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The structure and appearance of winds from supercritical accretion disks. I - Numerical modelsEquations for the structure and appearance of supercritical accretion disks and the radiation-driven winds which emanate from them are derived and solved by a steady-state hydrodynamic computer code with a relaxation technique used in stellar structure problems. The present model takes into account the mass of the accreting star, the total accretion rate, a generalization of the disk alpha parameter which accounts for heating by processes in addition to viscosity, and the ratio of the total luminosity to the Eddington luminosity. Solutions indicate that for accretion onto a hard-surfaced star, steady, optically thick winds result for even slightly supercritical accretion, and the object will appear as a supergiant star with a high mass loss rate and a nonblackbody spectrum. Winds from black hole accretion disks are expected to depend on the form of the accretion interior to the critical radius, possibly consisting of no ejection at all, a wind similar to that of a hard-surfaced star, or a column of material ejected from a hole in the accretion disk.
Document ID
19800026917
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Meier, D. L.
(Texas, University Austin, Tex.; California Institute of Technology, Pasadena, Calif., United States)
Date Acquired
August 10, 2013
Publication Date
October 15, 1979
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
80A11087
Funding Number(s)
CONTRACT_GRANT: NSF AST-76-80801-A01
CONTRACT_GRANT: NSF AST-76-20375
CONTRACT_GRANT: NSG-7232
Distribution Limits
Public
Copyright
Other

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