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Observational properties of relativistic black hole winds

Published online by Cambridge University Press:  01 August 2006

Ken-ya Watarai
Ken-ya Watarai*
Affiliation:
Department of Education, Osaka Kyoiku University, 82-8582, Osaka, Japan email: watarai@cc.osaka-kyoiku.ac.jp
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Abstract

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We examine observational properties of relativistic black hole winds as an origin of high luminosity sources such as microquasars and ultra-luminous X-ray sources (ULXs). When strong relativistic wind/outflow happens in the vicinity of the black hole, the wind might form the optically-thick photosphere. Therefore the emission observed in ULXs might come from the photosphere of the wind, not from the accretion disk.

We found that the location of the photosphere is larger than the disk thickness for super-Eddington mass-outflow rates and sub-relativistic wind velocities (v ∼ 0.1–0.2 c). To understand the radiative structure in the high luminosity sources, we should take into account not only the emission from the accretion disk but also the emission from the outflow at the same time.

Keywords

Black hole physics – stars: windsoutflows – X-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 471 - 472
Copyright
Copyright © International Astronomical Union 2007

References

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