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Massive stellar models: rotational evolution, metallicity effects

Ekström, Sylvia ; Georgy, Cyril ; Meynet, Georges ; Maeder, André ; Granada, Anahí

In: Proceedings of the International Astronomical Union, 2010, vol. 6, no. S272, p. 62-72

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    Titre
    • Massive stellar models: rotational evolution, metallicity effects
    Auteur
    • Ekström, Sylvia. Geneva Observatory, University of Geneva Maillettes 51 - Sauverny, CH-1290 Versoix, Switzerland
    • Georgy, Cyril. Geneva Observatory, University of Geneva Maillettes 51 - Sauverny, CH-1290 Versoix, Switzerland
    • Meynet, Georges. Geneva Observatory, University of Geneva Maillettes 51 - Sauverny, CH-1290 Versoix, Switzerland
    • Maeder, André. Geneva Observatory, University of Geneva Maillettes 51 - Sauverny, CH-1290 Versoix, Switzerland
    • Granada, Anahí. Geneva Observatory, University of Geneva Maillettes 51 - Sauverny, CH-1290 Versoix, Switzerland
    Type de document
    • Postprint
    Langue
    • Inglese
    Publié dans
    • Proceedings of the International Astronomical Union, 2010, vol. 6, no. S272, p. 62-72. Cambridge University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:298291
    Summary
    The Be star phenomenon is related to fast rotation, although the cause of this fast rotation is not yet clearly established. The basic effects of fast rotation on the stellar structure are reviewed: oblateness, mixing, anisotropic winds. The processes governing the evolution of the equatorial velocity of a single star (transport mechanisms and mass loss) are presented, as well as their metallicity dependence. The theoretical results are compared to observations of B and Be stars in the Galaxy and the Magellanic Clouds