Boundary-layer behavior of the flow at the inner edge of black hole accretion disks
We study further the flow of accreting material into black holes from Keplerian disks surrounding them. Solving the system of radial structure equations in Schwarzschild geometry for the case where the kinematic viscosity ..nu..=constant, we discover a boundary layer at the disk's inner edge, where the flow becomes non-Keplerian. We also show that, despite the operation of viscous stresses across the inner edge and the presence of the boundary layer there, very little extra energy or angular momentum is radiated or transported outward from inside that radius--a result many have often assumed but no one has carefully demonstrated. These results constitute a solution to the problem of adequately describing the flow across the inner edge and properly setting the boundary conditions there and at the event horizon.
- Research Organization:
- Department of Physics and Astronomy, University of Maryland, College Park
- OSTI ID:
- 5589466
- Journal Information:
- Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 235:1; ISSN ASJOA
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ANGULAR MOMENTUM
BLACK HOLES
BOUNDARY LAYERS
FIELD THEORIES
FLUID FLOW
FLUID MECHANICS
GENERAL RELATIVITY THEORY
GEODESICS
HYDRODYNAMICS
LAYERS
MECHANICS
RADIAL VELOCITY
STAR ACCRETION
STAR EVOLUTION
VELOCITY
VISCOSITY