TY - GEN
T1 - Z-burst scenario for the highest energy cosmic rays
AU - Fodor, Z.
AU - Katz, S. D.
AU - Ringwald, A.
PY - 2003
Y1 - 2003
N2 - The origin of highest energy cosmic rays is yet unknown. An appealing possibility is the so-called Z-burst scenario, in which a large fraction of these cosmic rays are decay products of Z bosons produced in the scattering of ultrahigh energy neutrinos on cosmological relic neutrinos. The comparison between the observed and predicted spectra constrains the mass of the heaviest neutrino. The required neutrino mass is fairly robust against variations of the presently unknown quantities, such as the amount of relic neutrino clustering, the universal photon radio background and the extragalactic magnetic field. Considering different possibilities for the ordinary cosmic rays the required neutrino masses are determined. In the most plausible case that the ordinary cosmic rays are of extragalactic origin and the universal radio background is strong enough to suppress high energy photons, the required neutrino mass is 0.08 eV ≤ m v 0.40 eV. The required ultrahigh energy neutrino flux should be detected in the near future by experiments such as AMANDA, RICE or the Pierre Auger Observatory.
AB - The origin of highest energy cosmic rays is yet unknown. An appealing possibility is the so-called Z-burst scenario, in which a large fraction of these cosmic rays are decay products of Z bosons produced in the scattering of ultrahigh energy neutrinos on cosmological relic neutrinos. The comparison between the observed and predicted spectra constrains the mass of the heaviest neutrino. The required neutrino mass is fairly robust against variations of the presently unknown quantities, such as the amount of relic neutrino clustering, the universal photon radio background and the extragalactic magnetic field. Considering different possibilities for the ordinary cosmic rays the required neutrino masses are determined. In the most plausible case that the ordinary cosmic rays are of extragalactic origin and the universal radio background is strong enough to suppress high energy photons, the required neutrino mass is 0.08 eV ≤ m v 0.40 eV. The required ultrahigh energy neutrino flux should be detected in the near future by experiments such as AMANDA, RICE or the Pierre Auger Observatory.
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M3 - Conference contribution
AN - SCOPUS:4444327908
SN - 0750309342
SN - 9780750309349
T3 - Beyond the Desert 2002: Accelerator, Non-Accelerator and Space APproaches in the New Millenium - Proceedings of the 3rd International Conference on Particle Physics Beyond the Standard Model
SP - 567
EP - 587
BT - Beyond the Desert 2002
A2 - Klapdor-Kleingrothaus, H.V.
T2 - Beyond the Desert 2002: Accelerator, Non-Accelerator and Space Approaches in the New Millennium - Proceedings of the 3rd International Conference on Particle Physics Beyond the Standard Model: Accelerator, Non-Accelerator and Space Approaches
Y2 - 2 July 2002 through 7 July 2002
ER -