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Equatorial mass loss from Be stars

Georgy, Cyril ; Ekström, Sylvia ; Granada, Anahí ; Meynet, Georges

In: Proceedings of the International Astronomical Union, 2010, vol. 6, no. S272, p. 640-641

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    Title
    • Equatorial mass loss from Be stars
    Author
    • Georgy, Cyril. Geneva University Observatory Chemin des Maillettes 51, 1290 Versoix, Switzerland
    • Ekström, Sylvia. Geneva University Observatory Chemin des Maillettes 51, 1290 Versoix, Switzerland
    • Granada, Anahí. Geneva University Observatory Chemin des Maillettes 51, 1290 Versoix, Switzerland
    • Meynet, Georges. Geneva University Observatory Chemin des Maillettes 51, 1290 Versoix, Switzerland
    Document Type
    • Postprint
    Language
    • English
    Published in
    • Proceedings of the International Astronomical Union, 2010, vol. 6, no. S272, p. 640-641. Cambridge University Press
    Other Version
    OAI-PMH Identifier
    • oai:doc.rero.ch:300345
    Summary
    Be stars are thought to be fast rotating stars surrounded by an equatorial disc. The formation, structure and evolution of the disc are still not well understood. In the frame of single star models, it is expected that the surface of an initially fast rotating star can reach its keplerian velocity (critical velocity). The Geneva stellar evolution code has been recently improved, in order to obtain some estimates of the total mass loss and of the mechanical mass loss rates in the equatorial disc during the whole critical rotation phase. We present here the first results of the computation of a grid of fast rotating B stars evolving towards the Be phase, and discuss the first estimates we obtained