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dc.contributor.authorBatta, Aldo
dc.contributor.authorRamirez-Ruiz, Enrico
dc.contributor.authorFryer, Chris L.
dc.date.accessioned2017-10-02T16:16:46Z
dc.date.available2017-10-02T16:16:46Z
dc.date.issued2017-09-01
dc.identifier.citationThe Formation of Rapidly Rotating Black Holes in High-mass X-Ray Binaries 2017, 846 (2):L15 The Astrophysical Journalen
dc.identifier.issn2041-8213
dc.identifier.doi10.3847/2041-8213/aa8506
dc.identifier.urihttp://hdl.handle.net/10150/625738
dc.description.abstractHigh-mass X-ray binaries (HMXRBs), such as Cygnus X-1, host some of the most rapidly spinning black holes (BHs) known to date, reaching spin parameters a greater than or similar to 0.84. However, there are several effects that can severely limit the maximum BH spin parameter that could be obtained from direct collapse, such as tidal synchronization, magnetic core-envelope coupling, and mass loss. Here, we propose an alternative scenario where the BH is produced by a failed supernova (SN) explosion that is unable to unbind the stellar progenitor. A large amount of fallback material ensues, whose interaction with the secondary naturally increases its overall angular momentum content, and therefore the spin of the BH when accreted. Through SPH hydrodynamic simulations, we studied the unsuccessful explosion of an 8 M-circle dot pre-SN star in a close binary with a 12 M-circle dot companion with an orbital period of approximate to 1.2 days, finding that it is possible to obtain a BH with a high spin parameter a greater than or similar to 0.8 even when the expected spin parameter from direct collapse is a less than or similar to 0.3. This scenario also naturally explains the atmospheric metal pollution observed in HMXRB stellar companions.
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/2041-8205/846/i=2/a=L15?key=crossref.5cecd83a002ac710af5967941de543eeen
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectbinaries: closeen
dc.subjectsupernovae: generalen
dc.titleThe Formation of Rapidly Rotating Black Holes in High-mass X-Ray Binariesen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Dept Physen
dc.identifier.journalThe Astrophysical Journal Lettersen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-14T00:05:56Z
html.description.abstractHigh-mass X-ray binaries (HMXRBs), such as Cygnus X-1, host some of the most rapidly spinning black holes (BHs) known to date, reaching spin parameters a greater than or similar to 0.84. However, there are several effects that can severely limit the maximum BH spin parameter that could be obtained from direct collapse, such as tidal synchronization, magnetic core-envelope coupling, and mass loss. Here, we propose an alternative scenario where the BH is produced by a failed supernova (SN) explosion that is unable to unbind the stellar progenitor. A large amount of fallback material ensues, whose interaction with the secondary naturally increases its overall angular momentum content, and therefore the spin of the BH when accreted. Through SPH hydrodynamic simulations, we studied the unsuccessful explosion of an 8 M-circle dot pre-SN star in a close binary with a 12 M-circle dot companion with an orbital period of approximate to 1.2 days, finding that it is possible to obtain a BH with a high spin parameter a greater than or similar to 0.8 even when the expected spin parameter from direct collapse is a less than or similar to 0.3. This scenario also naturally explains the atmospheric metal pollution observed in HMXRB stellar companions.


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