Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/4471
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dc.contributor.authorMoharana, Reetanjali-
dc.contributor.authorGupta, Nayantara-
dc.date.accessioned2012-05-08T04:49:52Z-
dc.date.available2012-05-08T04:49:52Z-
dc.date.issued2010-07-
dc.identifier.citationPhysical Review D, 2010, Vol.82, p023003en
dc.identifier.issn1550-7998-
dc.identifier.issn1550-2368 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/4471-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractUltrahigh-energy neutrons and pions are likely to be produced in particle interactions inside cosmic ray sources and subsequently decay to neutrinos and other secondary particles [π±→μ±νμ(ν¯μ),μ±→e±ν¯μ(νμ)νe(ν¯e)]. In high magnetic fields of the cosmic acceleration sites, the ultrahigh-energy-charged particles may lose energy significantly due to synchrotron radiation before decay. We show that for gamma-ray bursts in the internal shock model, the flux of very high-energy antineutrinos (ν¯e) produced from decaying ultrahigh-energy neutrons can be more than the total neutrino flux produced in pion decay depending on the values of their Lorentz factors, luminosities, and variability times.en
dc.language.isoenen
dc.publisherThe American Physical Societyen
dc.relation.urihttp://adsabs.harvard.edu/abs/2010PhRvD..82b3003Men
dc.relation.urihttp://arxiv.org/abs/1005.0250en
dc.relation.urihttp://dx.doi.org/10.1103/PhysRevD.82.023003en
dc.rights2010 The American Physical Societyen
dc.subjectRadio sourcesen
dc.subjectcosmic raysen
dc.titleTracing cosmic accelerators with decaying neutronsen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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