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Clumped stellar winds in supergiant high-mass X-ray binaries

Published online by Cambridge University Press:  21 February 2013

L. M. Oskinova ,
A. Feldmeier  and
P. Kretschmar
L. M. Oskinova
Affiliation:
Institute for Physics and Astronomy, University of Potsdam, 14476 Potsdam, Germany, email: lida@astro.physik.uni-potsdam.de
A. Feldmeier
Affiliation:
Institute for Physics and Astronomy, University of Potsdam, 14476 Potsdam, Germany, email: lida@astro.physik.uni-potsdam.de
P. Kretschmar
Affiliation:
European Space Astronomy Centre (ESA/ESAC), Science Operations Department, Villanueva de la Cañada, Madrid, Spain
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Abstract

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The clumping of massive star winds is an established paradigm, which is confirmed by multiple lines of evidence and is supported by stellar wind theory. We use the results from time-dependent hydrodynamical models of the instability in the line-driven wind of a massive supergiant star to derive the time-dependent accretion rate on to a compact object in the Bondi-Hoyle-Lyttleton approximation. The strong density and velocity fluctuations in the wind result in strong variability of the synthetic X-ray light curves. Photoionization of inhomogeneous winds is different from the photoinization of smooth winds. The degree of ionization is affected by the wind clumping. The wind clumping must also be taken into account when comparing the observed and model spectra of the photoionized stellar wind.

Keywords

accretioninstabilitiesstars: mass lossX-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 287 - 288
Copyright
Copyright © International Astronomical Union 2013

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