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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/2455
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dc.contributor.authorNityananda, R.-
dc.contributor.authorNarayan, R.-
dc.date.accessioned2007-05-25T09:25:50Z-
dc.date.available2007-05-25T09:25:50Z-
dc.date.issued1984-
dc.identifier.citationAdvances in Space Research, 1984, Vol.3, p319-321en
dc.identifier.issn0273-1177-
dc.identifier.urihttp://hdl.handle.net/2289/2455-
dc.descriptionRestricted Access. COSPAR, IAU, ESA, et al., Symposium on High-Energy Astrophysics and Cosmology, Pamporovo, Bulgaria, July 18-23, 1983.en
dc.description.abstractThick accretion disks with narrow funnels around massive black holes are considered promising models for active galactic nuclei. These models assumed a supercritical accretion rate and emit collimated beams with super-Eddington luminosities. Approximate calculations of the interaction between the emerging radiation and the walls for an optically thin funnel are made. The results are sensitive to the sound velocity and to the viscosity parameter. They suggest that a significant particle luminosity can accompany the radiation in the super-Eddington case. By applying an Eddington type limit based on mechanical equilibrium to a suitably chosen interior surface in the disk, it is found that energy transport, if radiative, can strongly limit the efficiency of these models.en
dc.format.extent116502 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherElsevier B.V.en
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/bib_query?1984AdSpR...3..319Nen
dc.relation.urihttp://dx.doi.org/10.1016/0273-1177(84)90109-1en
dc.rights1984 Elsevier B.V.en
dc.subjectACCRETION DISKSen
dc.subjectGALACTIC NUCLEIen
dc.subjectACTIVE GALACTIC NUCLEIen
dc.subjectBLACK HOLES (ASTRONOMY)en
dc.subjectLUMINOSITYen
dc.subjectOPTICAL THICKNESSen
dc.subjectRADIATIVE TRANSFERen
dc.titleThe relevance of the Eddington limit to thick accretion disksen
dc.typeArticleen
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