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The Dynamics of Gas around Active Galactic Nuclei

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dc.contributor.authorDopita, Michael
dc.date.accessioned2015-12-13T23:18:30Z
dc.date.issued2000
dc.date.updated2015-12-12T08:57:05Z
dc.description.abstractThis paper examines the relationship between the accretion flows into the accretion disk around the black holes of active galactic nuclei (AGN), and the jets which they produce. A large-scale accretion flow around the nucleus is proposed as the thick dusty toroid structure of the unified model. Physically, this is similar to the Kahn 'cocoon star' model. High (super-Eddington) accretion rates into the accretion disk are needed. It is assumed that all black holes produce relativistic jets. However, entrainment of thermal (wind) material into the jet determines the AGN class, radio-loud or radio quiet. The jet interacts with the ambient medium as it expands, generating a cocoon of fast radiative or partially-radiative shocks around it. Such a model can explain both the radio properties and the emission line properties over a wide variety of AGN classes.
dc.identifier.issn0004-640X
dc.identifier.urihttp://hdl.handle.net/1885/90207
dc.publisherKluwer Academic Publishers
dc.sourceAstrophysics and Space Science
dc.titleThe Dynamics of Gas around Active Galactic Nuclei
dc.typeJournal article
local.bibliographicCitation.lastpage89
local.bibliographicCitation.startpage79
local.contributor.affiliationDopita, Michael, College of Physical and Mathematical Sciences, ANU
local.contributor.authoruidDopita, Michael, u7501303
local.description.embargo2037-12-31
local.description.notesImported from ARIES
local.description.refereedYes
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationMigratedxPub20507
local.identifier.citationvolume272
local.identifier.scopusID2-s2.0-0034410318
local.type.statusPublished Version

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