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Article: The radio afterglow from the giant flare of SGR 1900+14: The same mechanism as afterglows from classic gamma-ray bursts?

TitleThe radio afterglow from the giant flare of SGR 1900+14: The same mechanism as afterglows from classic gamma-ray bursts?
Authors
KeywordsGamma rays: bursts
ISM: jets and outflows
Stars: individual (SGR 1900+14)
Issue Date2003
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2003, v. 593 n. 2 II, p. L85-L88 How to Cite?
AbstractA radio afterglow was detected following the 1998 August 27 giant flare from the soft gamma repeater (SGR) 4900+14. Its short-lived behavior is quite different from the radio nebula of SGR 1806-20, but very similar to radio afterglows from classic gamma-ray bursts (GRBs). Motivated by this, we attempt to explain it with the external shock model as invoked in the standard theory of GRB afterglows. We find that the light curve of this radio afterglow is not consistent with the forward shock emission of an ultrarelativistic outflow, which is suggested to be responsible for the initial hard spike of the giant flare. Nevertheless, shock emission from a mildly or subrelativistic outflow expanding into the interstellar medium could fit the observations. The possible origin for this kind of outflow is discussed, based on the magnetar model for SGRs. Furthermore, we suggest that the presence of an ultrarelativistic fireball from SGR giant flares could be tested by rapid radio to optical follow-up observations in the future.
Persistent Identifierhttp://hdl.handle.net/10722/43396
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorWang, XYen_HK
dc.date.accessioned2007-03-23T04:44:54Z-
dc.date.available2007-03-23T04:44:54Z-
dc.date.issued2003en_HK
dc.identifier.citationAstrophysical Journal Letters, 2003, v. 593 n. 2 II, p. L85-L88en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43396-
dc.description.abstractA radio afterglow was detected following the 1998 August 27 giant flare from the soft gamma repeater (SGR) 4900+14. Its short-lived behavior is quite different from the radio nebula of SGR 1806-20, but very similar to radio afterglows from classic gamma-ray bursts (GRBs). Motivated by this, we attempt to explain it with the external shock model as invoked in the standard theory of GRB afterglows. We find that the light curve of this radio afterglow is not consistent with the forward shock emission of an ultrarelativistic outflow, which is suggested to be responsible for the initial hard spike of the giant flare. Nevertheless, shock emission from a mildly or subrelativistic outflow expanding into the interstellar medium could fit the observations. The possible origin for this kind of outflow is discussed, based on the magnetar model for SGRs. Furthermore, we suggest that the presence of an ultrarelativistic fireball from SGR giant flares could be tested by rapid radio to optical follow-up observations in the future.en_HK
dc.format.extent85393 bytes-
dc.format.extent12158 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypetext/plain-
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 Letters. Copyright © University of Chicago Press.en_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectGamma rays: burstsen_HK
dc.subjectISM: jets and outflowsen_HK
dc.subjectStars: individual (SGR 1900+14)en_HK
dc.titleThe radio afterglow from the giant flare of SGR 1900+14: The same mechanism as afterglows from classic gamma-ray bursts?en_HK
dc.typeArticleen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/378216en_HK
dc.identifier.scopuseid_2-s2.0-0242680144en_HK
dc.identifier.hkuros84989-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0242680144&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume593en_HK
dc.identifier.issue2 IIen_HK
dc.identifier.spageL85en_HK
dc.identifier.epageL88en_HK
dc.identifier.isiWOS:000184823900007-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridWang, XY=9745320700en_HK

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