Really focused stellar winds in X-ray binaries

Abstract

We investigate the anisotropy of stellar winds in binaries to improve the models of accretion in high-mass X-ray binaries. We model numerically the stellar wind from a supergiant component of a binary in radial and three-dimensional radiation hydrodynamic approximation taking into account the Roche potential, Coriolis force, and radiative pressure in the continuum and spectral lines. The Coriolis force influences substantially the mass loss and thus also the accretion rate. The focusing of the stellar wind by the gravitational field of the compact companion leads to the formation of a gaseous tail behind the companion.

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References in corpus (3)

• General relativistic radiation hydrodynamics of accretion flows. I: Bondi-Hoyle accretion
• Stellar Wind Variations During the X-ray High and Low States of Cygnus X-1
• Revisiting the Flip-Flop Instability of Hoyle-Lyttleton Accretion

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