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Article: Limits on the Galactic model of gamma-ray bursts
Title | Limits on the Galactic model of gamma-ray bursts |
---|---|
Authors | |
Keywords | Gamma-rays: bursts Stars: neutron |
Issue Date | 1997 |
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, 1997, v. 289 n. 3, p. 681-684 How to Cite? |
Abstract | The Burst and Transient Source Experiment (BATSE) has shown that the sky distribution of gamma-ray bursts (GRBs) is remarkably isotropic but non-uniform, which implies that the observed bursts may occur either in an extended galactic halo or at cosmological distances. For the Galactic origin, Hartmann & Narayan have argued that the rotational energy of neutron stars is insufficient by orders of magnitude to provide the observed burst rate. Here we have calculated the period distribution of dead pulsars and found that the rotational energy of neutron stars may indeed be insufficient to account for the total observed energy of the bursts, because only a small fraction (∼IP/I) of rotational energy can be converted into gamma-rays if GRBs are produced by glitches. Furthermore, it is difficult to establish high-velocity neutron stars as a subclass of observed gamma-ray bursts since the observed burst rate is small, ∼ 10 yr-1. © 1997 RAS. |
Persistent Identifier | http://hdl.handle.net/10722/80882 |
ISSN | 2023 Impact Factor: 4.7 2023 SCImago Journal Rankings: 1.621 |
ISI Accession Number ID | |
References |
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Wei, DM | en_HK |
dc.contributor.author | Cheng, KS | en_HK |
dc.date.accessioned | 2010-09-06T08:11:18Z | - |
dc.date.available | 2010-09-06T08:11:18Z | - |
dc.date.issued | 1997 | en_HK |
dc.identifier.citation | Monthly Notices Of The Royal Astronomical Society, 1997, v. 289 n. 3, p. 681-684 | en_HK |
dc.identifier.issn | 0035-8711 | en_HK |
dc.identifier.uri | http://hdl.handle.net/10722/80882 | - |
dc.description.abstract | The Burst and Transient Source Experiment (BATSE) has shown that the sky distribution of gamma-ray bursts (GRBs) is remarkably isotropic but non-uniform, which implies that the observed bursts may occur either in an extended galactic halo or at cosmological distances. For the Galactic origin, Hartmann & Narayan have argued that the rotational energy of neutron stars is insufficient by orders of magnitude to provide the observed burst rate. Here we have calculated the period distribution of dead pulsars and found that the rotational energy of neutron stars may indeed be insufficient to account for the total observed energy of the bursts, because only a small fraction (∼IP/I) of rotational energy can be converted into gamma-rays if GRBs are produced by glitches. Furthermore, it is difficult to establish high-velocity neutron stars as a subclass of observed gamma-ray bursts since the observed burst rate is small, ∼ 10 yr-1. © 1997 RAS. | en_HK |
dc.language | eng | en_HK |
dc.publisher | Blackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNR | en_HK |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en_HK |
dc.subject | Gamma-rays: bursts | en_HK |
dc.subject | Stars: neutron | en_HK |
dc.title | Limits on the Galactic model of gamma-ray bursts | en_HK |
dc.type | Article | en_HK |
dc.identifier.openurl | http://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0035-8711&volume=289&spage=681&epage=684&date=1997&atitle=Limits+on+the+Galactic+Model+of+Gamma-Ray+Bursts | en_HK |
dc.identifier.email | Cheng, KS: hrspksc@hkucc.hku.hk | en_HK |
dc.identifier.authority | Cheng, KS=rp00675 | en_HK |
dc.description.nature | link_to_OA_fulltext | - |
dc.identifier.doi | 10.1093/mnras/289.3.681 | - |
dc.identifier.scopus | eid_2-s2.0-18444396922 | en_HK |
dc.identifier.hkuros | 28440 | en_HK |
dc.relation.references | http://www.scopus.com/mlt/select.url?eid=2-s2.0-18444396922&selection=ref&src=s&origin=recordpage | en_HK |
dc.identifier.volume | 289 | en_HK |
dc.identifier.issue | 3 | en_HK |
dc.identifier.spage | 681 | en_HK |
dc.identifier.epage | 684 | en_HK |
dc.identifier.isi | WOS:A1997XR49000020 | - |
dc.publisher.place | United Kingdom | en_HK |
dc.identifier.scopusauthorid | Wei, DM=7202908906 | en_HK |
dc.identifier.scopusauthorid | Cheng, KS=9745798500 | en_HK |
dc.identifier.issnl | 0035-8711 | - |