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.
Active OB Stars: Structure, Evolution, Mass Loss, and Critical Limits
- Pub Date:
- July 2011
- stars: evolution;
- stars: rotation;
- stars: winds;
- stars: mass loss;
- stars: emission-line;
- Astrophysics - Solar and Stellar Astrophysics
- 11 pages, 7 figures, to appear in the proceedings of IAUS 272 "Active OB stars: structure, evolution, mass loss and critical limits"