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dc.contributor.authorIgumenshchev, Igor V.
dc.contributor.authorAbramowicz, Marek A.
dc.contributor.authorNarayan, Ramesh
dc.date.accessioned2019-09-22T14:24:32Z
dc.date.issued2000
dc.identifier.citationIgumenshchev, Igor V., Marek A. Abramowicz, and Ramesh Narayan. 2000. “Numerical Simulations of Convective Accretion Flows in Three Dimensions.” The Astrophysical Journal 537 (1): L27–30. https://doi.org/10.1086/312755.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41384927*
dc.description.abstractAdvection-dominated accretion flows (ADAFs) are known to be convectively unstable for low values of the viscosity parameter a. Two-dimensional axisymmetric hydrodynamic simulations of such flows reveal a radial density profile that is significantly flatter than the rho proportional to r(-3/2) expected for a canonical ADAF. The modified density profile is the result of inward transport of angular momentum by axisymmetric convective eddies. We present three-dimensional hydrodynamic simulations of convective ADAFs that are free of the assumption of axisymmetry. We find that the results are qualitatively and quantitatively similar to those obtained with two-dimensional simulations. In particular the convective eddies are nearly axisymmetric and transport angular momentum inward.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleNumerical Simulations of Convective Accretion Flows in Three Dimensions
dc.typeJournal Article
dc.description.versionAccepted Manuscript
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorNarayan, Ramesh::dc7afe5d74d62c7b451015317ea2ccbe::600
dc.date.available2019-09-22T14:24:32Z
dash.workflow.comments1Science Serial ID 95807
dc.identifier.doi10.1086/312755
dash.source.volume537;1
dash.source.pageL27-L30


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