Astron. Astrophys. Suppl. Ser.
Volume 125, Number 3, November I 1997
|Page(s)||439 - 443|
|Published online||15 November 1997|
Stellar models for a wide range of initial chemical compositions until helium burning *
III. From X = 0.55 to X = 0.75, for Z = 0.03
Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, E-18080 Granada, Spain
Send offprint request to: A. Claret
Accepted: 24 January 1997
In this Paper I present grids for the stellar models with a slightly higher metallic content than in the previous works (Claret 1995; Claret & Giménez 1995), say, . The initial helium abundances in mass are , 0.32 and 0.22; this last value was used only to facilitate interpolations since it is a little bit smaller than the primordial helium abundance. The present computations are based on the radiative opacities with spin-orbit coupling provided by the Lawrence Livermore group (Iglesias et al. 1992). For the lower temperatures I have used the results by Alexander (1992). Core overshooting was taken into account as well as mass loss. The models presented here cover the mass range between 1 and . I also compute for all models the internal structure constants kj and the radius of gyration β. For the first time the calculation of the tidal constants E2 and , which are used to evaluate circularization and synchronization times in binary stars, are presented for stellar models as a function of the initial mass and time. The former is related with the dynamical tidal contribution to the total perturbed potential in a binary star while the latter is connected with the external structure of the outer layers.
Key words: stars: binaries: close; evolution; interiors; fundamental parameters; abundances
Tables 1-72 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsweb.u-strasbg.fr/Abstract.html
© European Southern Observatory (ESO), 1997