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Accretion of stellar winds in high-mass X-ray binaries

Published online by Cambridge University Press:  21 February 2013

Petr Hadrava  and
Jan Čechura
Petr Hadrava
Affiliation:
Astronomical Institute, Academy of Sciences, Prague, Czech Republic email: had@sunstel.asu.cas.cz
Jan Čechura
Affiliation:
Astronomical Institute, Academy of Sciences, Prague, Czech Republic email: had@sunstel.asu.cas.cz Faculty of Mathematics and Physics, Charles University, Prague email: j.cechura@gmail.com
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Abstract

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Our analysis of optical spectroscopy of high-mass X-ray binaries like Cyg X-1 confirms that most of the Balmer-lines emission anticorrelated with the X-ray flux originates from the circumstellar matter between the donor star and the accreting compact component. In order to study its structure and variability and the consequent accretion rate we have developed a 3-D numerical model based on radiation hydrodynamics of the supergiant stellar wind. The results show a non-stationary BHL-accretion on the compact component.

Keywords

Stars: windsoutflowsX-rays: binariesAccretionHydrodynamics

References

Hadrava, P. & Čechura, J. 2012, A&A, 542, A42Google Scholar
Yan, J., Liu, Q. & Hadrava, P. 2008 AJ, 136, 631CrossRefGoogle Scholar