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Article: A morphological approach to the pulsed emission from soft gamma repeaters

TitleA morphological approach to the pulsed emission from soft gamma repeaters
Authors
KeywordsGamma rays: bursts
Stars: magnetic fields
Stars: neutron
X-rays: stars
Issue Date2008
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2008, v. 677 n. 1, p. 488-494 How to Cite?
AbstractWe present a geometrical methodology to interpret the periodical light curves of soft gamma repeaters based on the magnetar model and the numerical arithmetic of the three-dimensional magnetosphere model for the young pulsars. The hot plasma released by the starquake is trapped in the magnetosphere, and photons are emitted tangentially to the local magnetic field lines. The variety of radiation morphologies in the burst tails and the persistent stages could be well explained by the trapped fireballs on different sites inside the closed field lines. Furthermore, our numerical results suggest that the pulse profile evolution of SGR 1806-20 during the 2004 December 27 giant flare is due to a lateral drift of the emitting region in the magnetosphere. © 2008. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/80751
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorJia, JJen_HK
dc.contributor.authorHuang, YFen_HK
dc.contributor.authorCheng, KSen_HK
dc.date.accessioned2010-09-06T08:09:52Z-
dc.date.available2010-09-06T08:09:52Z-
dc.date.issued2008en_HK
dc.identifier.citationAstrophysical Journal Letters, 2008, v. 677 n. 1, p. 488-494en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/80751-
dc.description.abstractWe present a geometrical methodology to interpret the periodical light curves of soft gamma repeaters based on the magnetar model and the numerical arithmetic of the three-dimensional magnetosphere model for the young pulsars. The hot plasma released by the starquake is trapped in the magnetosphere, and photons are emitted tangentially to the local magnetic field lines. The variety of radiation morphologies in the burst tails and the persistent stages could be well explained by the trapped fireballs on different sites inside the closed field lines. Furthermore, our numerical results suggest that the pulse profile evolution of SGR 1806-20 during the 2004 December 27 giant flare is due to a lateral drift of the emitting region in the magnetosphere. © 2008. The American Astronomical Society. All rights reserved.en_HK
dc.languageengen_HK
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectGamma rays: burstsen_HK
dc.subjectStars: magnetic fieldsen_HK
dc.subjectStars: neutronen_HK
dc.subjectX-rays: starsen_HK
dc.titleA morphological approach to the pulsed emission from soft gamma repeatersen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=677&spage=488&epage=494&date=2008&atitle=A+morphological+approach+to+the+pulsed+emission+from+soft+gamma+repeatersen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1086/529425en_HK
dc.identifier.scopuseid_2-s2.0-42549093155en_HK
dc.identifier.hkuros141997en_HK
dc.identifier.volume677en_HK
dc.identifier.issue1en_HK
dc.identifier.spage488en_HK
dc.identifier.epage494en_HK
dc.identifier.isiWOS:000254754300038-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridJia, JJ=14060347800en_HK
dc.identifier.scopusauthoridHuang, YF=24448042100en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK

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