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Article: Quiescent high-energy gamma-ray emission from soft gamma-ray repeaters
Title | Quiescent high-energy gamma-ray emission from soft gamma-ray repeaters |
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Authors | |
Keywords | Gamma rays: theory Pulsars: general Stars: neutron |
Issue Date | 2002 |
Publisher | Institute 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? |
Abstract | We 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 Identifier | http://hdl.handle.net/10722/43387 |
ISSN | 2023 Impact Factor: 8.8 2023 SCImago Journal Rankings: 2.766 |
ISI Accession Number ID | |
References |
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Zhang, L | en_HK |
dc.contributor.author | Cheng, KS | en_HK |
dc.date.accessioned | 2007-03-23T04:44:44Z | - |
dc.date.available | 2007-03-23T04:44:44Z | - |
dc.date.issued | 2002 | en_HK |
dc.identifier.citation | Astrophysical Journal Letters, 2002, v. 579 n. 2 I, p. 716-724 | en_HK |
dc.identifier.issn | 2041-8205 | en_HK |
dc.identifier.uri | http://hdl.handle.net/10722/43387 | - |
dc.description.abstract | We 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.extent | 201466 bytes | - |
dc.format.extent | 12158 bytes | - |
dc.format.mimetype | application/pdf | - |
dc.format.mimetype | text/plain | - |
dc.language | eng | en_HK |
dc.publisher | Institute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205 | en_HK |
dc.relation.ispartof | Astrophysical Journal Letters | en_HK |
dc.rights | The Astrophysical Journal. Copyright © University of Chicago Press. | en_HK |
dc.subject | Gamma rays: theory | en_HK |
dc.subject | Pulsars: general | en_HK |
dc.subject | Stars: neutron | en_HK |
dc.title | Quiescent high-energy gamma-ray emission from soft gamma-ray repeaters | en_HK |
dc.type | Article | en_HK |
dc.identifier.openurl | http://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+Repeaters | en_HK |
dc.identifier.email | Cheng, KS: hrspksc@hkucc.hku.hk | en_HK |
dc.identifier.authority | Cheng, KS=rp00675 | en_HK |
dc.description.nature | published_or_final_version | en_HK |
dc.identifier.doi | 10.1086/342831 | en_HK |
dc.identifier.scopus | eid_2-s2.0-0041831260 | en_HK |
dc.identifier.hkuros | 77190 | - |
dc.relation.references | http://www.scopus.com/mlt/select.url?eid=2-s2.0-0041831260&selection=ref&src=s&origin=recordpage | en_HK |
dc.identifier.volume | 579 | en_HK |
dc.identifier.issue | 2 I | en_HK |
dc.identifier.spage | 716 | en_HK |
dc.identifier.epage | 724 | en_HK |
dc.identifier.isi | WOS:000179062700025 | - |
dc.publisher.place | United Kingdom | en_HK |
dc.identifier.scopusauthorid | Zhang, L=38762428100 | en_HK |
dc.identifier.scopusauthorid | Cheng, KS=9745798500 | en_HK |
dc.identifier.issnl | 2041-8205 | - |