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Be stars in the X-ray binary context

Published online by Cambridge University Press:  30 December 2019

Thomas Rivinius
Thomas Rivinius*
Affiliation:
ESO — European Organisation for Astronomical Research in the Southern Hemisphere, Casilla 19001, Santiago 19, Chile email: triviniu@eso.org
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Abstract

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Rapidly rotating B-type stars with gaseous mass-loss disks in Keplerian rotation are common central objects in X-Ray binaries. These disks are physically well understood in the framework of the viscous decretion disk, and their typical parameters have been established for a large number of single Be stars in the recent years. According to the current observational evidence, the Be stars and disks found in BeXRBs are well within the boundaries known from single Be stars, i.e., they are normal Be stars. New results have also been obtained on the orbital disk truncation and other tidal effects of the companion objects on the disk.

Keywords

circumstellar matterstars: emission-lineBe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 105 - 113
Copyright
© International Astronomical Union 2019 

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