Add to ORKGThe 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.Instituto de Astrofísica de La Plat
Context. Massive star evolution remains only partly constrained. In particular, the exact role of ro...
Context. Even though it is broadly accepted that single Be stars are rapidly rotating star...
Context.More and more evidence leads to considering classical Be stars as rotating close to the crit...
The Be star phenomenon is related to fast rotation, although the cause of this fast rotation is not ...
Fast rotation seems to be the major factor to trigger the Be phenomenon. Surface fast rotation can b...
New constraints on stellar models are provided by large surveys of massive stars, interferometric ob...
New constraints on stellar models are provided by large surveys of massive stars, interferometric ob...
After a brief review of the observational evidences indicating how the populations of Be stars, red/...
Accepted by A&ASpectroscopic observations of hot stars belonging to the young cluster LMC-NGC 2004 a...
3 pages ; to appear in the proceedings of the Sapporo meeting on active OB stars ; ASP Conference Se...
18 pages, 6 figures, A&A, in pressA sample of 97 galactic field Be stars were studied by taking into...
We discuss the impact of the inclusion of both mass loss and rotation in massive star models at diff...
Mass loss and axial rotation are playing key roles in shaping the evolution of massive stars. They a...
Be stars are thought to be fast rotating stars surrounded by an equatorial disc. The formation, stru...
We search for effects of metallicity on B and Be stars in the Small and Large Magellanic Clouds (SMC...
Context. Massive star evolution remains only partly constrained. In particular, the exact role of ro...
Context. Even though it is broadly accepted that single Be stars are rapidly rotating star...
Context.More and more evidence leads to considering classical Be stars as rotating close to the crit...
The Be star phenomenon is related to fast rotation, although the cause of this fast rotation is not ...
Fast rotation seems to be the major factor to trigger the Be phenomenon. Surface fast rotation can b...
New constraints on stellar models are provided by large surveys of massive stars, interferometric ob...
New constraints on stellar models are provided by large surveys of massive stars, interferometric ob...
After a brief review of the observational evidences indicating how the populations of Be stars, red/...
Accepted by A&ASpectroscopic observations of hot stars belonging to the young cluster LMC-NGC 2004 a...
3 pages ; to appear in the proceedings of the Sapporo meeting on active OB stars ; ASP Conference Se...
18 pages, 6 figures, A&A, in pressA sample of 97 galactic field Be stars were studied by taking into...
We discuss the impact of the inclusion of both mass loss and rotation in massive star models at diff...
Mass loss and axial rotation are playing key roles in shaping the evolution of massive stars. They a...
Be stars are thought to be fast rotating stars surrounded by an equatorial disc. The formation, stru...
We search for effects of metallicity on B and Be stars in the Small and Large Magellanic Clouds (SMC...
Context. Massive star evolution remains only partly constrained. In particular, the exact role of ro...
Context. Even though it is broadly accepted that single Be stars are rapidly rotating star...
Context.More and more evidence leads to considering classical Be stars as rotating close to the crit...