Structure around the Inner Edge of Geometrically Thin Accretion Disks
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概要
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In geometrically thin, nearly Keplerian disks, there is an inner edge inside which the gas falls toward the black hole by dynamical instabilitydue to a relativistic effect. The disk structure around this edge isexamined in detail when the geometry is Schwarzschildian and thevertically averaged kinematic viscosity is constant. A steady disk modelis found in which the disk structure changes continuously at the edgefrom a nearly Keplerian structure to a thin non-Keplerian structure ofthe infalling gas. The structure of this transition region is demonstrated.
- Astronomical Society of Japanの論文
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