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Relic Neutrino Background from Cosmic-Ray Reservoirs
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abstract
We compute the flux of relic neutrino background (R$\nu$B) up-scattered by ultra-high-energy (UHE) cosmic rays (CRs) in clusters that act as CR-reservoirs. The long trapping times of UHECRs make this flux larger than that of R$\nu$B up-scattered by UHECRs on their way to Earth, which we also compute. We find that IceCube excludes R$\nu$B weighted overdensities larger than $10^{10}$ in clusters, and that PUEO, RNO-G, GRAND and IceCube-Gen2 will test values down to $10^{8}$. Our treatment incorporates the momentum transfer dependence of the neutrino-nucleus cross section, deep inelastic scattering, a mixed UHECR composition, and flavour information on the up-scattered R$\nu$B fluxes for both cases of neutrino mass spectrum with normal and inverted ordering, providing new handles to possibly disentangle the up-scattered R$\nu$B from cosmogenic neutrinos.
Forward citations
Cited by 2 Pith papers
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The Cosmic Neutrino Background is within Reach of Future Neutrino Telescopes
Including deep-inelastic scattering makes cosmic-ray-boosted relic neutrinos bright enough for IceCube to bound the CνB overdensity to ~100–1000, and future networks could reach the ΛCDM value.
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High-Energy Neutrinos from Cosmic-Ray Scatterings with Supernova Neutrinos
Cosmic-ray boosted supernova neutrinos could be detectable in optimistic astrophysical scenarios and yield a bound of about 30 TeV on the extra-dimensional scale.
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