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dc.contributor.authorEsin, Ann A.
dc.contributor.authorKuulkers, Erik
dc.contributor.authorMcClintock, Jeffrey E.
dc.contributor.authorNarayan, Ramesh
dc.date.accessioned2019-09-22T14:24:33Z
dc.date.issued2000
dc.identifier.citationEsin, Ann A., Erik Kuulkers, Jeffrey E. McClintock, and Ramesh Narayan. 2000. “Optical Light Curves of the Black Hole Binaries GRS 1124−68 and A0620−00 in Outburst: The Importance of Irradiation.” The Astrophysical Journal 532 (2): 1069–77. https://doi.org/10.1086/308615.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41384928*
dc.description.abstractWe test whether the model proposed by Esin ct al. to explain X-ray observations of the black hole soft X-ray transient GRS 1124-68 in outburst can also explain the optical light curves of a similar object, A0620-00. We show that to reproduce the observed X-ray to optical flux ratio in A0620-00, we need to assume X-ray irradiation of the outer disk that is significantly in excess of what is expected for a standard planar disk. With enhanced irradiation, the Esin et al. model can reproduce the optical evolution of A0620-00 in outburst very well. Though we find that optical observations of GRS 1124-68 also imply enhanced X-ray heating of the outer disk, the irradiation appears to be a factor of similar to 3 weaker in this system than in A0620-00. This is surprising, since GRS 1124-68 has a larger disk. We speculate that enhanced irradiation may be due to disk warping, and that the degree of warping differs between the two binaries.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleOptical Light Curves of the Black Hole Binaries GRS 1124−68 and A0620−00 in Outburst: The Importance of Irradiation
dc.typeJournal Article
dc.description.versionAccepted Manuscript
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorNarayan, Ramesh::dc7afe5d74d62c7b451015317ea2ccbe::600
dc.date.available2019-09-22T14:24:33Z
dash.workflow.comments1Science Serial ID 95817
dc.identifier.doi10.1086/308615
dash.source.volume532;2
dash.source.page1069-1077


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