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The Missing Population of Be+Black Hole X-Ray Binaries

Published online by Cambridge University Press:  01 April 2008

Aleksander Sadowski ,
J. Ziółkowski ,
K. Belczyński  and
T. Bulik
Aleksander Sadowski
Affiliation:
Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland email: jz@camk.edu.pl
J. Ziółkowski
Affiliation:
Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland email: jz@camk.edu.pl
K. Belczyński
Affiliation:
Department of Astronomy, New Mexico State University, Frenger Mall, Las Cruces, NM 88003, USA email: kbelczyn@lanl.gov
T. Bulik
Affiliation:
Astronomical Observatory of Warsaw University, Al. Ujazdowskie 4, 00-478 Warsaw, Poland email: tb@astrouw.edu.pl
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Abstract

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At present, 117 Be/neutron star (Be/NS) X-ray binaries (XRBs) are known in the Galaxy and the Magellanic Clouds, but not a single Be/black hole (Be/BH) binary was found so far. We carried out the calculations of stellar population synthesis to investigate the case of the apparently missing population of Be/BH XRBs. According to our calculations, the main reason of this disparity is the fact that within the orbital period range where Be XRBs are found (~10 to ~300 days), these systems are formed predominantly with a NS component. The systems with a BH component are formed predominantly with much longer orbital periods and they are not easy to detect.

Keywords

X-rays: binaries(stars:) binaries: closestars: evolutionstars: emission-lineBe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 399 - 403
Copyright
Copyright © International Astronomical Union 2008

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