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Article: Neutrino production from accreting x-ray pulsars

TitleNeutrino production from accreting x-ray pulsars
Authors
Issue Date1992
PublisherInstitute of Physics Publishing. The Journal's web site is located at http://www.iop.org/Journals/jpg
Citation
Journal Of Physics G: Nuclear And Particle Physics, 1992, v. 18 n. 4, p. 725-738 How to Cite?
AbstractThere exist electrostatic acceleration regions (accelerator gaps) above the inner part of a Keplerian accretion disc of an x-ray pulsar which can accelerate positively charged particles (protons/ions) to extreme relativistic energies (>or=10 15 eV) towards the accretion disc. The subsequent hadronic collisions between such ultrarelativistic protons (ions) and the disc material can produce numerous secondary mesons whose decay generates a luminous neutrino flux. Although the neutrinos can directly escape from the collision regions without any energy loss, the disc magnetic field can modify the neutrino spectrum because their unstable charged parent particles can lose energy via synchrotron radiation. This can provide direct information on the structure of the accretion disc. In calculating the meson production rate, the authors have used an improved scaling violation model which has the effect of enhancing the neutrino production rate. It appears that a large fraction of the accretion power of x-ray pulsars ( approximately 10 37 erg s -1) could be carried away by the neutrino flux. It may be to detect these neutrino sources in future.
Persistent Identifierhttp://hdl.handle.net/10722/175062
ISSN
2015 Impact Factor: 2.448
2015 SCImago Journal Rankings: 0.856
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_US
dc.contributor.authorCheung, Ten_US
dc.contributor.authorLau, MMen_US
dc.contributor.authorNg, KWen_US
dc.date.accessioned2012-11-26T08:49:03Z-
dc.date.available2012-11-26T08:49:03Z-
dc.date.issued1992en_US
dc.identifier.citationJournal Of Physics G: Nuclear And Particle Physics, 1992, v. 18 n. 4, p. 725-738en_US
dc.identifier.issn0954-3899en_US
dc.identifier.urihttp://hdl.handle.net/10722/175062-
dc.description.abstractThere exist electrostatic acceleration regions (accelerator gaps) above the inner part of a Keplerian accretion disc of an x-ray pulsar which can accelerate positively charged particles (protons/ions) to extreme relativistic energies (>or=10 15 eV) towards the accretion disc. The subsequent hadronic collisions between such ultrarelativistic protons (ions) and the disc material can produce numerous secondary mesons whose decay generates a luminous neutrino flux. Although the neutrinos can directly escape from the collision regions without any energy loss, the disc magnetic field can modify the neutrino spectrum because their unstable charged parent particles can lose energy via synchrotron radiation. This can provide direct information on the structure of the accretion disc. In calculating the meson production rate, the authors have used an improved scaling violation model which has the effect of enhancing the neutrino production rate. It appears that a large fraction of the accretion power of x-ray pulsars ( approximately 10 37 erg s -1) could be carried away by the neutrino flux. It may be to detect these neutrino sources in future.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing. The Journal's web site is located at http://www.iop.org/Journals/jpgen_US
dc.relation.ispartofJournal of Physics G: Nuclear and Particle Physicsen_US
dc.titleNeutrino production from accreting x-ray 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.doi10.1088/0954-3899/18/4/008en_US
dc.identifier.scopuseid_2-s2.0-34247274674en_US
dc.identifier.volume18en_US
dc.identifier.issue4en_US
dc.identifier.spage725en_US
dc.identifier.epage738en_US
dc.identifier.isiWOS:A1992HK79100008-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US
dc.identifier.scopusauthoridCheung, T=7103334177en_US
dc.identifier.scopusauthoridLau, MM=16441454100en_US
dc.identifier.scopusauthoridNg, KW=7403178388en_US

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