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Cygnus X-1: X-ray Emission Mechanism and Geometry

Wei Cui·S. N. Zhang·J. H. Swank·X. -M. Hua·K. Ebisawa·T. Dotani
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Abstract

We summarize recent observations of Cyg X-1 during its 1996 state transition. The results favor an emission geometry with a central optically thin corona surrounded by an optically thick, geometrically thin accretion disk. As the soft state is approached, the inner edge of the disk moves closer to the black hole, and the corona shrinks, perhaps due to more efficient cooling. Soft X-rays are from the innermost disk, and inverse-Comptionization by the corona appears to be responsible for the hard X-ray emission. Both Compton reflection and an iron emission line have been observed in both states. They are likely to originate in the inner region of the disk. Also briefly discussed is the theoretical effort to simultaneously model the observed spectral and temporal X-ray properties of Cyg X-1.

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Wei Cui, S. N. Zhang, J. H. Swank, X. -M. Hua, K. Ebisawa, T. Dotani. 1997-11-14. Cygnus X-1: X-ray Emission Mechanism and Geometry. https://arxiv.org/abs/astro-ph/9711166

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