Astron. Astrophys. Suppl. Ser.
Volume 133, Number 1, November II 1998
|Page(s)||123 - 127|
|Published online||15 November 1998|
Stellar models for a wide range of initial chemical compositions until helium burning *
IV. From X = 0.65 to X = 0.80, for Z = 0.004
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
Send offprint request to: A. Claret
Accepted: 15 May 1998
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 while the hydrogen content varies from 0.65 to 0.80 leaving as an intermediate value that given by standard laws of enrichment, . 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
Tables 1-72 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsweb.u-strasbg.fr/Abstract.html
© European Southern Observatory (ESO), 1998