Stellar models for a wide range of initial chemical compositions until helium burning

Free access article

Issue		Astron. Astrophys. Suppl. Ser. Volume 133, Number 1, November_II 1998


Page(s)		123 - 127
DOI		http://dx.doi.org/10.1051/aas:1998452

DOI: 10.1051/aas:1998452

Astron. Astrophys. Suppl. Ser. 133, 123-127

IV. From X = 0.65 to X = 0.80, for Z = 0.004

A. Claret ¹ and A. Giménez ^1,2

Send offprint request: A. Claret, e-mail: claret@iaa.es

1 - Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, E-18080 Granada, Spain
2 - Laboratorio de Astrofísica Espacial y Física Fundamental, INTA, Apartado 50727, E-28080 Madrid, Spain

Received March 9; accepted May 15, 1998

Abstract:

As a continuation of previous papers in a series devoted to the computation of stellar structure and evolution models we present a grid specifically obtained for detailed studies of the stellar content of the Small Magellanic Cloud. The initial metal content has thus been adopted to be Z = 0.004 while the hydrogen content varies from 0.65 to 0.80 leaving as an intermediate value that given by standard laws of enrichment, X = 0.744. Interpolation for different environment is therefore possible with these new models. Other input physics parameters, e.g. convective overshooting, mixing-length, opacities or nuclear reaction rates, have been adopted to be homogeneous with the previously published models in order to facilitate comparative studies.

Key words: binaries: eclipsing -- stars: evolution; interiors; fundamental parameters -- Magellanic Clouds

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