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X-Ray Observations of Be Stars

Published online by Cambridge University Press:  14 August 2015

Saul Rappaport  and
Edward P.J. Van Den Heuvel
Saul Rappaport
Affiliation:
Massachusetts Institute of Technology
Edward P.J. Van Den Heuvel
Affiliation:
University of Amsterdam

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Be star binaries with neutron star companions are shown to constitute a major class of X-ray sources. Some general observational and interpretive techniques of X-ray astronomy are reviewed. Data for 12 Be/X-ray binary systems are summarized. The Be/X-ray binaries are found to be systematically wider systems, with lower-mass primaries, and with significantly more transient behavior than the “standard” massive X-ray binaries such as Cen X-3 and SMC X-1. The difference between the two types of X-ray binaries is explained in the context of slightly different evolutionary scenarios for the progenitor binaries. The “standard” massive X-ray binaries result from wind-mass-loss dominated evolution of very massive close binaries, while Be/X-ray binaries probably result from mass-transfer dominated evolution of systems with primary masses ≲ 20 M⊙. The implications of the X-ray observations of Be/X-ray binaries for Be stars in general are discussed.

Type
VI. X-Ray Observations
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 327 - 346
Copyright
Copyright © Reidel 1982 

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