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Diffuse PeV neutrinos from EeV cosmic ray sources: Semirelativistic hypernova remnants in star-forming galaxies

Liu, Ruo-Yu; Wang, Xiang-Yu; Inoue, Susumu; Crocker, Roland; Aharonian, F

Description

We argue that the excess of sub-PeV/PeV neutrinos recently reported by IceCube could plausibly originate through pion-production processes in the same sources responsible for cosmic rays (CRs) with energy above the second knee around 1018eV. The pion-production efficiency for escaping CRs that produce PeV neutrinos is required to be 0.1 in such sources. On the basis of current data, we identify semirelativistic hypernova remnants as possible sources that satisfy the requirements. By virtue of...[Show more]

dc.contributor.authorLiu, Ruo-Yu
dc.contributor.authorWang, Xiang-Yu
dc.contributor.authorInoue, Susumu
dc.contributor.authorCrocker, Roland
dc.contributor.authorAharonian, F
dc.date.accessioned2015-12-10T23:36:09Z
dc.identifier.issn1550-7998
dc.identifier.urihttp://hdl.handle.net/1885/70021
dc.description.abstractWe argue that the excess of sub-PeV/PeV neutrinos recently reported by IceCube could plausibly originate through pion-production processes in the same sources responsible for cosmic rays (CRs) with energy above the second knee around 1018eV. The pion-production efficiency for escaping CRs that produce PeV neutrinos is required to be 0.1 in such sources. On the basis of current data, we identify semirelativistic hypernova remnants as possible sources that satisfy the requirements. By virtue of their fast ejecta, such objects can accelerate protons to EeV energies, which, in turn, can interact with the dense surrounding medium during propagation in their host galaxies to produce sufficient high-energy neutrinos via proton-proton (pp) collisions. Their accompanying gamma-ray flux can remain below the diffuse isotropic gamma-ray background observed by the Fermi Large Area Telescope. In order to test this scenario and discriminate from alternatives, the density of target protons/nuclei and the residence time of CRs in the interacting region are crucial uncertainties that need to be clarified. As long as the neutrinos and EeV CRs originate from the same source class, detection of 10PeV neutrinos may be expected within 5-10 years' operation of IceCube. Together with further observations in the PeV range, the neutrinos can help in revealing the currently unknown sources of EeV CRs.
dc.publisherAmerican Physical Society
dc.rightsAuthor/s retain copyright
dc.sourcePhysical Review D-Particles, Fields, Gravitation and Cosmology
dc.titleDiffuse PeV neutrinos from EeV cosmic ray sources: Semirelativistic hypernova remnants in star-forming galaxies
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume89
dc.date.issued2014
local.identifier.absfor020104 - Galactic Astronomy
local.identifier.absfor020106 - High Energy Astrophysics; Cosmic Rays
local.identifier.absfor020103 - Cosmology and Extragalactic Astronomy
local.identifier.ariespublicationU3488905xPUB2196
local.type.statusPublished Version
local.contributor.affiliationLiu, Ruo-Yu, Nanjing University
local.contributor.affiliationWang, Xiang-Yu, Nanjing University
local.contributor.affiliationInoue, Susumu, National Astronomical Observatory of Japan
local.contributor.affiliationCrocker, Roland, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationAharonian, F, Max-Planck-Institut fur Kernphysik
local.bibliographicCitation.issue8
local.identifier.doi10.1103/PhysRevD.89.083004
dc.date.updated2015-12-10T11:51:24Z
local.identifier.scopusID2-s2.0-84898636009
local.identifier.thomsonID000334335400002
dcterms.accessRightsOpen Access
CollectionsANU Research Publications

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