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dc.contributor.authorLoeb, Abraham
dc.contributor.authorNarayan, Ramesh
dc.contributor.authorRaymond, John C.
dc.date.accessioned2019-09-22T14:24:37Z
dc.date.issued2001
dc.identifier.citationLoeb, Abraham, Ramesh Narayan, and John C. Raymond. 2001. “Does the Mass Accretion Rate Depend on the Radius of the Accreting Star?” The Astrophysical Journal 547 (2): L151–54. https://doi.org/10.1086/318913.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41384934*
dc.description.abstractIn some circumstances, the mass accretion rate (M) over dot (*) onto a compact star may depend not only on external boundary conditions but also on the radius R-* of the accreting star. Writing the dependence as M-* proportional to R-*(p), we estimate p for transient binary systems in a quiescent state. We use the observed luminosities L of binary accreting white dwarfs (R-* similar to 10(9) cm) and neutron stars (R-* similar to 10(6) cm) under similar quiescent conditions and estimate M-* in each system through the relation L approximate to GM(*)M(*)/R-*, where M-* is the mass of the star. From the limited data available, we infer that p similar to 0.9 +/- 0.5 for quiescent binaries. This radial dependence is consistent with radiatively inefficient accretion flows that either are convective or lose mass via a wind.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleDoes the Mass Accretion Rate Depend on the Radius of the Accreting Star?
dc.typeJournal Article
dc.description.versionAccepted Manuscript
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorNarayan, Ramesh::dc7afe5d74d62c7b451015317ea2ccbe::600
dc.date.available2019-09-22T14:24:37Z
dash.workflow.comments1Science Serial ID 95998
dc.identifier.doi10.1086/318913
dash.source.volume547;2
dash.source.pageL151


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