Influence of hadronic interaction models on characteristics of the high-energy atmospheric neutrino flux

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.