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Article: Particle acceleration and non-thermal emission in the pulsar outer magnetospheric gap

TitleParticle acceleration and non-thermal emission in the pulsar outer magnetospheric gap
Authors
KeywordsPulsars: general
Radiation mechanisms: non-thermal
Issue Date2008
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, 2008, v. 386 n. 2, p. 748-758 How to Cite?
AbstractA two-dimensional electrodynamic model is used to study particle acceleration and non-thermal emission mechanisms in the pulsar magnetosphere. We solve the distribution of the accelerating electric field with the emission process and the pair-creation process in the meridional plane, which includes the rotational and magnetic axes. By solving the evolutions of the Lorentz factor, and of the pitch angle, we calculate the spectrum in optical through γ-ray bands with the curvature radiation, synchrotron radiation and inverse-Compton process, not only for outgoing particles but also for ingoing particles, which have been ignored in previous studies. We apply this theory to the Vela pulsar. We find that the curvature radiation from the outgoing particles is the major emission process above 10 MeV bands. In soft γ-ray to hard X-ray bands, the synchrotron radiation from the incoming primary particles in the gap dominates in the spectrum. Below hard X-ray bands, the synchrotron emissions from both outgoing and ingoing particles contribute to the calculated spectrum. The calculated spectrum is consistent with the observed phase-averaged spectrum of the Vela pulsar. Taking into account the predicted dependence of the emission process and the emitting particles on the energy bands, we compute the expected pulse profile in X-ray and γ-ray bands with a three-dimensional geometrical model. We show that the observed five-peak pulse profile in the X-ray bands of the Vela pulsar is reproduced by the inward and outward emissions, and the observed double-peak pulse profile in γ-ray bands is explained by the outward emissions. We also apply the theory to PSR B1706-44 and PSR B1951+32, for which X-ray emission properties have not been constrained observationally very well, to predict the spectral features with the present outer-gap model. © 2008 The Authors.
Persistent Identifierhttp://hdl.handle.net/10722/134624
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorTakata, Jen_HK
dc.contributor.authorChang, HKen_HK
dc.contributor.authorShibata, Sen_HK
dc.date.accessioned2011-06-29T07:32:05Z-
dc.date.available2011-06-29T07:32:05Z-
dc.date.issued2008en_HK
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society, 2008, v. 386 n. 2, p. 748-758en_HK
dc.identifier.issn0035-8711en_HK
dc.identifier.urihttp://hdl.handle.net/10722/134624-
dc.description.abstractA two-dimensional electrodynamic model is used to study particle acceleration and non-thermal emission mechanisms in the pulsar magnetosphere. We solve the distribution of the accelerating electric field with the emission process and the pair-creation process in the meridional plane, which includes the rotational and magnetic axes. By solving the evolutions of the Lorentz factor, and of the pitch angle, we calculate the spectrum in optical through γ-ray bands with the curvature radiation, synchrotron radiation and inverse-Compton process, not only for outgoing particles but also for ingoing particles, which have been ignored in previous studies. We apply this theory to the Vela pulsar. We find that the curvature radiation from the outgoing particles is the major emission process above 10 MeV bands. In soft γ-ray to hard X-ray bands, the synchrotron radiation from the incoming primary particles in the gap dominates in the spectrum. Below hard X-ray bands, the synchrotron emissions from both outgoing and ingoing particles contribute to the calculated spectrum. The calculated spectrum is consistent with the observed phase-averaged spectrum of the Vela pulsar. Taking into account the predicted dependence of the emission process and the emitting particles on the energy bands, we compute the expected pulse profile in X-ray and γ-ray bands with a three-dimensional geometrical model. We show that the observed five-peak pulse profile in the X-ray bands of the Vela pulsar is reproduced by the inward and outward emissions, and the observed double-peak pulse profile in γ-ray bands is explained by the outward emissions. We also apply the theory to PSR B1706-44 and PSR B1951+32, for which X-ray emission properties have not been constrained observationally very well, to predict the spectral features with the present outer-gap model. © 2008 The Authors.en_HK
dc.languageeng-
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.subjectPulsars: generalen_HK
dc.subjectRadiation mechanisms: non-thermalen_HK
dc.titleParticle acceleration and non-thermal emission in the pulsar outer magnetospheric gapen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0035-8711&volume=386&issue=2&spage=748&epage=758&date=2008&atitle=Particle+acceleration+and+non-thermal+emission+in+the+pulsar+outer+magnetospheric+gap-
dc.identifier.emailTakata, J: takata@hku.hken_HK
dc.identifier.authorityTakata, J=rp00786en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1111/j.1365-2966.2008.12877.xen_HK
dc.identifier.scopuseid_2-s2.0-42549102178en_HK
dc.identifier.hkuros170776-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-42549102178&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume386en_HK
dc.identifier.issue2en_HK
dc.identifier.spage748en_HK
dc.identifier.epage758en_HK
dc.identifier.isiWOS:000255287100012-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridTakata, J=22735157300en_HK
dc.identifier.scopusauthoridChang, HK=7407523188en_HK
dc.identifier.scopusauthoridShibata, S=7402120464en_HK
dc.identifier.citeulike2732916-

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