Clumpy wind accretion in Cygnus X-1

Abstract

Cygnus X-1 is one of the brightest X-ray sources observed and shows the X-ray intensity variations on time scales from milliseconds to months in both the soft and hard X-rays. The accretion onto the black hole is believed to be wind fed due to focused stellar wind from the binary companion HDE-226868. We aim to understand the physical mechanism responsible for the short timescale X-ray variability ($<$100 s) of the source in its Hard/Low state. We compute the 2D relativistic hydrodynamic simulation of the low angular momentum accretion flow with a time dependent outer boundary condition that reflects the focused, clumpy wind from the super-giant in this X-ray binary system. We follow the dynamical evolution of our model for about 100 s and present the results showing an oscillatory shock, being a potential explanation of variability observed in hard X-rays. The simulated model with shock solutions is in good agreement with the observed power density spectra of the source.

arXiv comment16 pages, 10 figures, 2 tables, accepted for publication in ApJ

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Cited by in corpus (4)

• Review the possible advective disk structures around a black hole with two-type gas inflows
• Carter-Penrose diagrams for emergent spacetime in axisymmetrically accreting black hole systems
• On the origin of core radio emissions from black hole sources in the realm of relativistic shocked accretion flow
• Conditions for accretion disc formation and observability of wind-accreting X-ray binaries