Sylvia Ekström, Cyril Georgy, Patrick Eggenberger, Georges Meynet, Nami Mowlavi, Aurélien Wyttenbach, Anahí Granada, Thibaut Decressin, Raphael Hirschi, Urs Frischknecht, Corinne Charbonnel
[abridged] Many topical astrophysical research areas, as the properties of
planet host stars, the nature of the progenitors of different types of
supernovae and of gamma ray bursts, the evolution of galaxies, require, in
order to be studied during the whole cosmic history, complete and homogeneous
sets of stellar models at different metallicities. We present here a first set
of models for solar metallicity, where the effects of rotation are accounted
for in a homogeneous way.
We computed a grid of 48 different stellar evolutionary tracks, both rotating
and non-rotating, at Z=0.014, spanning a wide mass range from 0.8 to 120 Msun.
For each of the stellar masses considered, electronic tables provide data for
400 stages along the evolutionary track and at each stage, 43 different
physical data are given. These grids thus provide an extensive and detailed
data basis for comparisons with the observations. The rotating models start on
the ZAMS with a rotation rate Vini/Vcrit=0.40. The evolution is computed until
the end of the central carbon-burning phase, the early AGB phase, or the core
helium-flash for respectively the massive, intermediate, low and very low mass
stars. The initial abundances are those which best fit the observed abundances
of massive stars in the solar neighbourhood and correspond to the solar
abundances as deduced by Asplund and collaborators. Opacities and nuclear
reactions rates are updated. New prescriptions for the mass loss rates are
introduced in particular when stars approach the Eddington and/or the critical
velocity. Atomic diffusion and magnetic braking are accounted for in low-mass
star models. [...]
View original:
http://arxiv.org/abs/1110.5049
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