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Be Star Discs: Inflow or Outflow?

Published online by Cambridge University Press:  12 April 2016

John M. Porter
John M. Porter*
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead L41 1LD.UK

Abstract

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It is assumed that the dynamics of Be star discs is dominated by the effects of viscous stresses. By examining angular momentum transport in discs, we show that many, if not all observed Be star discs should be accretion discs unless (i) the disc is acted upon by another agent (e.g. magnetic fields or the stellar radiation field), or (ii) the disc cools significantly as it flows outwards.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 617 - 620
Copyright
Copyright © Astronomical Society of the Pacific 2000

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