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

In this Paper I present grids for the stellar models with a slightly higher metallic content than in the previous works (\cite[Claret 1995]{ref2}; \cite[Claret & Gimenez 1995]{ref4}), say, Z=0.03. The initial helium abundances in mass are Y_i=0.42, 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 (\cite[Iglesias et al. 1992]{ref6}). For the lower temperatures I have used the results by \cite[Alexander (1992)]{ref1}. Core overshooting was taken into account as well as mass loss. The models presented here cover the mass range between 1 and 40 M_odot. I also compute for all models the internal structure constants $k_j$ and the radius of gyration beta. For the first time the calculation of the tidal constants E_2 and lambda_2, 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. Tables 1-72 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html