IceCube PeV-EeV neutrinos and secret interactions of neutrinos
By K. Ioka, Kohta Murase. 2014
135 citations recorded by the source corpus.
We show that the PeV neutrinos detected by IceCube put unique constraints on "secret" interactions of neutrinos with the cosmic neutrino background (C$\nu$B). The coupling must be $g <0.03$ for the mediating boson mass $m_{X} \lesssim 2$ MeV, $g/m_{X} < 5$ GeV$^{-1}$ for $m_{X} \gtrsim 20$ MeV, and $g/m_{X} < 0.07$ GeV$^{-1}$ in between. We also investigate the possibility that neutrino cascades degrade high-energy neutrinos to PeV energies by upgrading C$\nu$B where the energy flux of PeV neutrinos can coincide with the Waxman-Bahcall bound or the cosmogenic neutrino flux for protons, thanks to energy conservation. However a large coupling is required, which is disfavored by laboratory decay constraints. The suppression of PeV-EeV neutrinos is a testable prediction for the Askaryan Radio Array.
Subfields: Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/562803d6c13a476de374ad566b03abebf750185e
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In Nuclear and High Energy Physics
Citations in the corpus
- IceCube-Gen2: the window to the extreme Universe (2020, background): “are coherent interactions between neutrinos and dark matter [327–333]; neutrinos and dark energy [334]; very-long-range Le − Lμ and Le − Lτ gauged interactions sourced by the universe’s electron content [286, 335–337]; and new interactions between high-energy cosmic neutrinos and low-energy relic ne”
- Open Questions in Cosmic-Ray Research at Ultrahigh Energies (2019, unknown): “…of different types can affect all neutrino observables: the energy spectrum (see e.g., Baerwald et al., 2012; Blum et al., 2014; Ibe and Kaneta, 2014; Ioka and Murase, 2014; Ng and Beacom, 2014; Kopp et al., 2015; Bustamante et al., 2017), distribution of arrival directions (see e.g., Davis and…”
- The POEMMA (Probe of Extreme Multi-Messenger Astrophysics) observatory (2020, methodology): “This has been studied before in the context of supernova neutrinos and TeV–PeV astrophysical neutrinos [110, 120–129].”