  High-energy neutrinos, arising from decays of mesons produced through the
collisions of cosmic ray particles with air nuclei, form the background in the
astrophysical neutrino detection problem. An ambiguity in high-energy behavior
of pion and especially kaon production cross sections for nucleon-nucleus
collisions may affect essentially the calculated neutrino flux. We present
results of the calculation of the energy spectrum and zenith-angle distribution
of the muon and electron atmospheric neutrinos in the energy range 10 GeV to 10
PeV. The calculation was performed with usage of known hadronic models
(QGSJET-II-03, SIBYLL 2.1, Kimel & Mokhov) for two of the primary spectrum
parametrizations, by Gaisser & Honda and by Zatsepin & Sokolskaya. The
comparison of the calculated muon neutrino spectrum with the IceCube40
experiment data make it clear that even at energies above 100 TeV the prompt
neutrino contribution is not so apparent because of tangled uncertainties of
the strange (kaons) and charm (D-mesons) particle production cross sections. An
analytic description of calculated neutrino fluxes is presented.
