Massive stellar models: rotational evolution, metallicity effects

dc.creatorEkström, Sylvia
dc.creatorGeorgy, Cyril
dc.creatorMeynet, Georges
dc.creatorMaeder, André
dc.creatorGranada, Anahí
dc.date2011-07-12
dc.date2019-10-25T13:40:56Z
dc.identifierhttp://sedici.unlp.edu.ar/handle/10915/84049
dc.identifierissn:1743-9213
dc.descriptionThe 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.
dc.descriptionInstituto de Astrofísica de La Plata
dc.formatapplication/pdf
dc.format62-72
dc.languageen
dc.rightshttp://creativecommons.org/licenses/by-nc-sa/4.0/
dc.rightsCreative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.subjectCiencias Astronómicas
dc.subjectCiencias Exactas
dc.subjectBe
dc.subjectOutflows
dc.subjectStars: emission-line
dc.subjectStars: evolution
dc.subjectStars: mass loss
dc.subjectStars: rotation
dc.subjectStars: winds
dc.titleMassive stellar models: rotational evolution, metallicity effects
dc.typeArticulo
dc.typePreprint


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