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A New Opacity-Sampling Model Atmosphere Program for Arbitrary Abundances

Published online by Cambridge University Press:  12 April 2016

Robert L. Kurucz
Robert L. Kurucz*
Affiliation:
Harvard-Smithsonian Center for Astrophysics60 Garden Street, Cambridge, Massachusetts 02138

Abstract

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I have developed a new version of my model atmosphere program called ATLAS12. It recognizes more than 1000 species, each in up to 10 isotopic forms, including all ions of the elements up through Zn and the first 5 ions of heavier elements up through Es. The elemental abundances are treated as variable with depth. ATLAS12 has 6 input files of line data containing 58,000,000 atomic and molecular lines. For each line the wavelength, identification, lower energy level, gf, radiative, Stark, and van der Waals damping constants are packed into 16 bytes. At each wavelength point in a frequency integration the profiles of all the significant nearby lines are computed and summed. The program and line files will be distributed in the fall of 1992.

There are no significant differences at A0 between an opacity-sampled model computed with ATLAS12 and opacity-distribution-function model computed with ATLAS9. ATLAS12 allows arbitrary abundances but is slower. The new program can be used to produce improved models for Am and Ap stars that include the effects of millions of lines.

Type
I. General Properties of CP Stars
Information
International Astronomical Union Colloquium , Volume 138: Peculiar versus Normal Phenomena in A-Type and Related Stars , 1993 , pp. 87 - 97
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Adelman, S.J. and Gulliver, A.F. 1990, Ap. J., 348, 712.CrossRefGoogle Scholar
Avrett, E.H., Kurucz, R.L., and Loeser, R. 1984, Bull. A.A.S., 16, 450.Google Scholar
Buser, R. and Kurucz, R.L. 1978, Astr. Ap., 70, 555.Google Scholar
Castelli, F. and Kurucz, R.L. 1992, in this volume.Google Scholar
Cowan, R.D. 1968, J. Opt. Soc. Am., 58, 808.CrossRefGoogle Scholar
Gulliver, A.F., Adelman, S.J., Cowley, C.R., and Fletcher, J.M. 1991, Ap. J., 348, 712.Google Scholar
Hayes, D.S. and Latham, D.W. 1975, Ap. J., 197, 593.CrossRefGoogle Scholar
Kurucz, R.L. 1970, SAO Spec. Rep., 309.Google Scholar
Kurucz, R.L. 1977, SAO Spec. Rep., 374.Google Scholar
Kurucz, R.L. 1979a, Ap. J. Suppl., 40, 1.CrossRefGoogle Scholar
Kurucz, R.L. 1979b, Dudley Observ. Report No. 14, ed. Davis Philip, A.G., 363.Google Scholar
Kurucz, R.L. 1980, Bull. A.A.S., 11, 710.Google Scholar
Kurucz, R.L. 1981, SAO Spec. Rep., 390.Google Scholar
Kurucz, R.L. 1987, in IAU Coll. 95, The Second Conference on Faint Blue Stars eds. Davis Philip, A.G., Hayes, D.S., and Liebert, J.W., L. Davis Press, Schenectady, 129.Google Scholar
Kurucz, R.L. 1991, in Stellar Atmospheres: Beyond Classical Models eds. Crivellari, L., Hubeny, I., and Hummer, D.G., NATO ASI Series, Kluwer, Dordrecht, 440.Google Scholar
Kurucz, R.L. 1992, in IAU Symp. 149, The Stellar Populations of Galaxies eds. Barbuy, B. and Renzini, A., Kluwer, Dordrecht, 225.CrossRefGoogle Scholar
Kurucz, R.L. and Avrett, E.H. 1981, SAO Spec. Rep., 391.Google Scholar
Kurucz, R.L., and Peytremann, E. 1975, SAO Spec. Rep., 362.Google Scholar
Labs, D., Neckel, H., Simon, P.C., and Thuillier, G. 1987, Solar Phys. 107, 203.CrossRefGoogle Scholar
Lester, J.B., Gray, R.O., Kurucz, R.L. 1986, Ap. J. Suppl., 61, 509.CrossRefGoogle Scholar
Muthsam, H. 1979, Astr. Ap., 73, 159.Google Scholar
Neckel, H. and Labs, D. 1984, Solar Phys. 90, 205.CrossRefGoogle Scholar
Peterson, D.M. 1969, SAO Spec. Rep., 293.Google Scholar
Relyea, L.J. and Kurucz, R.L. 1978, Ap. J. Suppl., 37, 45.CrossRefGoogle Scholar
Tug, H., White, N.M., and Lockwood, G.W. 1977, Astr. Ap., 61, 679.Google Scholar