Hostname: page-component-7c8c6479df-r7xzm Total loading time: 0 Render date: 2024-03-29T11:38:06.779Z Has data issue: false hasContentIssue false

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

Published online by Cambridge University Press:  01 April 2008

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
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

Artymowicz, P. & Lubow, S. H. 1994, ApJ 421, 651CrossRefGoogle Scholar
Belczyński, K., Kalogera, V., & Bulik, T. 2002, ApJ 572, 407Google Scholar
Belczyński, K., Kalogera, V., Rasio, F.A., Taam, R.E., Zezas, A., Bulik, T., Maccarone, T.J., & Ivanova, N. 2008, ApJ Suppl (in press), also astro-ph/051181Google Scholar
Lejeune, T. & Schaerer, D. 2001, A&A 366, 538Google Scholar
McSwain, M.V. & Gies, D.R. 2005, ApJ Suppl 161, 118CrossRefGoogle Scholar
Podsiadlowski, Ph., Rappaport, S., & Han, Z. 2003, MNRAS 341, 385CrossRefGoogle Scholar
Zhang, F., Li, X.-D., & Wang, Z.-R. 2004, ApJ 603, 663CrossRefGoogle Scholar