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Article: Clumpy jets from black hole–massive star binaries as engines of fast radio bursts

TitleClumpy jets from black hole–massive star binaries as engines of fast radio bursts
Authors
KeywordsBlack hole physics
Radiation mechanisms: general
Binaries: general
Issue Date2019
PublisherOxford University press, co-published with Royal Astronomical Society. The Journal's web site is located at http://www.oxfordjournals.org/our_journals/mnras/
Citation
Monthly Notices of the Royal Astronomical Society, 2019, v. 483 n. 3, p. 4197-4201 How to Cite?
AbstractWe propose a new model of fast radio bursts (FRBs) based on stellar-mass black hole-massive star binaries. We argue that the inhomogeneity of the circumstellar materials or/and the time varying wind activities of the stellar companion will cause the black hole to accrete at a transient super-Eddington rate. The collision among the clumpy ejecta in the resulted jet could trigger plasma instability. As a result, the plasma in the jet will emit coherent curvature radiation. When the jet cone aims toward the observer, the apparent luminosity can be 10(41)-10(42) erg s(-1). The duration of the resulted flare is similar to millisecond. The high event rate of the observed non-repeating FRBs can be explained. A similar scenario in the vicinity of a supermassive black hole can be used to explain the interval distribution of the repeating source FRB 121102 qualitatively.
Persistent Identifierhttp://hdl.handle.net/10722/269559
ISSN
2017 Impact Factor: 5.194
2015 SCImago Journal Rankings: 2.806
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorYi, S-
dc.contributor.authorCheng, KS-
dc.contributor.authorLuo, R-
dc.date.accessioned2019-04-24T08:10:10Z-
dc.date.available2019-04-24T08:10:10Z-
dc.date.issued2019-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2019, v. 483 n. 3, p. 4197-4201-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/269559-
dc.description.abstractWe propose a new model of fast radio bursts (FRBs) based on stellar-mass black hole-massive star binaries. We argue that the inhomogeneity of the circumstellar materials or/and the time varying wind activities of the stellar companion will cause the black hole to accrete at a transient super-Eddington rate. The collision among the clumpy ejecta in the resulted jet could trigger plasma instability. As a result, the plasma in the jet will emit coherent curvature radiation. When the jet cone aims toward the observer, the apparent luminosity can be 10(41)-10(42) erg s(-1). The duration of the resulted flare is similar to millisecond. The high event rate of the observed non-repeating FRBs can be explained. A similar scenario in the vicinity of a supermassive black hole can be used to explain the interval distribution of the repeating source FRB 121102 qualitatively.-
dc.languageeng-
dc.publisherOxford University press, co-published with Royal Astronomical Society. The Journal's web site is located at http://www.oxfordjournals.org/our_journals/mnras/-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2018 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.-
dc.subjectBlack hole physics-
dc.subjectRadiation mechanisms: general-
dc.subjectBinaries: general-
dc.titleClumpy jets from black hole–massive star binaries as engines of fast radio bursts-
dc.typeArticle-
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hk-
dc.identifier.authorityCheng, KS=rp00675-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1093/mnras/sty3231-
dc.identifier.hkuros297591-
dc.identifier.volume483-
dc.identifier.issue3-
dc.identifier.spage4197-
dc.identifier.epage4201-
dc.identifier.isiWOS:000462280000093-
dc.publisher.placeUnited Kingdom-

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