Structure around the Inner Edge of Geometrically Thin Accretion Disks

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  • Structure Around the Inner Edge of Geom

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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 instability due to a relativistic effect. The disk structure around this edge is examined in detail when the geometry is Schwarzschildian and the vertically averaged kinematic viscosity is constant. A steady disk model is found in which the disk structure changes continuously at the edge from a nearly Keplerian structure to a thin non-Keplerian structure of the infalling gas. The structure of this transition region is demonstrated.

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