The thickness of accretion α-disks: Theory and observationsстатья

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Дата последнего поиска статьи во внешних источниках: 18 июля 2013 г.

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[1] Suleimanov V. F., Lipunova G. V., Shakura N. I. The thickness of accretion α-disks: Theory and observations // Astronomy Reports. — 2007. — Vol. 51. — P. 549–562. Observations of X-ray binaries indicate substantial half-thicknesses for the accretion disks in these systems (up to h/R 0.25, where h is the disk half-thickness and R its radius), while standard α accretion disks predict appreciably smaller half-thicknesses. We study the theoretical vertical structure of such disks using two independent numerical methods, and show that their maximum half-thicknesses in the subcritical regime cannot exceed h/R 0.1. We consider various reasons for the apparent increase in the disk thickness, the most probable of which is the presence of matter above the disk in the form of a hot corona that scatters hard radiation from the central source and inner parts of the disk. As a result, the observed thickness of the disk and the illumination of its outer parts effectively increase. This mechanism can also explain both the optical-to-X-ray flux ratio in these systems and the observed parameters of eclipsing X-ray binaries. [ DOI ]

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