Cosmogenic neutrinos: parameter space and detectabilty from PeV to ZeV
By Kumiko Kotera, D. Allard, Angela V. Olinto. 2010
251 citations recorded by the source corpus.
While propagating from their source to the observer, ultrahigh energy cosmic rays interact with cosmological photon backgrounds and generate to the so-called ``cosmogenic neutrinos''. Here we study the parameter space of the cosmogenic neutrino flux given recent cosmic ray data and updates on plausible source evolution models. The shape and normalization of the cosmogenic neutrino flux are very sensitive to some of the current unknowns of ultrahigh energy cosmic ray sources and composition. We investigate various chemical compositions and maximum proton acceleration energies Ep,max which are allowed by current observations. We consider different models of source evolution in redshift and three possible scenarios for the Galactic to extragalactic transition. We summarize the parameter space for cosmogenic neutrinos into three regions: an optimistic scenario that is currently being constrained by observations, a plausible range of models in which we base many of our rate estimates, and a pessimistic scenario that will postpone detection for decades to come. We present the implications of these three scenarios for the detection of cosmogenic neutrinos from PeV to ZeV (1014−21 eV) with the existing and upcoming instruments. In the plausible range of parameters, the narrow flux variability in the EeV energy region assures low but detectable rates for IceCube (0.06–0.2 neutrino per year) and the Pierre Auger Observatory (0.03–0.06 neutrino per year), and detection should happen in the next decade. If EeV neutrinos are detected, PeV information can help select between competing models of cosmic ray composition at the highest energy and the Galactic to extragalactic transition at ankle energies. With improved sensitivity, ZeV neutrino observatories, such as ANITA and JEM-EUSO could explore and place limits on the maximum acceleration energy.
Subfields: Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/000c4b69be59a2990d710568a563af904098badb
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In Nuclear and High Energy Physics
Citations in the corpus
- The POEMMA (Probe of Extreme Multi-Messenger Astrophysics) observatory (2020, background): “The cosmogenic flux depends on the nuclear composition of UHECRs [89–98] providing another way to measure it [96, 99].”
- The Astrophysics of Ultrahigh-Energy Cosmic Rays (2011, methodology): “…LE,19 & 3 × 1044 erg s−1(d/100 Mpc)−2 and LE,19 & 1043 erg s−1(d/100 Mpc)−2 for E > 1019 eV could be detected by current instruments such as H.E.S.S. and by the future CTA respectively, with fluxes of order ∼ 10−10 GeV cm−2 s−1 around 1−10 TeV (Ferrigno et al. 2004; Kotera et al. 2010a).”
- Open Questions in Cosmic-Ray Research at Ultrahigh Energies (2019, unknown): “Their flux mainly depends on the chemical composition, maximum energy of UHECRs, and the source evolution model (e.g., Takami et al., 2009; Kotera et al., 2010; see Hooper et al., 2005; Anchordoqui et al., 2008 for secondaries from heavy nuclei).”
- IceCube-Gen2: the window to the extreme Universe (2020, background): “emely well motivated, its level depends strongly on the composition of the CR [241, 242], the cosmic evolution of the sources, the spectral index of the sources, and their maximum acceleration energy [71, 72]. IceCube can already exclude scenarios firm conclusions much larger exposures are needed. Th”
- OBSERVATION AND CHARACTERIZATION OF A COSMIC MUON NEUTRINO FLUX FROM THE NORTHERN HEMISPHERE USING SIX YEARS OF ICECUBE DATA (2016, background): “A flux of cosmogenic neutrinos as predicted by Kotera et al. (2010) would only contribute subdominantly to the measured astrophysical neutrino flux.”