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Be Components in X-Ray Binaries

Published online by Cambridge University Press:  14 August 2015

C. de Loore ,
M. Burger ,
E.L. van Dessel  and
M. Mouchet
C. de Loore
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel
M. Burger
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel
E.L. van Dessel
Affiliation:
Royal Belgian Observatory
M. Mouchet
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel

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The Be X-ray binaries show rather weak and variable X-rays. They can be divided into two types, the transient sources and the permanent sources. Two ranges for the X-ray luminosity Lx can be discerned: a) Lx~1034erg s−1 (X Per, λ Cas, 2S0114+65, all permanent sources); b) Lx~1036erg s−1. They have long periods, hence wide orbits, they ar not eclipsing and their mass loss rates are low. The optical spectra are generally very variable and irregular, masking periodic changes. No optical orbits exist and only for 4U0115+63 an X-ray orbit is known (Rappaport et al.1978). An overview of the Be X-ray binaries with some of their characteristics is given in Table 1.

Type
VI. X-Ray Observations
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 347 - 351
Copyright
Copyright © Reidel 1982 

References

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