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Article: How do γ-ray bursts associated with supernovae avoid baryon contamination?
Title | How do γ-ray bursts associated with supernovae avoid baryon contamination? |
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Authors | |
Keywords | 04.70.-S 97.60.Bw 97.60.Jd 98.70.Rz |
Issue Date | 2001 |
Publisher | Elsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/astropartphys |
Citation | Astroparticle Physics, 2001, v. 16 n. 1, p. 67-74 How to Cite? |
Abstract | Current hypernova models for γ-ray bursts (GRBs) associated with supernovae suffer from the baryon contamination problem, which prevents formation of relativistic shocks and emission of γ-rays. Here we present a possible solution to this difficulty. Our model can be divided into two steps. In the first step, the core collapse of a star with mass≥19Mȯ leads to a massive neutron star and a supernova (SN), and subsequently, one jet produced via neutrino annihilation during hypercritical accretion of the neutron star will push out of its front matter, resulting in a small cone relatively free of baryons. In the second step, once the mass of the neutron star reaches the maximum value, it will promptly implode to a rapidly rotating black hole surrounded by a torus. The gravitational binding energy of the torus will convert to the expansion energy of the SN ejecta, thus yielding a hypernova, while the rotational energy of the black hole will be extracted via the Blandford-Znajek process to generate another jet responsible for a GRB. We show that the mass of baryons loading with the second jet is smaller than 10-3Mȯ and the Lorentz factor of this jet is larger than 100. Thus our model can avoid the baryon contamination problem suffered from in the hypernova models. © 2001 Elsevier Science B.V. |
Persistent Identifier | http://hdl.handle.net/10722/174674 |
ISSN | 2023 Impact Factor: 4.2 2023 SCImago Journal Rankings: 1.151 |
ISI Accession Number ID | |
References |
DC Field | Value | Language |
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dc.contributor.author | Cheng, KS | en_US |
dc.contributor.author | Dai, ZG | en_US |
dc.date.accessioned | 2012-11-26T08:46:49Z | - |
dc.date.available | 2012-11-26T08:46:49Z | - |
dc.date.issued | 2001 | en_US |
dc.identifier.citation | Astroparticle Physics, 2001, v. 16 n. 1, p. 67-74 | en_US |
dc.identifier.issn | 0927-6505 | en_US |
dc.identifier.uri | http://hdl.handle.net/10722/174674 | - |
dc.description.abstract | Current hypernova models for γ-ray bursts (GRBs) associated with supernovae suffer from the baryon contamination problem, which prevents formation of relativistic shocks and emission of γ-rays. Here we present a possible solution to this difficulty. Our model can be divided into two steps. In the first step, the core collapse of a star with mass≥19Mȯ leads to a massive neutron star and a supernova (SN), and subsequently, one jet produced via neutrino annihilation during hypercritical accretion of the neutron star will push out of its front matter, resulting in a small cone relatively free of baryons. In the second step, once the mass of the neutron star reaches the maximum value, it will promptly implode to a rapidly rotating black hole surrounded by a torus. The gravitational binding energy of the torus will convert to the expansion energy of the SN ejecta, thus yielding a hypernova, while the rotational energy of the black hole will be extracted via the Blandford-Znajek process to generate another jet responsible for a GRB. We show that the mass of baryons loading with the second jet is smaller than 10-3Mȯ and the Lorentz factor of this jet is larger than 100. Thus our model can avoid the baryon contamination problem suffered from in the hypernova models. © 2001 Elsevier Science B.V. | en_US |
dc.language | eng | en_US |
dc.publisher | Elsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/astropartphys | en_US |
dc.relation.ispartof | Astroparticle Physics | en_US |
dc.rights | Astroparticle Physics. Copyright © Elsevier BV. | - |
dc.subject | 04.70.-S | en_US |
dc.subject | 97.60.Bw | en_US |
dc.subject | 97.60.Jd | en_US |
dc.subject | 98.70.Rz | en_US |
dc.title | How do γ-ray bursts associated with supernovae avoid baryon contamination? | 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_subscribed_fulltext | en_US |
dc.identifier.doi | 10.1016/S0927-6505(00)00172-9 | en_US |
dc.identifier.scopus | eid_2-s2.0-0012166417 | en_US |
dc.identifier.hkuros | 63712 | - |
dc.relation.references | http://www.scopus.com/mlt/select.url?eid=2-s2.0-0012166417&selection=ref&src=s&origin=recordpage | en_US |
dc.identifier.volume | 16 | en_US |
dc.identifier.issue | 1 | en_US |
dc.identifier.spage | 67 | en_US |
dc.identifier.epage | 74 | en_US |
dc.identifier.isi | WOS:000171063500004 | - |
dc.publisher.place | Netherlands | en_US |
dc.identifier.scopusauthorid | Cheng, KS=9745798500 | en_US |
dc.identifier.scopusauthorid | Dai, ZG=7201387760 | en_US |
dc.identifier.issnl | 0927-6505 | - |