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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 (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 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. 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) 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). 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
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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