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Article: Very high energy gamma rays from millisecond pulsars

TitleVery high energy gamma rays from millisecond pulsars
Authors
Issue Date1990
PublisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/npbps
Citation
Nuclear Physics B (Proceedings Supplements), 1990, v. 14 n. 1, p. 28-37 How to Cite?
AbstractIn this paper we concentrate on the emission of TeV γ - rays from radio pulsars. It will be shown that the polar gap model fails to explain the observed TeV flux levels: The X-ray luminosity should exceed the TeV luminosity if the latter originates from the polar gap regions. The outer gap model of Cheng, Ho and Ruderman provides a consistent picture of TeV γ - ray emission: The total gap power is converted to TeV γ - rays by means of the inverse Compton scattering of primary electrons on the abundant soft IR flux in and around the gap. A fraction exp(-f- 1 2) escapes photon-photon absorption and may be observable Here f (∼ 0.1 for Vela and Vela-like pulsars) is the fraction of the open magnetosphere occupied by the gap. The remaining power is used for the gap sustaining mechanism. As the pulsar grows older, f → 1 and the TeV power increases and becomes comparable to the spindown power. This is the so-called "post Vela-like" stage. The model is applied to millisecond pulsars which are all Vela- and post Vela-like. The luminosity estimates are consistent with the TeV observations - despite the experimental uncertainties and theoretical assumptions. © 1990.
Persistent Identifierhttp://hdl.handle.net/10722/174854
ISSN
2005 Impact Factor: 0.875

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_US
dc.contributor.authorDe Jager, OCen_US
dc.date.accessioned2012-11-26T08:47:49Z-
dc.date.available2012-11-26T08:47:49Z-
dc.date.issued1990en_US
dc.identifier.citationNuclear Physics B (Proceedings Supplements), 1990, v. 14 n. 1, p. 28-37en_US
dc.identifier.issn0920-5632en_US
dc.identifier.urihttp://hdl.handle.net/10722/174854-
dc.description.abstractIn this paper we concentrate on the emission of TeV γ - rays from radio pulsars. It will be shown that the polar gap model fails to explain the observed TeV flux levels: The X-ray luminosity should exceed the TeV luminosity if the latter originates from the polar gap regions. The outer gap model of Cheng, Ho and Ruderman provides a consistent picture of TeV γ - ray emission: The total gap power is converted to TeV γ - rays by means of the inverse Compton scattering of primary electrons on the abundant soft IR flux in and around the gap. A fraction exp(-f- 1 2) escapes photon-photon absorption and may be observable Here f (∼ 0.1 for Vela and Vela-like pulsars) is the fraction of the open magnetosphere occupied by the gap. The remaining power is used for the gap sustaining mechanism. As the pulsar grows older, f → 1 and the TeV power increases and becomes comparable to the spindown power. This is the so-called "post Vela-like" stage. The model is applied to millisecond pulsars which are all Vela- and post Vela-like. The luminosity estimates are consistent with the TeV observations - despite the experimental uncertainties and theoretical assumptions. © 1990.en_US
dc.languageengen_US
dc.publisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/npbpsen_US
dc.relation.ispartofNuclear Physics B (Proceedings Supplements)en_US
dc.titleVery high energy gamma rays from millisecond pulsarsen_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-0040551808en_US
dc.identifier.volume14en_US
dc.identifier.issue1en_US
dc.identifier.spage28en_US
dc.identifier.epage37en_US
dc.publisher.placeNetherlandsen_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridde Jager, OC=7003482279en_US

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