Massive stellar models: rotational evolution, metallicity effects. (En prensa)

EKSTROM, S.; CYRIL GEORGY; GEORGES MEYNET; ANDRE MAEDER; GRANADA, A.

Paris

Simposio; IAU Symposium 272 "Active OB stars: structure, evolution, mass loss and critical limits".; 2010

IAU

Abstract. The Be star phenomenon is related to fast rotation, although the cause of this fast otation is not yet clearly established. The basic effects of fast rotation on the stellar structure ae 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.The Be star phenomenon is related to fast rotation, although the cause of this fast otation is not yet clearly established. The basic effects of fast rotation on the stellar structure ae 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.