2014/04/30 by K. Ioka, Kunihito Ioka, Kohta Murase +1 · 117 citations
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #COSMIC cancer database #Cosmic neutrino background #Cosmic ray #Coupling (piping) #Dark Matter and Cosmic Phenomena #Flux (metallurgy) #Neutrino #Neutrino Physics Research #Neutrino astronomy #Solar neutrino problem #astro-ph.HE #hep-ph
paper · pdf · doi:10.1093/ptep/ptu090
published in Progress of Theoretical and Experimental Physics 2014(6), 61E01-0 (University of Oxford) · 6 pages, 2 figures, final version to be published in PTEP
arxiv created 2014/06/06 · openalex publication_date 2014/06/23 · arxiv updated 2015/04/23 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We show that the PeV neutrinos detected by IceCube put unique constraints on “secret” interactions of neutrinos with the cosmic neutrino background (C|ν |B). The coupling must be |g <0.03| for the mediating boson mass |mX \lesssim 2| MeV, |g/mX < 5| GeV|-1| for |mX \gtrsim 20| MeV, and |g/mX < 0.07| GeV|-1| in between. We also investigate the possibility that neutrino cascades degrade high-energy neutrinos to PeV energies by upgrading C|ν |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.