Dynamical Processes in the Formation of Hot-Star Disks

Details Dynamical Processes in the Formation of Hot-Star Disks Dynamical Processes in the Formation of Hot-Star Disks

Nov 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..337..101o&link_type=abstract

The Nature and Evolution of Disks Around Hot Stars, ASP Conference Series, Vol. 337, Proceedings of a meeting held 7-9 July 2004

Physics

19

Scientific paper

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 review, I use analogies with launching orbital satellites to discuss candidate processes (radiation, pulsation, magnetic) 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.

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