Neutrinos from propagation of ultrahigh-energy protons
By Ralph Engel, D. Seckel, Todor Stanev. 2001
346 citations recorded by the source corpus.
We present a calculation of the production of neutrinos during propagation of ultra-high energy cosmic rays from their astrophysical sources to us. Photoproduction interactions are modeled with the event generator SOPHIA that represents very well the experimentally measured particle production cross sections at accelerator energies. We give the fluxes expected from different assumptions on cosmic ray source distributions, cosmic ray injection spectra, cosmological evolution of the sources and different cosmologies, and compare them to the Waxman-Bahcall limit on source neutrinos. We estimate rates for detection of neutrino induced showers in a km3 water detector. The ratio of the local high energy neutrino flux to the ultra-high energy cosmic ray flux is a crucial parameter in distinguishing between astrophysical and cosmological (top-down) scenarios of the ultra-high energy cosmic ray origin.
Subfields: Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/4e959a2075ea54a8cb56485a8f6c2adbe398b38f
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In Nuclear and High Energy Physics
Citations in the corpus
- IceCube-Gen2: the window to the extreme Universe (2020, neutral): “, [44, 63–81]).”
- Cosmogenic neutrinos: parameter space and detectabilty from PeV to ZeV (2010, background): “…2006; Stanev et al., 2006; Allard et al., 2006; Takami et al., 2009, and see Anchordoqui and Montaruli, 2009 for a recent review): in particular, Engel et al. (2001) and Ave et al. (2005) calculated analytically and semi-analytically the expected neutrino flux around PeV energies, considering…”
- The POEMMA (Probe of Extreme Multi-Messenger Astrophysics) observatory (2020, neutral): “The cosmogenic flux depends on the nuclear composition of UHECRs [88–97] providing another way to measure”
- The Astrophysics of Ultrahigh-Energy Cosmic Rays (2011, background): “A number of authors have estimated the cosmogenic neutrino flux with varying assumptions (e.g., Engel et al. 2001; Ave et al. 2005; Seckel & Stanev 2005; Hooper et al. 2005; Berezinsky 2006; Stanev et al. 2006; Allard et al. 2006; Takami et al. 2009; Kotera et al. 2010b).”