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Dynamics of Self-Accreting Disks in Be Stars

Published online by Cambridge University Press:  12 April 2016

P. Kroll  and
R.W. Hanuschik
P. Kroll
Affiliation:
Sonneberg Observatory, Sternwartestr. 32, D-96515 Sonneberg, Germany
R.W. Hanuschik
Affiliation:
Astronomical Institute, Ruhr-Universität Bochum, D-44780 Bochum, Germany

Abstract

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Be star disks are formed by ejection of stellar matter from the surface of a B star rotating at almost critical velocity. In SPH simulations we find that most of the ejected particles fall back on the stellar surface but those with sufficient angular momentum are able to feed a disk-like structure. Owing to viscous interaction some particles are lifted to larger radii where they carry high angular momentum. Viscous forces also cause a thinning of the initially geometrically thick disk and the final accretion of most of the disk material. Different simulations show how the formation and the extension of the decretion disk depend on the ejection velocity, the viscous parameter α and on how long the source is active. After the outburst the disk thins out more and more, over a timescale much longer than the outburst time.

The simulations are compared to Hα observations of the Be star µ Cen.

Type
Part 10. Accretion Disks and Outflows
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 494 - 497
Copyright
Copyright © Astronomical Society of the Pacific 1997

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