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Observations and Evolutionary Scenario For Be/X-Ray Binaries

Published online by Cambridge University Press:  23 September 2016

G.M.H.J. Habets
G.M.H.J. Habets*
Affiliation:
Sterrewacht ‘Sonnenborgh', Rijksuniversiteit Utrecht, Zonnenburg 2, 3512 NL Utrecht, The Netherlands

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Rappaport & Van den Heuvel (1982) suggested the following formation scenario for B emission (Be)/X-ray binaries: the progenitor of the neutron star is the initial primary star with mass M1 = 10-20 M⊙, which during hydrogen-shell burning transfers mass to the companion (with M2 < M1). The secondary is spun up due to disk-accretion (e.g. Packet 1981) and has become a rapidly rotating Be star (M ≃ 10-20 M⊙).

With this scenario the observed orbital periods (Porb > 15 d) of the Be/X-ray binaries can be explained. This was shown by van den Heuvel (1983) by adopting an idealized period distribution for unevolved O- and B-type close binaries with Porb, < 30 d (see Fig. 1) and assuming conservative evolution, i.e. that mass and angular momentum are conserved during mass transfer.

Type
V. Evolutionary Status of Be Stars
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 509 - 513
Copyright
Copyright © Cambridge University Press 1987

References

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