Communications from ULO Number 81 
Supplementary  material for ``Neon abundances in normal late-B and mercury-manganese stars'' by M. M. Dworetsky & J. Budaj, submitted to Monthly Notices of the Royal Astronomical Society on 23 June 2000

Text files for Ne I calculations

This issue of Comms ULO contains text files referenced in the paper on Neon abundances.  We discuss the details of the Ne I abundance calculations and Non-LTE calculations in the main paper.

The first file is an input file of the Ne I data for the Non-LTE calculation.  It is provided in the format used for input data to the Non-LTE code TLUSTY195 of Hubeny (1988), Hubeny & Lanz (1992, 1995),  and Hubeny, Lanz & Jeffery (1995).  This file is given in text form.  It must be added to existing files for other elements included in the calculation, specifically hydrogen.    The Ne I input file was created with the aid of the interface tool MODION written by Varosi et al (1995), which is part of the TLUSTY package.

To save any of the files as a download, with a Web browser either use the `File--save as' pulldown menu after opening the file, or <shift>left-click on the highlighted link and you should be able to save the whole file without viewing it.

tlusty_ne1.dat   Input data for TLUSTY195 for Ne I model

The second file is the Fortran77 program used to calculate the equivalent width ratios LTE/NLTE (Table 7 in the paper).  This is a simple three-way interpolation routine that used the third and fourth files as inputs to set up the grids.  Interpolation is done in the dimensions of effective temperature, surface gravity (as log g[cgs]), and Neon abundance.  The dependence on microturbulence is negligible.  In a few cases in the paper, the authors extrapolated slightly in Teff  after fixing gravity and abundance parameters.

3dintp.f    Fortran program for interpolation of R, the equivalent width ratio.  This program compiles correctly under Linux with a g77 compiler (g77 v0.5.24).  It is a short program and we think it should compile correctly under any f77 or g77 system, but no guarantees can be given by us for systems we have not tested.  With this program, anyone can use our results to do their own interpolation for any star with a measured Ne I 6402 A equivalent width and use an LTE code to deduce the NLTE abundance by scaling the observed equivalent width.

3dintp.in  Data block read into 3dintp.f

3dintp.in2  Another data block read into 3dintp.f
 

M. M. Dworetsky (University of London Observatory, University College London)
J. Budaj (UCL and Astronomical Institute of the Slovak Academy of Sciences, 05960 Tatranska Lomnica, Slovak Republic)

Acknowledgements

J. Budaj gratefully acknowledges the support of a Royal Society/NATO Fellowship (98B).

References

Hubeny I., 1988, Comput. Phys. Comm., 52, 103
Hubeny I., Lanz T., 1992, Astron. & Astrophys., 262, 501
Hubeny I., Lanz T., 1995, Astrophys. J., 439, 875
Hubeny I., Lanz T., Jeffery, C.S., 1995, Tlusty & Synspec-A User's Guide http://tlusty.gsfc.nasa.gov/
Varosi F., Lanz T., Dekoter A., Hubeny I. & Heap S., 1995, MODION (NASA Goddard SFC) ftp://idlastro.gsfc.nasa.gov/pub/contrib/varosi/modion/
 

3 July 2000