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arXiv · 0705.1639

Modeling of orbital modulation of Cygnus X-3 by particle simulations

Osmi Vilhu·Pasi Hakala·Linnea Hjalmarsdotter·Diana Hannikainen·Ada Paizis·Michael McCollough
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Abstract

The formation of the circumbinary envelope of Cygnus X-3 was studied by particle simulations of the WR (Wolf Rayet) companion wind. Light curves resulting from electron scattering absorption in this envelope were computed and compared with observed IBIS/ISGRI and BATSE light curves. The matching was relatively good. For reasonable values of binary parameters (masses, inclination) and wind velocities, a stable envelope was formed during a few binary orbits. Assuming approximately 10^-6 solar mass/year for the rate of the WR-wind, the observed light curves and accretion luminosity can be re-produced (assuming Thomson scattering opacity in the ionized He-rich envelope). The illuminated envelope can also model the CHANDRA-spectrum using the photoionizing XSTAR-code. Furthermore, we discuss observed radial velocity curves of IR emission lines in the context of simulated velocity fields and find good agreement.

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Osmi Vilhu, Pasi Hakala, Linnea Hjalmarsdotter, Diana Hannikainen, Ada Paizis, Michael McCollough. 2007-05-11. Modeling of orbital modulation of Cygnus X-3 by particle simulations. https://arxiv.org/abs/0705.1639

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