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Article: How do γ-ray bursts associated with supernovae avoid baryon contamination?

TitleHow do γ-ray bursts associated with supernovae avoid baryon contamination?
Authors
Keywords04.70.-S
97.60.Bw
97.60.Jd
98.70.Rz
Issue Date2001
PublisherElsevier 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?
AbstractCurrent 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 Identifierhttp://hdl.handle.net/10722/174674
ISSN
2015 Impact Factor: 3.425
2015 SCImago Journal Rankings: 1.612
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_US
dc.contributor.authorDai, ZGen_US
dc.date.accessioned2012-11-26T08:46:49Z-
dc.date.available2012-11-26T08:46:49Z-
dc.date.issued2001en_US
dc.identifier.citationAstroparticle Physics, 2001, v. 16 n. 1, p. 67-74en_US
dc.identifier.issn0927-6505en_US
dc.identifier.urihttp://hdl.handle.net/10722/174674-
dc.description.abstractCurrent 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.languageengen_US
dc.publisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/astropartphysen_US
dc.relation.ispartofAstroparticle Physicsen_US
dc.rightsAstroparticle Physics. Copyright © Elsevier BV.-
dc.subject04.70.-Sen_US
dc.subject97.60.Bwen_US
dc.subject97.60.Jden_US
dc.subject98.70.Rzen_US
dc.titleHow do γ-ray bursts associated with supernovae avoid baryon contamination?en_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.doi10.1016/S0927-6505(00)00172-9en_US
dc.identifier.scopuseid_2-s2.0-0012166417en_US
dc.identifier.hkuros63712-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0012166417&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume16en_US
dc.identifier.issue1en_US
dc.identifier.spage67en_US
dc.identifier.epage74en_US
dc.identifier.isiWOS:000171063500004-
dc.publisher.placeNetherlandsen_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridDai, ZG=7201387760en_US

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