dc.contributor.author Loeb, Abraham dc.contributor.author Narayan, Ramesh dc.contributor.author Raymond, John C. dc.date.accessioned 2019-09-22T14:24:37Z dc.date.issued 2001 dc.identifier.citation Loeb, 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.issn 0004-637X dc.identifier.issn 1538-4357 dc.identifier.uri http://nrs.harvard.edu/urn-3:HUL.InstRepos:41384934 * dc.description.abstract In 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.iso en_US dc.publisher American Astronomical Society dash.license LAA dc.title Does the Mass Accretion Rate Depend on the Radius of the Accreting Star? 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 2019-09-22T14:24:37Z dash.workflow.comments 1Science Serial ID 95998 dc.identifier.doi 10.1086/318913 dash.source.volume 547;2 dash.source.page L151
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