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dc.contributor.authorGammie, Charles
dc.contributor.authorNarayan, Ramesh
dc.contributor.authorBlandford, Roger
dc.date.accessioned2019-09-22T14:24:24Z
dc.date.issued1999
dc.identifier.citationGammie, Charles F., Ramesh Narayan, and Roger Blandford. 1999. “What Is the Accretion Rate in NGC 4258?” The Astrophysical Journal 516 (1): 177–86. https://doi.org/10.1086/307089.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41384922*
dc.description.abstractWe estimate the accretion rate (M) over dot onto the black hole in the nucleus of NGC 4258. The result is model dependent. We find that a thin disk that is flat out to greater than or equal to 2 x 10(3) GM/c(2) (M = black hole mass) and that has inclination equal to that of the masing disk must have (M) over dot similar or equal to 0.01 M-. yr(-1) for consistency with near-infrared data. A thin disk that is warped at similar to 10(3) GM/c(2) requires (M) over dot greater than or similar to 1.5 x 10(-4) M-. yr(-1) for consistency with near-infrared data. Reasonable warp models and the near-infrared data are not consistent with (M) over dot as low as the 7 x 10(-5) alpha M-. yr(-1) proposed by Neufeld & Maloney. An advection-dominated flow model combined with the X-ray data implies (M) over dot similar or equal to 0.01 M-. yr(-1). Consistency with a tight 22 GHz upper limit on the flux from the central source requires a transition radius of similar to(10-100)GM/c(2), although the 22 GHz upper limit may be relaxed by appeal to free-free absorption. Physical conditions in the observed VLBI jet features can also be related to conditions in the inner accretion how. We conclude with a list of observations that might further constrain (M) over dot.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleWhat is the accretion rate in NGC 4258?
dc.typeJournal Article
dc.description.versionAccepted Manuscript
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorNarayan, Ramesh::dc7afe5d74d62c7b451015317ea2ccbe::600
dc.date.available2019-09-22T14:24:24Z
dash.workflow.comments1Science Serial ID 95678
dc.identifier.doi10.1086/307089
dash.source.volume516;1
dash.source.page177


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