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X-Ray Observations of B-Emission Stars (Review Paper)

Published online by Cambridge University Press:  23 September 2016

E.P.J. van den Heuvel  and
S. Rappaport
E.P.J. van den Heuvel
Affiliation:
Astronomical Institute, University of Amsterdam, Roetersstraat 15, 1018 WB Amsterdam, the Netherlands
S. Rappaport
Affiliation:
Department of Physics and Center for Space Research, Massachusetts Institute of Technology, Cambridge, MA, 02139, USA

Abstract

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Most evidence on X-ray emission from the vicinity of Be stars concerns the Be/X-ray binaries. Presently some 20 of these systems are known, making them the most numerous class of massive X-ray binaries. Evidence for the binary nature of these systems comes from (i) Doppler modulation of X-ray pulse periods, (ii) periodic X-ray flaring behavior, and (iii) correlated optical and X-ray variability. The correlation between X-ray pulse period and orbital period found by Corbet (1984) can potentially provide important information on the densities and velocities in the circumstellar disks of Be stars.

Evolutionary models indicate that the Be/X-ray binaries represent a later stage in the evolution of normal close binaries with initial primary masses predominantly in the the range 8 to 15 M⊙ . These models indicate that also a class of slightly less massive Be star binaries should exist in which the compact companions are white dwarfs. Be-type blue stragglers in galactic clusters may be such systems.

Type
III. The Circumstellar Gas
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 291 - 308
Copyright
Copyright © Cambridge University Press 1987

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