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Article: Pulsar Wind Origin of Cosmic Ray Positrons

TitlePulsar Wind Origin of Cosmic Ray Positrons
Authors
KeywordsAcceleration of particles
Ism - cosmic rays
Stars - pulsars - general
Issue Date1996
PublisherUniversity of Chicago Press. The Journal's web site is located at http://www.journals.uchicago.edu/ApJ
Citation
The Astrophysical Journal, 1996, v. 459, p. L83-L86 How to Cite?
AbstractWe show that the electron-positron pairs produced in the magnetosphere of a pulsar can be accelerated monoenergetically to relativistic energies in the wind driven by low-frequency electromagnetic waves. The final achievable energy, depending on the surface magnetic field and rotation period of the individual pulsar, is mostly in the range 10-2--102 GeV. Based on the pair production rate of the individual pulsars and the Galactic pulsar population, the electron-positron flux from the Galactic pulsars is estimated from a statistical analysis of the observed pulsar data. We find that the flux is enough to account for the measured positron fraction and that its energy spectrum well matches the measured one. Our model predicts that the positron fraction will rise with increasing energy until its peak value at 30 GeV and then drop off.
Persistent Identifierhttp://hdl.handle.net/10722/43162
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266

 

DC FieldValueLanguage
dc.contributor.authorChi, Xen_HK
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorYoung, ECMen_HK
dc.date.accessioned2007-03-23T04:40:26Z-
dc.date.available2007-03-23T04:40:26Z-
dc.date.issued1996en_HK
dc.identifier.citationThe Astrophysical Journal, 1996, v. 459, p. L83-L86en_HK
dc.identifier.issn0004-637Xen_HK
dc.identifier.urihttp://hdl.handle.net/10722/43162-
dc.description.abstractWe show that the electron-positron pairs produced in the magnetosphere of a pulsar can be accelerated monoenergetically to relativistic energies in the wind driven by low-frequency electromagnetic waves. The final achievable energy, depending on the surface magnetic field and rotation period of the individual pulsar, is mostly in the range 10-2--102 GeV. Based on the pair production rate of the individual pulsars and the Galactic pulsar population, the electron-positron flux from the Galactic pulsars is estimated from a statistical analysis of the observed pulsar data. We find that the flux is enough to account for the measured positron fraction and that its energy spectrum well matches the measured one. Our model predicts that the positron fraction will rise with increasing energy until its peak value at 30 GeV and then drop off.en_HK
dc.format.extent628400 bytes-
dc.format.extent12158 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypetext/plain-
dc.languageengen_HK
dc.publisherUniversity of Chicago Press. The Journal's web site is located at http://www.journals.uchicago.edu/ApJen_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.subjectAcceleration of particlesen_HK
dc.subjectIsm - cosmic raysen_HK
dc.subjectStars - pulsars - generalen_HK
dc.titlePulsar Wind Origin of Cosmic Ray Positronsen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=459&spage=L83&epage=L86&date=1996&atitle=Pulsar+Wind+Origin+of+Cosmic+Ray+Positronsen_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/309943en_HK
dc.identifier.hkuros11052-

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