A&A Supplement Series, Vol. 125, November I 1997, 439-443
Received October 28, 1996; accepted January 24, 1997
A. Claret
Send offprint request: A. Claret, e-mail:claret@iaa.es
Instituto de Astrofísica de Andalucía, CSIC,
Apartado 3004, E-18080 Granada, Spain
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, Z=0.03. 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 
. 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.
keywords: stars: binaries: close; evolution; interiors; fundamental parameters; abundances