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Article: A possible energy mechanism for cosmological γ-ray bursts
Title | A possible energy mechanism for cosmological γ-ray bursts |
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Authors | |
Keywords | Accretion, Accretion Discs Black Hole Physics Galaxies: General Gamma-Rays: Bursts Gamma-Rays: Theory Radiation Mechanisms: Non-Thermal |
Issue Date | 2001 |
Publisher | Blackwell 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? |
Abstract | We 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 Identifier | http://hdl.handle.net/10722/174865 |
ISSN | 2023 Impact Factor: 4.7 2023 SCImago Journal Rankings: 1.621 |
ISI Accession Number ID | |
References |
DC Field | Value | Language |
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dc.contributor.author | Cheng, KS | en_US |
dc.contributor.author | Lu, Y | en_US |
dc.date.accessioned | 2012-11-26T08:47:52Z | - |
dc.date.available | 2012-11-26T08:47:52Z | - |
dc.date.issued | 2001 | en_US |
dc.identifier.citation | Monthly Notices Of The Royal Astronomical Society, 2001, v. 320 n. 2, p. 235-240 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/10722/174865 | - |
dc.description.abstract | We 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.language | eng | en_US |
dc.publisher | Blackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNR | en_US |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en_US |
dc.subject | Accretion, Accretion Discs | en_US |
dc.subject | Black Hole Physics | en_US |
dc.subject | Galaxies: General | en_US |
dc.subject | Gamma-Rays: Bursts | en_US |
dc.subject | Gamma-Rays: Theory | en_US |
dc.subject | Radiation Mechanisms: Non-Thermal | en_US |
dc.title | A possible energy mechanism for cosmological γ-ray bursts | en_US |
dc.type | Article | en_US |
dc.identifier.email | Cheng, KS: hrspksc@hkucc.hku.hk | en_US |
dc.identifier.authority | Cheng, KS=rp00675 | en_US |
dc.description.nature | link_to_OA_fulltext | - |
dc.identifier.doi | 10.1046/j.1365-8711.2001.03930.x | en_US |
dc.identifier.scopus | eid_2-s2.0-0041761729 | en_US |
dc.identifier.hkuros | 56353 | - |
dc.relation.references | http://www.scopus.com/mlt/select.url?eid=2-s2.0-0041761729&selection=ref&src=s&origin=recordpage | en_US |
dc.identifier.volume | 320 | en_US |
dc.identifier.issue | 2 | en_US |
dc.identifier.spage | 235 | en_US |
dc.identifier.epage | 240 | en_US |
dc.identifier.isi | WOS:000166574700005 | - |
dc.publisher.place | United Kingdom | en_US |
dc.identifier.scopusauthorid | Cheng, KS=9745798500 | en_US |
dc.identifier.scopusauthorid | Lu, Y=7405476987 | en_US |
dc.identifier.issnl | 0035-8711 | - |