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Abstract
The high-energy conventional atmospheric neutrino fluxes are calculated with the hadronic interaction models: Kimel & Mokhov, QGSJET II-03(04), SIBYL 2.1(2.3), EPOS LHC. The influence of hadron-nuclear interactions on the neutrino flux ratios, \(v/\bar{v},({v}_{\mu }+{\bar{v}}_{\mu })/({v}_{e}+{\bar{v}}_{e})\), is studied. A comparison of calculations obtained with use of two different approaches, \({\mathscr{Z}}(E,h)\) -functions method and the Matrix Cascade Equations (MCEQ), demonstrates close agreement in whole but some of partial contrubutions. The comparison of calculated muon neutrino spectra with the latest experimental data justifies reliability of performed computation which describes correctly the atmospheric neutrino production. The calculation made with the model EPOS LHC, combined with Hillas & Gaisser parametrization of the cosmic ray spectrum, is in close agreement with the best fit of IceCube for energy spetrum of atmospheric muon neutrinos in the energy range 1–500 TeV.
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Details
1 Lomonosov Moscow State University, Leninskie Gory, 1, Moscow, 119991, Russia
2 Institute of Solar-Terrestrial Physics SB RAS, Lermontov str. 126a, Irkutsk, Russia; Irkutsk State University, Gagarin blv. 20, Irkutsk, 664003, Russia
3 Irkutsk State Transport University, Chernyshevskiy str. 15, Irkutsk, 664074, Russia
4 Irkutsk State University, Gagarin blv. 20, Irkutsk, 664003, Russia; Joint Institute for Nuclear Research, Joliot-Curie, 6, Dubna, Moscow region, 141980, Russia