Formation of black hole x-ray binaries in globular clusters

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dc.citation.epage957en_US
dc.citation.issue2en_US
dc.citation.spage948en_US
dc.citation.volume717en_US
dc.contributor.authorIvanova, Natalia
dc.contributor.authorChaichenets, Semyon
dc.contributor.authorFregeau, John
dc.contributor.authorHeinke, Craig O.
dc.contributor.authorLombardi, James C., Jr. (Jamie)
dc.contributor.authorWoods, Tyrone E.
dc.contributor.avlauthorLombardi, James C., Jr. (Jamie)
dc.contributor.departmentPhysicsen_US
dc.date.accessioned2018-01-22T18:18:52Z
dc.date.available2018-01-22T18:18:52Z
dc.date.issued2010-07-10
dc.description.abstractInspired by the recent identification in extragalactic globular clusters of the first candidate black hole–white dwarf (BH–WD) X-ray binaries, where the compact accretors may be stellar-mass black holes (BHs), we explore how such binaries could be formed in a dynamical environment. We provide analyses of the formation rates via well-known formation channels like binary exchange and physical collisions and propose that the only possibility of forming BH–WD binaries is via coupling these usual formation channels with subsequent hardening and/or triple formation. In particular, we find that the most important mechanism for the creation of a BH–WD X-ray binary from an initially dynamically formed BH–WD binary is mass transfer induced in a triple system via the Kozai mechanism. Furthermore, we find that BH–WD binaries that evolve into X-ray sources can be formed by exchanges of a BH into a WD–WD binary or possibly by collisions of a BH and a giant star. If BHs undergo significant evaporation from the cluster or form a completely detached subcluster of BHs, then we cannot match the observationally inferred production rates even using the most optimistic estimates of formation rates. To explain the observations with stellar-mass BH–WD binaries, at least 1% of all formed BHs, or presumably 10% of the BHs present in the core now, must be involved in interactions with the rest of the core stellar population.en_US
dc.description.versionPublished articleen_US
dc.identifier.citationIvanova, N., Chaichenets, S., Fregeau, J., Heinke, C.O., Lombardi, J.C. Jr., and Woods, T.E. (2010). Formation of black hole x-ray binaries in globular clusters. The Astrophysical Journal 717(2): 948-957. doi: 10.1088/0004-637X/717/2/948en_US
dc.identifier.doi10.1088/0004-637X/717/2/948
dc.identifier.issn0004-637X
dc.identifier.issne1538-4357
dc.identifier.urihttp://hdl.handle.net/10456/45475
dc.language.isoen_USen_US
dc.publisherInstitute of Physicsen_US
dc.relation.ispartofThe Astrophysical Journalen_US
dc.relation.isversionofhttp://dx.doi.org/10.1088/0004-637X/717/2/948en_US
dc.rightsThis article has been accepted for publication in The Astrophysical Journal ©: 2010. Ivanova, N., Chaichenets, S., Fregeau, J., Heinke, C.O., Lombardi, J.C. Jr, and Woods, T.E. Published by the American Astronomical Society. All rights reserved.en_US
dc.subjectgalaxies: star clusters: generalen_US
dc.subjectstars: kinematics and dynamicsen_US
dc.subjectX-rays: binariesen_US
dc.titleFormation of black hole x-ray binaries in globular clustersen_US
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