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Relativistic Accretion

Blandford, Roger D. (1999) Relativistic Accretion. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20190603-100127969

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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.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
https://arxiv.org/abs/astro-ph/9902001arXivDiscussion Paper
ORCID:
AuthorORCID
Blandford, Roger D.0000-0002-1854-5506
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.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFAST 95-29170
NASA5-2837
Alfred P. Sloan FoundationUNSPECIFIED
Record Number:CaltechAUTHORS:20190603-100127969
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190603-100127969
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96032
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:03 Jun 2019 18:44
Last Modified:03 Oct 2019 21:18

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