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Article: A possible energy mechanism for cosmological γ-ray bursts

TitleA possible energy mechanism for cosmological γ-ray bursts
Authors
KeywordsAccretion, Accretion Discs
Black Hole Physics
Galaxies: General
Gamma-Rays: Bursts
Gamma-Rays: Theory
Radiation Mechanisms: Non-Thermal
Issue Date2001
PublisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNR
Citation
Monthly Notices Of The Royal Astronomical Society, 2001, v. 320 n. 2, p. 235-240 How to Cite?
AbstractWe suggest that an extreme Kerr black hole with a mass ∼106M⊙, a dimensionless angular momentum A ∼ 1 and a marginally stable orbital radius rms ∼ 3rs ∼ 1012M6 cm located in a normal galaxy may produce a γ-ray burst (GRB) by capturing and disrupting a star. During the capture period, a transient accretion disc is formed and a strong transient magnetic field ∼2.4 × 109M-1/2 6 G, lasting for rms/c ∼ 30M6 s, may be produced at the inner boundary of the accretion disc. A large amount of rotational energy of the black hole is extracted and released in an ultrarelativistic jet with a bulk Lorentz factor Γ larger than 103 via the Blandford-Znajek process. The relativistic jet energy can be converted into γ-radiation via an internal shock mechanism. The GRB duration should be the same as the lifetime of the strong transient magnetic field. The maximum number of sub-bursts is estimated to be rms/h ∼ (10-102) because the disc material is likely to break into pieces with a size about the thickness of the disc h at the cusp (2rs ≤ r ≤ 3rs). The shortest risetime of the burst estimated from this model is ∼h/Γc ∼ 3 × 10-4Γ-1 3(h/r)-2M6S. The model GRB density rate is also estimated.
Persistent Identifierhttp://hdl.handle.net/10722/174865
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_US
dc.contributor.authorLu, Yen_US
dc.date.accessioned2012-11-26T08:47:52Z-
dc.date.available2012-11-26T08:47:52Z-
dc.date.issued2001en_US
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society, 2001, v. 320 n. 2, p. 235-240en_US
dc.identifier.issn0035-8711en_US
dc.identifier.urihttp://hdl.handle.net/10722/174865-
dc.description.abstractWe suggest that an extreme Kerr black hole with a mass ∼106M⊙, a dimensionless angular momentum A ∼ 1 and a marginally stable orbital radius rms ∼ 3rs ∼ 1012M6 cm located in a normal galaxy may produce a γ-ray burst (GRB) by capturing and disrupting a star. During the capture period, a transient accretion disc is formed and a strong transient magnetic field ∼2.4 × 109M-1/2 6 G, lasting for rms/c ∼ 30M6 s, may be produced at the inner boundary of the accretion disc. A large amount of rotational energy of the black hole is extracted and released in an ultrarelativistic jet with a bulk Lorentz factor Γ larger than 103 via the Blandford-Znajek process. The relativistic jet energy can be converted into γ-radiation via an internal shock mechanism. The GRB duration should be the same as the lifetime of the strong transient magnetic field. The maximum number of sub-bursts is estimated to be rms/h ∼ (10-102) because the disc material is likely to break into pieces with a size about the thickness of the disc h at the cusp (2rs ≤ r ≤ 3rs). The shortest risetime of the burst estimated from this model is ∼h/Γc ∼ 3 × 10-4Γ-1 3(h/r)-2M6S. The model GRB density rate is also estimated.en_US
dc.languageengen_US
dc.publisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNRen_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.subjectAccretion, Accretion Discsen_US
dc.subjectBlack Hole Physicsen_US
dc.subjectGalaxies: Generalen_US
dc.subjectGamma-Rays: Burstsen_US
dc.subjectGamma-Rays: Theoryen_US
dc.subjectRadiation Mechanisms: Non-Thermalen_US
dc.titleA possible energy mechanism for cosmological γ-ray burstsen_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1046/j.1365-8711.2001.03930.xen_US
dc.identifier.scopuseid_2-s2.0-0041761729en_US
dc.identifier.hkuros56353-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0041761729&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume320en_US
dc.identifier.issue2en_US
dc.identifier.spage235en_US
dc.identifier.epage240en_US
dc.identifier.isiWOS:000166574700005-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridLu, Y=7405476987en_US

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