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Massive Stars as Cosmic Engines Through the Ages

Maeder, André ; Meynet, Georges ; Ekström, Sylvia ; Hirschi, Raphael ; Georgy, Cyril

In: Proceedings of the International Astronomical Union, 2007, vol. 3, no. S250, p. 3-16

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    Titre
    • Massive Stars as Cosmic Engines Through the Ages
    Auteur
    • Maeder, André. Geneva Observatory, University of Geneva, CH-1290 Sauverny, Switzerland email: andre.maeder@obs.unige.ch, georges.meynet@obs.unige.ch, sylvia.ekstrom@obs.unige.ch, cyril.georgy@obs.unige.ch
    • Meynet, Georges. Geneva Observatory, University of Geneva, CH-1290 Sauverny, Switzerland email: andre.maeder@obs.unige.ch, georges.meynet@obs.unige.ch, sylvia.ekstrom@obs.unige.ch, cyril.georgy@obs.unige.ch
    • Ekström, Sylvia. Geneva Observatory, University of Geneva, CH-1290 Sauverny, Switzerland email: andre.maeder@obs.unige.ch, georges.meynet@obs.unige.ch, sylvia.ekstrom@obs.unige.ch, cyril.georgy@obs.unige.ch
    • Hirschi, Raphael. Astrophysics, EPSAM, University of Keele email: r.hirschi@epsam.keele.ac.uk
    • Georgy, Cyril. Geneva Observatory, University of Geneva, CH-1290 Sauverny, Switzerland email: andre.maeder@obs.unige.ch, georges.meynet@obs.unige.ch, sylvia.ekstrom@obs.unige.ch, cyril.georgy@obs.unige.ch
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Proceedings of the International Astronomical Union, 2007, vol. 3, no. S250, p. 3-16. Cambridge University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:304894
    Summary
    Some useful developments in the model physics are briefly presented, followed by model results on chemical enrichments and WR stars. We discuss the expected rotation velocities of WR stars. We emphasize that the (C+O)/He ratio is a better chemical indicator of evolution for WC stars than the C/He ratios. With or without rotation, at a given luminosity the (C+O)/He ratios should be higher in regions of lower metallicity Z. Also, for a given (C+O)/He ratio the WC stars in lower Z regions have higher luminosities. The WO stars, which are likely the progenitors of supernovae SNIc and of some GRBs, should preferentially be found in regions of low Z and be the descendants of very high initial masses. Finally, we emphasize the physical reasons why massive rotating low Z stars may also experience heavy mass loss