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Article: Quiescent high-energy gamma-ray emission from soft gamma-ray repeaters

TitleQuiescent high-energy gamma-ray emission from soft gamma-ray repeaters
Authors
KeywordsGamma rays: theory
Pulsars: general
Stars: neutron
Issue Date2002
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2002, v. 579 n. 2 I, p. 716-724 How to Cite?
AbstractWe present a model for the high-energy γ-ray emission from the outer gap of soft gamma-ray repeaters (SGRs) during their quiescent states. In this model, X-rays come from the stellar surface, but the emerging X-ray spectrum will have a power-law tail because of the multiple scattering at the cyclotron resonance in the magneto sphere, as pointed out by Thompson, Lyukitov, &Kulkarni. The outer gap is sustained by the collision between these X-rays with the high-energy photons produced in the outer gap through the photon-photon pair production. We have taken a magnetic dipole geometry into account in estimating the fractional size of the outer gap. The fractional size of the outer gap depends on the period, surface magnetic field, average X-ray energy, and the magnetic inclination angle of the neutron star. After the average fractional size outer gap is determined, the spectrum and luminosity of high-energy photons from the outer gap can be calculated. We apply this model to some SGRs, such as SGR 1806-20 and SGR 1900+14, and compare the expected integral fluxes with the sensitivities of EGRET, GLAST, MAGIC, and VERITAS. We predict that the integral flux of SGR 1900+14 may be greater than the sensitivity of GLAST, and especially that the integral flux for a large magnetic inclination angle (say 80°) may be greater than the sensitivities of GLAST and MAGIC. However, we predict that SGR 1806-20 would not be detected by GLAST because its distance is about 3 times of that of SGR 1900+14.
Persistent Identifierhttp://hdl.handle.net/10722/43387
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorZhang, Len_HK
dc.contributor.authorCheng, KSen_HK
dc.date.accessioned2007-03-23T04:44:44Z-
dc.date.available2007-03-23T04:44:44Z-
dc.date.issued2002en_HK
dc.identifier.citationAstrophysical Journal Letters, 2002, v. 579 n. 2 I, p. 716-724en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43387-
dc.description.abstractWe present a model for the high-energy γ-ray emission from the outer gap of soft gamma-ray repeaters (SGRs) during their quiescent states. In this model, X-rays come from the stellar surface, but the emerging X-ray spectrum will have a power-law tail because of the multiple scattering at the cyclotron resonance in the magneto sphere, as pointed out by Thompson, Lyukitov, &Kulkarni. The outer gap is sustained by the collision between these X-rays with the high-energy photons produced in the outer gap through the photon-photon pair production. We have taken a magnetic dipole geometry into account in estimating the fractional size of the outer gap. The fractional size of the outer gap depends on the period, surface magnetic field, average X-ray energy, and the magnetic inclination angle of the neutron star. After the average fractional size outer gap is determined, the spectrum and luminosity of high-energy photons from the outer gap can be calculated. We apply this model to some SGRs, such as SGR 1806-20 and SGR 1900+14, and compare the expected integral fluxes with the sensitivities of EGRET, GLAST, MAGIC, and VERITAS. We predict that the integral flux of SGR 1900+14 may be greater than the sensitivity of GLAST, and especially that the integral flux for a large magnetic inclination angle (say 80°) may be greater than the sensitivities of GLAST and MAGIC. However, we predict that SGR 1806-20 would not be detected by GLAST because its distance is about 3 times of that of SGR 1900+14.en_HK
dc.format.extent201466 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.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.subjectGamma rays: theoryen_HK
dc.subjectPulsars: generalen_HK
dc.subjectStars: neutronen_HK
dc.titleQuiescent high-energy gamma-ray emission from soft gamma-ray repeatersen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=579&issue=2 pt 1&spage=716&epage=724&date=2002&atitle=Quiescent+High-Energy+Gamma-Ray+Emission+from+Soft+Gamma-Ray+Repeatersen_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.doi10.1086/342831en_HK
dc.identifier.scopuseid_2-s2.0-0041831260en_HK
dc.identifier.hkuros77190-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0041831260&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume579en_HK
dc.identifier.issue2 Ien_HK
dc.identifier.spage716en_HK
dc.identifier.epage724en_HK
dc.identifier.isiWOS:000179062700025-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridZhang, L=38762428100en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK

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