abundance multiplier.
The files include data for ionisation fractions, for each (T, Ne).
The file contents are described in the paper ACC and as comments in
the code add.f
(2) Code add.f
This reads a file stages.zz and creates a file acc.zz giving
radiative accelerations averaged over ionisation stages.
The code prompts for names of input and output files.
The code, as provided, gives equal weights (as defined in the paper
ACC) to all stages.
Th weights are set in SUBROUTINE WEIGHTS, which could be changed
to give any weights preferred by the user.
The dependence of diffusion coefficients on ionisation stage is given
by a function ZET, which is defined in SUBROUTINE ZETA. The
expressions used for ZET are as given in the paper. The user can
change that subroutine if other expressions are preferred. The output
file contains values, ZETBAR, of ZET, averaged over ionisation stages.
(3) Files acc.zz
Radiative accelerations computed using add.f as provided.
The user will need to run the code add.f only if it is required to
change the subroutines WEIGHTS or ZETA.
The contents of the files acc.zz are described in the paper ACC and
in comments contained in the code add.f.
(4) Code accfit.f
This code gives gives radiative accelerations, and some related
data, for a stellar model.
Methods used to interpolate data to the values of (T, RHO) for
the stellar model are based on those used in the code opfit.for
(see the paper OPF).
The executable file accfit.com runs accfit.f.
It uses a list of files given in accfit.files (see that
file for further description).
The mesh used for the abundance-multiplier CHI on the output file
will generally be finer than that used in the input files acc.zz.
The mesh to be used is specified on a file chi.dat.
For a test run, the stellar model used is given in the file
10000_4.2 (Teff=10000 K, LOG10(g)=4.2)
The output file from that test run is acc_10000_4.2.
The contents of the output file are described in the paper ACC and
as comments in the code accfit.f.
(5) The code diff.f
This code reads the output file (e.g. acc_100000_4.2) created
by accfit.f. For any specified depth point in the model
and value of CHI, it gives values of radiative accelerations,
the quantity ZETBAR required for calculation of diffusion
coefficients, and Rosseland-mean opacities.
The code prompts for input data. It creates a file recording
all data calculated.
The code diff.f is intended for incorporation, as a set of
subroutines, in codes for diffusion calculations.