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Article: A strongly magnetized strange star model for soft gamma-ray repeaters

TitleA strongly magnetized strange star model for soft gamma-ray repeaters
Authors
Issue Date2002
PublisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/astropartphys
Citation
Astroparticle Physics, 2002, v. 16 n. 3, p. 277-284 How to Cite?
AbstractSoft γ-ray repeaters (SGRs) have been currently argued as super-strongly magnetized neutron stars (magnetars) with magnetic fields with a few 1014 G. Here we propose an alternate model, in which SGRs are young strange stars with superconducting cores and with poloidal magnetic fields of normal radio pulsars. For SGR 1806 - 20, its magnetic field is taken to be ∼3 × 1013 G in order to match the stellar characteristic timescale and the age of the surrounding supernova remnant (SNR) associated with this burster. The movement of the magnetic flux tubes in these strange stars not only leads to crustal cracking of the stars, giving rise to deconfinement of crustal matter to strange matter, but also to movement of internal magnetic toruses together with the flux tubes. The former process will result in bursting and quiescent emission and the latter process will produce quasi-steady relativistic winds which will power the surrounding SNR. The observed persistent X-ray luminosity, bursting behavior and inferred wind luminosity of SGRs can be explained in this model. The possible relation between the sources of SGRs, anomalous X-ray pulsars and gamma-ray bursts is discussed. © 2002 Elsevier Science B.V. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/80757
ISSN
2015 Impact Factor: 3.425
2015 SCImago Journal Rankings: 1.612
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorDai, ZGen_HK
dc.date.accessioned2010-09-06T08:09:56Z-
dc.date.available2010-09-06T08:09:56Z-
dc.date.issued2002en_HK
dc.identifier.citationAstroparticle Physics, 2002, v. 16 n. 3, p. 277-284en_HK
dc.identifier.issn0927-6505en_HK
dc.identifier.urihttp://hdl.handle.net/10722/80757-
dc.description.abstractSoft γ-ray repeaters (SGRs) have been currently argued as super-strongly magnetized neutron stars (magnetars) with magnetic fields with a few 1014 G. Here we propose an alternate model, in which SGRs are young strange stars with superconducting cores and with poloidal magnetic fields of normal radio pulsars. For SGR 1806 - 20, its magnetic field is taken to be ∼3 × 1013 G in order to match the stellar characteristic timescale and the age of the surrounding supernova remnant (SNR) associated with this burster. The movement of the magnetic flux tubes in these strange stars not only leads to crustal cracking of the stars, giving rise to deconfinement of crustal matter to strange matter, but also to movement of internal magnetic toruses together with the flux tubes. The former process will result in bursting and quiescent emission and the latter process will produce quasi-steady relativistic winds which will power the surrounding SNR. The observed persistent X-ray luminosity, bursting behavior and inferred wind luminosity of SGRs can be explained in this model. The possible relation between the sources of SGRs, anomalous X-ray pulsars and gamma-ray bursts is discussed. © 2002 Elsevier Science B.V. All rights reserved.en_HK
dc.languageengen_HK
dc.publisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/astropartphysen_HK
dc.relation.ispartofAstroparticle Physicsen_HK
dc.rightsAstroparticle Physics. Copyright © Elsevier BV.en_HK
dc.titleA strongly magnetized strange star model for soft gamma-ray repeatersen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0927-6505&volume=16&spage=277&epage=284&date=2002&atitle=A+strongly+magnetized+strange+star+model+for+soft+gamma-ray+repeatersen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1016/S0927-6505(01)00113-Xen_HK
dc.identifier.scopuseid_2-s2.0-0012126789en_HK
dc.identifier.hkuros66577en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0012126789&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume16en_HK
dc.identifier.issue3en_HK
dc.identifier.spage277en_HK
dc.identifier.epage284en_HK
dc.identifier.isiWOS:000173144000006-
dc.publisher.placeNetherlandsen_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridDai, ZG=7201387760en_HK

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