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Article: Three-dimensional two-layer outer gap model: Fermi energy-dependent light curves of the Vela pulsar

TitleThree-dimensional two-layer outer gap model: Fermi energy-dependent light curves of the Vela pulsar
Authors
KeywordsMethods: numerical
Pulsars: general
Radiation mechanisms: non-thermal
Issue Date2011
PublisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNR
Citation
Monthly Notices Of The Royal Astronomical Society, 2011, v. 414 n. 3, p. 2664-2673 How to Cite?
AbstractWe extend the two-dimensional two-layer outer gap model to a three-dimensional geometry and use it to study the high-energy emission of the Vela pulsar. In this model, the outer gap is divided into two parts, i.e. the main acceleration region on the top of last-open field lines and the screening region around the upper boundary of the gap. In the main acceleration region, the charge density is much lower than the Goldreich-Julian charge density, and the charged particles are accelerated by the electric field along the magnetic field to emit multi-GeV photons. In the screening region, the charge density is larger than the Goldreich-Julian value to close the gap, and particles in this region are responsible for multi-100MeV photon emission. We apply this three-dimensional two-layer model to the Vela pulsar and compare the model light curves, the phase-averaged spectrum and the phase-resolved spectra with the recent Fermi observations, which also reveals the existence of the third peak between two main peaks. The phase position of the third peak moves with the photon energy, which cannot be explained by the geometry of magnetic field structure and the caustic effects of the photon propagation. We suggest that the existence of the third peak and its energy-dependent movement results from the azimuthal structure of the outer gap. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/135362
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorWang, Yen_HK
dc.contributor.authorTakata, Jen_HK
dc.contributor.authorCheng, KSen_HK
dc.date.accessioned2011-07-27T01:34:10Z-
dc.date.available2011-07-27T01:34:10Z-
dc.date.issued2011en_HK
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society, 2011, v. 414 n. 3, p. 2664-2673en_HK
dc.identifier.issn0035-8711en_HK
dc.identifier.urihttp://hdl.handle.net/10722/135362-
dc.description.abstractWe extend the two-dimensional two-layer outer gap model to a three-dimensional geometry and use it to study the high-energy emission of the Vela pulsar. In this model, the outer gap is divided into two parts, i.e. the main acceleration region on the top of last-open field lines and the screening region around the upper boundary of the gap. In the main acceleration region, the charge density is much lower than the Goldreich-Julian charge density, and the charged particles are accelerated by the electric field along the magnetic field to emit multi-GeV photons. In the screening region, the charge density is larger than the Goldreich-Julian value to close the gap, and particles in this region are responsible for multi-100MeV photon emission. We apply this three-dimensional two-layer model to the Vela pulsar and compare the model light curves, the phase-averaged spectrum and the phase-resolved spectra with the recent Fermi observations, which also reveals the existence of the third peak between two main peaks. The phase position of the third peak moves with the photon energy, which cannot be explained by the geometry of magnetic field structure and the caustic effects of the photon propagation. We suggest that the existence of the third peak and its energy-dependent movement results from the azimuthal structure of the outer gap. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.en_HK
dc.languageengen_US
dc.publisherBlackwell Publishing Ltd. The Journal's web site is located at http://www.blackwellpublishing.com/journals/MNRen_HK
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_HK
dc.rightsThe definitive version is available at www.blackwell-synergy.com-
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectMethods: numericalen_HK
dc.subjectPulsars: generalen_HK
dc.subjectRadiation mechanisms: non-thermalen_HK
dc.titleThree-dimensional two-layer outer gap model: Fermi energy-dependent light curves of the Vela pulsaren_HK
dc.typeArticleen_HK
dc.identifier.emailTakata, J: takata@hku.hken_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityTakata, J=rp00786en_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1111/j.1365-2966.2011.18577.xen_HK
dc.identifier.scopuseid_2-s2.0-79959377961en_HK
dc.identifier.hkuros186457en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-79959377961&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume414en_HK
dc.identifier.issue3en_HK
dc.identifier.spage2664en_HK
dc.identifier.epage2673en_HK
dc.identifier.isiWOS:000292977600067-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridWang, Y=36085420300en_HK
dc.identifier.scopusauthoridTakata, J=22735157300en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.citeulike9519687-

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