Published January 30, 1999
| Submitted
Discussion Paper
Open
Relativistic Accretion
- Creators
-
Blandford, Roger D.
Chicago
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Abstract
A brief summary of the properties of astrophysical black holes is presented. Various modes of accretion are distinguished, corresponding to accretion at rates from well below to well above the Eddington rate. The importance of mass loss is emphasized when the accreting gas cannot radiate and it is asserted that a strong wind is likely to be necessary to carry off mass, angular momentum and energy from the accreting gas. The possible importance of the black hole spin in the formation of jets and in dictating the relative importance of non-thermal emission over thermal radiation is discussed.
Additional Information
I am indebted to Mitch Begelman and Henk Spruit for recent collaboration and to Charles Gammie, Andy Fabian, John Hawley, Mario Livio, Ramesh Narayan, Eve Ostriker, Jim Pringle and Martin Rees for stimulating discussions. Support under NSF contract AST 95-29170 and NASA contract 5-2837 and the Sloan Foundation is gratefully acknowledged. I thank John Bahcall and the Institute for Advanced Study for hospitality during the completion of this paper.Attached Files
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Additional details
- Eprint ID
- 96032
- Resolver ID
- CaltechAUTHORS:20190603-100127969
- NSF
- AST 95-29170
- NASA
- 5-2837
- Alfred P. Sloan Foundation
- Created
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2019-06-03Created from EPrint's datestamp field
- Updated
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2023-06-02Created from EPrint's last_modified field
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