Massive stellar models: rotational evolution, metallicity effects

Abstract

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.

11 pages, 7 figures, to appear in the proceedings of IAUS 272 "Active OB stars: structure, evolution, mass loss and critical limits"

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Cited by in corpus (4)

• Low-metallicity massive single stars with rotation. Evolutionary models applicable to I Zwicky 18
• Evolution of rotation in rapidly rotating early-type stars during the main sequence with 2D models
• A systematic study of super-Eddington layers in the envelopes of massive stars
• SILCC -- IX. The multi-phase interstellar medium at low metallicity