Evolutionary sequences of stellar models with very high metallicity. V. Z=0.1

We present detailed tabulations of a large grid of stellar models with initial chemical compositions [Y = 0.475, Z = 0.1] computed with the radiative opacities by Huebner et al. (1977) and convective overshoot. This choice of the opacity is due to the high metallicity in use, because the Livermore Library of radiative opacities (Iglesias et al. 1992) did not contain tabulations for Z = 0.1. The tracks span the range of initial masses from 0.6 M. to 9 M. and extend from the zero age main sequence (ZAMS) till very advanced evolutionary phases. Specifically, low- and intermediate-mass stars axe followed either till the white dwarf (WD) or late stages of the early asymptotic giant branch (AGB) phase, depencling on the mass of the star and on details of the evolutionary behaviour discussed in the text. Massive stars are calculated till core C-ignition. The critical masses separating low- from intermediate-, and intermediate-mass from massive stars axe M(HeF) = 1.3 M. and M(up) = 4 M., respectively. All the models are calculated at constant mass. The results for all the models are given in extensive tables which summarize also the lifetimes of the various phases and the vaxiations of the surface abundances limited to the first dredge-up. The stellar models presented here are particularly suited to interpret the CMDs of very metal-rich dusters and the stellar content of elliptical galaxies. However we warn the reader that, because of the opacity, these models axe not fully homogeneous with the others of the same series by Bressan et al. (1993) and Fagotto et al. (1994a,b) that are calculated with the Livermore opacity.