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

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

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26as..105...39f&link_type=abstract

Astronomy and Astrophysics Suppl. 105, 39-45 (1994)

Astronomy and Astrophysics

Astrophysics

102

Stars: Evolution, Stars: Interiors

Scientific paper

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 0.6Msun_ to 9Msun_ and extend from the zero age main sequence (ZAMS) till very advanced evolutionary phases. Specifically, low- and intermediate-mass stars are followed either till the white dwarf (WD) or late stages of the early asymptotic giant branch (AGB) phase, depending 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 are M_HeF_=1.3Msun_ andM_up_=4Msun_, 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 variations 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 clusters and the stellar content of elliptical galaxies. However we warn the reader that, because of the opacity, these models are 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.

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