VI/89A Radiative forces for stellar envelopes (Seaton, 1997)
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 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 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 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 1996MNRAS.279...95S
Radiative forces in stellar envelopes
Seaton M.J.
<Mon. Not. R. Astron. Soc. 289, 700, (1997)>
=1997MNRAS.289..700S 1997MNRAS.289..700S
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 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 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 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 1997MNRAS.289..700S
This paper will be referred to as ACC.
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 acc100004.2.
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. acc1000004.2) 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.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
stages.06 77 14134 Basic data for C (1)
stages.07 80 14769 Basic data for N (1)
stages.08 77 15263 Basic data for O (1)
stages.10 77 16600 Basic data for Ne (1)
stages.11 80 16880 Basic data for Na (1)
stages.12 80 17369 Basic data for Mg (1)
stages.13 80 17950 Basic data for Al (1)
stages.14 80 18439 Basic data for Si (1)
stages.16 80 19409 Basic data for S (1)
stages.18 80 20221 Basic data for Ar (1)
stages.20 80 20831 Basic data for Ca (1)
stages.24 80 21568 Basic data for Cr (1)
stages.25 80 22925 Basic data for Mn (1)
stages.26 80 22043 Basic data for Fe (1)
stages.28 80 23596 Basic data for Ni (1)
acc.06 66 7742 Averaged atomic data for C (2)
acc.07 77 7742 Averaged atomic data for N (2)
acc.08 66 7742 Averaged atomic data for O (2)
acc.10 66 7742 Averaged atomic data for Ne (2)
acc.11 77 7742 Averaged atomic data for Na (2)
acc.12 77 7742 Averaged atomic data for Mg (2)
acc.13 77 7742 Averaged atomic data for Al (2)
acc.14 77 7742 Averaged atomic data for Si (2)
acc.16 77 7742 Averaged atomic data for S (2)
acc.18 77 7742 Averaged atomic data for Ar (2)
acc.20 77 7742 Averaged atomic data for Ca (2)
acc.24 77 7742 Averaged atomic data for Cr (2)
acc.25 77 7742 Averaged atomic data for Mn (2)
acc.26 77 7742 Averaged atomic data for Fe (2)
acc.28 77 7742 Averaged atomic data for Ni (2)
plus.13 56 61795 Data for Fe XIII (6)
plus.14 56 294789 Data for Fe XII (6)
plus.15 56 846292 Data for Fe XI (6)
plus.16 56 1367480 Data for Fe X (6)
plus.17 56 1273210 Data for Fe IX (6)
plus.18 56 730148 Data for Fe VIII (6)
plus.f 76 145 Code to read the "plus" data
add.f 71 322 Code for creation of acc.zz from stages.zz (2)
accfit.f 77 1215 Code for computation of input for diff.f (3)
accfit.com 57 11 Executable file for running accfit.f
accfit.fil 13 4 File names for test run of accfit.f (4)
10000_4.2 48 1129 Stellar model for test run of accfit.f
chi.dat 2 4 CHI mesh for test run of accfit.f
diff.f 72 377 Interactive example of code for
diffusion calculations. (5)
--------------------------------------------------------------------------------
Note (1):
Basic atomic data for element with nuclear charge zz.
Includes data for each ionisation stage.
Note (2): files acc.zz contain atomic data averaged over ionisation stages.
The code add.f creates the files acc.zz from files stages.zz;
it contains information on file contents.
The user will need to run add.f only if changes are made in the
subroutines WEIGHTS or ZETA.
Note (3): the code accfit.f:
Reads: file acc.zz; a file specifying LOG10(T), LOG10(RHO) and
RI=(r/R_star) for a stellar model;
a file specifying output mesh for abundance-multipier CHI.
Gives an output file with data for each depth-point in the model.
Note (4):
The test run is for Ca (zz=20) in a model with
Teff=10000 K, LOG10(g)=4.2.
Note (5): Run interactively. Prompts for:
input file which is output from accfit.f (e.g. acc100004.2);
values of depth-point n in model, and
required value of CHI.
This code is intended for incorporation as set of subroutines
in codes for diffusion calculations.
Note (6): the "plus" data were added in February 2000 (see the
"History" section below). The data can be read with the code
plus.f which includes full documentation.
The data provided includes energy levels and S and L quantum numbers;
parameters for use in EOS calculations; and parameters required for
the calculation of oscillator strengths, line-broadening by electron
impacts, and photo-ionisation cross-sections. Flags indicate whether
levels in plus files have already been included in TOPbase data. All
transitions and photo-ionisation cross-sections included in the plus
files have NOT been included in TOPbase data.
-------------------------------------------------------------------------------
See also:
VI/80 : Opacities from the Opacity Project (Seaton+, 1995)
http://cdsweb.u-strasbg.fr/OP.htx : The Opacity Project at CDS
Author's address:
Mike J. Seaton, University College London
Email:
History:
* 08-Aug-1997: created by Mike J. Seaton [Univ. Coll. London]
* 22-Jan-2000; PLUS Data added
The paper Seaton (1997MNRAS.289..700S 1997MNRAS.289..700S) says that additional atomic
data for iron (the "PLUS" data) "are now available at CDS". The data
are from A.E. Lynas-Gray, P.J. Storey and M.J. Seaton, J. Phys. B.,
28, 2817, 1995 (1995JPhB...28.2817L 1995JPhB...28.2817L). Due to an oversight, those data
were not included earlier in the present directory for anonymous ftp
transfers. They are now included. The data files are plus.nn with
nn=13,14,15,16,17 and 18 (data for Fe XIII to VIII). The data can be
read with the code plus.f which includes full documentation.
(End) Mike J. Seaton [Univ. Coll. London] 22-Feb-2000