Clumped stellar winds in supergiant high-mass X-ray binaries: X-ray variability and photoionization
Article first published online: 5 MAR 2012
© 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
Monthly Notices of the Royal Astronomical Society
Volume 421, Issue 4, pages 2820–2831, April 2012
How to Cite
Oskinova, L. M., Feldmeier, A. and Kretschmar, P. (2012), Clumped stellar winds in supergiant high-mass X-ray binaries: X-ray variability and photoionization. Monthly Notices of the Royal Astronomical Society, 421: 2820–2831. doi: 10.1111/j.1365-2966.2012.20507.x
- Issue published online: 10 APR 2012
- Article first published online: 5 MAR 2012
- Accepted 2012 January 5. Received 2012 January 5; in original form 2011 July 23
Light curves. Synthetic X-ray light curves for Bondi-Hoyle accretion of a non-stationary stellar wind on to a NS with mX = 1.4 M⊙ for radii in the range 1.5R* to 30R*. The SG donor parameters are given in Table 1. The orbital separation a forms part of the filename. For example, xlc-a02.0.dat is an ASCII file that contains two columns: time and X-ray luminosity. The data in this file are for the orbital separation a = 2.0R*.
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