Where Are Be/black-hole Binaries?

Abstract

We apply the tidal truncation model proposed by Negueruela & Okazaki(2001) to arbitrary Be/compact star binaries to study the truncation efficiency dependance on the binary parameters. We find that the viscous decretion disks around the Be stars could be truncated very effectively in narrow systems. Combining this with the population synthesis results of Podsiadlowski, Rappaport and Han (2003) that binary black holes are most likely to be born in systems with orbital periods less than about 30 days, we suggest that most of the Be/black-hole binaries may be transient systems with very long quiescent states. This could explain the lack of observed Be/black-hole X-ray binaries. We also discuss the evolution of the Be/black-hole binaries and their possible observational features.

14 pages,3 figures, ApJ accepted

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• Population Synthesis of Black Hole X-Ray Binaries
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• On the neutron star-disc interaction in Be/X-ray binaries
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• Suzaku Observation of Be/X-ray Binary Pulsar EXO 2030+375
• Whispering in the dark: Faint X-ray emission from black holes with OB star companions
• Simulating the X-ray luminosity of Be X-ray binaries: the case for black holes versus neutron stars
• Populations of evolved massive binary stars in the Small Magellanic Cloud II: Predictions from rapid binary evolution
• Long-term Optical Studies of the Be/X-ray Binary RX J0440.9+4431/LS V+44 17
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• Identifying four $INTEGRAL$ sources in the Galactic Plane via VLT/optical and $XMM$-$Newton$/X-ray spectroscopy
• LS I+61 303: microquasar or not microquasar?
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