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Rotation and Mass Ejection: the Launching of Be-Star Disks

Published online by Cambridge University Press:  26 May 2016

Stanley P. Owocki
Stanley P. Owocki*
Affiliation:
Bartol Research Institute, University of Delaware, Newark, DE 19350 USA Department of Physics and Astronomy, University of Glasgow, Glasgow G12 8QQ UK

Abstract

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The characteristic signature of Be Stars is the Balmer line emission understood to arise in a circumstellar disk. Unlike the accretion disks of protostars or mass-exchange binary systems, the evolved and generally single or wide-binary status of Be Stars seems to require that its disk must form from mass ejection (a.k.a. decretion) from the star itself. In this paper, I use analogies with launching orbital satellites to discuss two candidate processes (radiation, pulsation) for driving such orbital mass ejection, with particular emphasis on the role of the rapid, possibly near-critical, rotation of Be Stars in facilitating the formation of their signature disks.

Type
Session 4 Rotation and Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 515 - 524
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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