Hostname: page-component-586b7cd67f-g8jcs Total loading time: 0 Render date: 2024-11-24T04:08:22.249Z Has data issue: false hasContentIssue false

On the apparent lack of Be X-ray binaries with black holes in the galaxy and in the Magellanic Clouds

Published online by Cambridge University Press:  24 February 2011

Janusz Ziółkowski
Affiliation:
Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland email: [email protected]
Krzysztof Belczyński
Affiliation:
Los Alamos National Lab, P.O. Box 1663, MS 466, Los Alamos, NM 87545 email: [email protected]
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.

In the Galaxy there are 67 Be X-ray binaries known to-date. Out of those, 45 host a neutron star, and for the reminder the nature of a companion is not known. None, so far, is known to host a black hole. This disparity is referred to as a missing Be – black hole X-ray binary problem. The stellar population synthesis calculations following the formation of Be X-ray binaries (Belczyński & Ziółkowski 2009) predict that the ratio of the binaries with neutron stars to the ones with black holes is rather high FNS/BH ~ 30–50. A comparison of this ratio with the number of confirmed Be – neutron star X-ray binaries (45) indicates that the expected number of Be – black hole X-ray binaries is of the order of only ~0–2. This is entirely consistent with the observed Galactic sample. Therefore, there is no problem of the missing Be+BH X-Ray Binaries for the Galaxy

In the Magellanic Clouds there are 94 Be X-ray binaries known to-date. Out of those, 60 host a neutron star. Again, none hosts a black hole. The stellar population synthesis calculations carried out specifically for the Magellanic Clouds (Ziółkowski & Belczyński 2010) predict that the ratio of the Be X-ray binaries with neutron stars to the ones with black holes is only FNS/BH ~ 10. This value is rather too low, as it implies the expected number of Be+BH X-ray binaries of the order of ~6, while none is observed. We found, that to remove the discrepancy, one has to take into account a different history of the star formation rate in the Magellanic Clouds, with the respect to the Galaxy. New stellar population synthesis calculations are currently being carried out.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Belczyński, K., Kalogera, V., Rasio, F. A., Taam, R. E., Zezas, A., Bulik, T., Maccarone, T. J., & Ivanova, N. 2008, ApJ Suppl 174, 223Google Scholar
Belczyński, K. & Ziolkowski, J. 2009, ApJ 707, 870CrossRefGoogle Scholar
Negueruela, I., Okazaki, A. T., Fabregat, J., Coe, M. J., Munari, U. & Tomov, T. 2001, A&A 369, 117Google Scholar
Ziółkowski, J. 2002, Mem. Soc. Astron. Ital. 73, 1038Google Scholar
Ziolkowski, J. & Belczyński, K. 2010, in preparationGoogle Scholar