dc.contributor.author | Ball, Gregory H. | |
dc.contributor.author | Narayan, Ramesh | |
dc.contributor.author | Quataert, Eliot | |
dc.date.accessioned | 2019-09-22T14:24:40Z | |
dc.date.issued | 2001 | |
dc.identifier.citation | Ball, Gregory H., Ramesh Narayan, and Eliot Quataert. 2001. “Spectral Models of Convection‐dominated Accretion Flows.” The Astrophysical Journal 552 (1): 221–26. https://doi.org/10.1086/320465. | |
dc.identifier.issn | 0004-637X | |
dc.identifier.issn | 1538-4357 | |
dc.identifier.uri | http://nrs.harvard.edu/urn-3:HUL.InstRepos:41384938 | * |
dc.description.abstract | For small values of the dimensionless viscosity parameter, namely alpha less than or similar to0.1, the dynamics of nonradiating accretion hows is dominated by convection; convection strongly suppresses the accretion of matter onto the central object and transports a luminosity similar to (10(-3)-10(-2))Mc(2) from Small to large radii in the flow. A fraction of this convective luminosity is likely to be radiated at large radii via thermal bremsstrahlung emission. We show that this leads to a correlation between the frequency of maximal bremsstrahlung emission and the luminosity of the source, v(peak) proportional to L-2/3. Accreting black holes with X-ray luminosities 10(-4)L(Edd) greater than or similar toL(x) (0.5-10 keV) greater than or similar to 10(-7)L(Edd) are expected to have hard X-ray spectra, with photon indices Gamma similar to 2, and sources with L-x less than or similar to 10(-9)L(Edd) are expected to have soft spectra, with Gamma similar to 3.5. This is testable with Chandra and XMM. | |
dc.language.iso | en_US | |
dc.publisher | American Astronomical Society | |
dash.license | LAA | |
dc.title | Spectral Models of Convection‐dominated Accretion Flows | |
dc.type | Journal Article | |
dc.description.version | Accepted Manuscript | |
dc.relation.journal | The Astrophysical Journal | |
dash.depositing.author | Narayan, Ramesh::dc7afe5d74d62c7b451015317ea2ccbe::600 | |
dc.date.available | 2019-09-22T14:24:40Z | |
dash.workflow.comments | 1Science Serial ID 96095 | |
dc.identifier.doi | 10.1086/320465 | |
dash.source.volume | 552;1 | |
dash.source.page | 221-226 | |