Astronomy and Astrophysics – Astrophysics
Scientific paper
1998-04-16
Astronomy and Astrophysics
Astrophysics
Accepted for publication in A&A. 11 pages, including 11 encapsulated figures. Stellar evolution models available at ftp://ob
Scientific paper
An analysis of some properties of stellar models as a function of metallicity Z (and helium content Y) is presented, with special attention to those stars with metallicities higher than twice or three times solar. It is shown that the stellar properties as a function of Z are mainly determined by the effects of the opacities at sub-solar metallicities, and by the effects of the mean molecular weight and stellar mass loss at higher metallicities. As a result, very metal-rich stars (Z >~0.05) exhibit properties that deviate from what is expected from the known characteristics at lower metallicities. In particular, they are more luminous and hotter than those at Z <~ 0.05 due to the effect of the mean molecular weight. They have main sequence lifetimes much shorter (60 % shorter at Z=0.1 than at Z=0.02) than those at solar metallicity due to their lower initial hydrogen content. Finally, the high mass loss rates at high metallicities affect significantly the population synthesis of massive stars in very metal-rich regions. An analysis of expected Wolf-Rayet and supernovae populations in such conditions is briefly presented.
Charbonnel Corinne
Maeder Andre
Meynet George
Mowlavi Nami
Schaerer Daniel
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