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Article: Pulsar high energy emissions from outer gap accelerator closed by a magnetic pair-creation process

TitlePulsar high energy emissions from outer gap accelerator closed by a magnetic pair-creation process
Authors
KeywordsMagnetic fields
Pulsars: general
Radiation mechanisms: non-thermal
Issue Date2010
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2010, v. 715 n. 2, p. 1318-1326 How to Cite?
AbstractWe discuss outer gap closure mechanism in the trans-field direction with the magnetic pair-creation process near the stellar surface. The gap closure by the magnetic pair creation is possible if some fraction of the pairs are produced with an outgoing momentum. By assuming that multiple magnetic field will affect the local field near the stellar surface, we show a specific magnetic field geometry near the stellar surface resulting in the outflow of the pairs. Together with the fact that the electric field is weak below null charge surface, the characteristic curvature photon energy emitted by incoming particles, which were accelerated in the outer gap, decreases drastically to ∼100 MeV near the stellar surface. We estimate the height measured from the last-open field line, above which 100 MeV photons are converted into pairs by the magnetic pair creation. We also show the resultant multiplicity due to the magnetic pair-creation process could acquire M e± ∼ 10 410 5. In this model, the fractional outer gap size is proportional to P ?1/2. The predicted γ -ray luminosity (L γ ) and the characteristic curvature photon energy (E c) emitted from the outer gap are proportional to B 2P ?5/2 and B 3/4P ?1, respectively. This model also predicts that L γ and E c are related to the spin-down power (L sd) or the spin-down age of pulsars or the spin-down age of pulsars (τ) as L γ ∝ L sd 5/8 or L γ ∝ τ -5/4 and E c ∝ τ -5/4 and E c ∝ L 1/4 sd or E c ∝ τ -1/2, respectively. © 2010. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/129027
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
Funding AgencyGrant Number
Hong Kong SAR GovernmentHKU700908P
Funding Information:

We thank the referee for insightful comments on the manuscript. We thank the useful discussions with H.-K. Chang, K. Hirotani, C. Y. Hui, B. Rudak, M. Ruderman, and S. Shibata. We also thank the Theoretical Institute for Advanced Research in Astrophysics (TIARA) operated under Academia Sinica Institute of Astronomy and Astrophysics, Taiwan, which enabled J.T. to use the PC cluster at TIARA. This work is supported by a GRF grant of Hong Kong SAR Government under HKU700908P.

References

 

DC FieldValueLanguage
dc.contributor.authorTakata, Jen_HK
dc.contributor.authorWang, Yen_HK
dc.contributor.authorCheng, KSen_HK
dc.date.accessioned2010-12-20T06:36:25Z-
dc.date.available2010-12-20T06:36:25Z-
dc.date.issued2010en_HK
dc.identifier.citationAstrophysical Journal Letters, 2010, v. 715 n. 2, p. 1318-1326en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/129027-
dc.description.abstractWe discuss outer gap closure mechanism in the trans-field direction with the magnetic pair-creation process near the stellar surface. The gap closure by the magnetic pair creation is possible if some fraction of the pairs are produced with an outgoing momentum. By assuming that multiple magnetic field will affect the local field near the stellar surface, we show a specific magnetic field geometry near the stellar surface resulting in the outflow of the pairs. Together with the fact that the electric field is weak below null charge surface, the characteristic curvature photon energy emitted by incoming particles, which were accelerated in the outer gap, decreases drastically to ∼100 MeV near the stellar surface. We estimate the height measured from the last-open field line, above which 100 MeV photons are converted into pairs by the magnetic pair creation. We also show the resultant multiplicity due to the magnetic pair-creation process could acquire M e± ∼ 10 410 5. In this model, the fractional outer gap size is proportional to P ?1/2. The predicted γ -ray luminosity (L γ ) and the characteristic curvature photon energy (E c) emitted from the outer gap are proportional to B 2P ?5/2 and B 3/4P ?1, respectively. This model also predicts that L γ and E c are related to the spin-down power (L sd) or the spin-down age of pulsars or the spin-down age of pulsars (τ) as L γ ∝ L sd 5/8 or L γ ∝ τ -5/4 and E c ∝ τ -5/4 and E c ∝ L 1/4 sd or E c ∝ τ -1/2, respectively. © 2010. The American Astronomical Society. All rights reserved.en_HK
dc.languageeng-
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.rightsThe Astrophysical Journal. Copyright © Institute of Physics Publishing, Inc.-
dc.subjectMagnetic fieldsen_HK
dc.subjectPulsars: generalen_HK
dc.subjectRadiation mechanisms: non-thermalen_HK
dc.titlePulsar high energy emissions from outer gap accelerator closed by a magnetic pair-creation processen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=715&issue=2&spage=1318&epage=1326&date=2010&atitle=Pulsar+high+energy+emissions+from+outer+gap+accelerator+closed+by+a+magnetic+pair-creation+process-
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.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1088/0004-637X/715/2/1318en_HK
dc.identifier.scopuseid_2-s2.0-77952873553en_HK
dc.identifier.hkuros170765-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-77952873553&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume715en_HK
dc.identifier.issue2en_HK
dc.identifier.spage1318en_HK
dc.identifier.epage1326en_HK
dc.identifier.eissn1538-4357-
dc.identifier.isiWOS:000277642100046-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridTakata, J=22735157300en_HK
dc.identifier.scopusauthoridWang, Y=7601492574en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK

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