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Massive stellar models: rotational evolution, metallicity effects

Published online by Cambridge University Press:  12 July 2011

Sylvia Ekström ,
Cyril Georgy ,
Georges Meynet ,
André Maeder  and
Anahí Granada
Sylvia Ekström
Affiliation:
Geneva Observatory, University of GenevaMaillettes 51 - Sauverny, CH-1290 Versoix, Switzerland
Cyril Georgy
Affiliation:
Geneva Observatory, University of GenevaMaillettes 51 - Sauverny, CH-1290 Versoix, Switzerland
Georges Meynet
Affiliation:
Geneva Observatory, University of GenevaMaillettes 51 - Sauverny, CH-1290 Versoix, Switzerland
André Maeder
Affiliation:
Geneva Observatory, University of GenevaMaillettes 51 - Sauverny, CH-1290 Versoix, Switzerland
Anahí Granada
Affiliation:
Geneva Observatory, University of GenevaMaillettes 51 - Sauverny, CH-1290 Versoix, Switzerland Instituto de Astrofísica de La Plata, Universidad Nacional de La Plata, Paseo del Bosque S/N, La Plata, Buenos Aires, Argentina
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Abstract

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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.

Keywords

stars: evolutionstars: rotationstars: windsoutflowsstars: mass lossstars: emission-lineBe

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