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Nucleosynthesis from massive stars 50 years after B2FH

Published online by Cambridge University Press:  06 November 2008

C. Charbonnel ,
J.-P. Zahn  and
G. Meynet
G. Meynet*
Affiliation:
Geneva Observatory, University of Geneva, 1290 Sauverny, Switzerland
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Abstract

We review some important observed properties of massive stars. Then we discuss how mass loss and rotation affect their evolution and help in giving better fits to observational constraints. Consequences for nucleosynthesis at different metallicities are discussed. 
Mass loss appears to be the key feature at high metallicity, while rotation is likely dominant at low and very low metallicities. We discuss various indications supporting the view that very metal-poor stars had their evolution strongly affected by rotational mixing. Many features, like the origin of primary nitrogen at low metallicity, that of the C-rich extremely metal-poor halo stars, of He-rich stars in massive globular clusters, of the O-Na anticorrelation in globular clusters may be related to the existence of a population of very fast rotating metal-poor stars that we tentatively call the spinstars. A fraction of these spinstars may also be the progenitors of GRB in very metal-poor regions. They may avoid pair instability explosion due to the heavy mass loss undergone during their early evolutionary phases and be, dependent on their frequency, important sources of ionising photons in the early Universe.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 32: Stellar Nucleosynthesis: 50 years after B2FH , 2008 , pp. 187 - 232
Copyright
© EAS, EDP Sciences, 2008

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