Influence of Cosmic-Ray Spectrum and Hadron-Nucleus Interaction Model on the Properties of High-Energy Atmospheric-Neutrino Fluxes

被引：0
作者：
Morozova, A. D. [1 ,2 ]
Kochanov, A. A. [3 ,4 ]
Sinegovskaya, T. S. [5 ]
Sinegovsky, S., I [2 ,4 ]
机构：
[1] Moscow MV Lomonosov State Univ, Moscow 119991, Russia
[2] Joint Inst Nucl Res, Dubna 141980, Moscow Oblast, Russia
[3] Russian Acad Sci, Siberian Branch, Inst Solar Terr Phys, Irkutsk 664033, Russia
[4] Irkutsk State Univ, Irkutsk 664003, Russia
[5] Irkutsk State Transport Univ, Irkutsk 664074, Irkutskaya Obla, Russia
来源：
PHYSICS OF ATOMIC NUCLEI | 2019年 / 82卷 / 05期
关键词：
GLUON-STRING MODEL; CHARMED PARTICLES;
D O I：
10.1134/S1063778819040136
中图分类号：
O57 [原子核物理学、高能物理学];
学科分类号：
070202 ;
摘要：
The neutrino/antineutrino flux ratios (nu(e)/(nu) over bar (e) and nu(mu)/(nu) over bar (mu)) and the flavor ratio (nu(mu)/(nu) over bar (mu))/(nu(e)/(nu) over bar (e)) clearly demonstrate the distinctions between the predictions of hadronic-interaction models for the production spectra of pions and kaons, which are the main sources of atmospheric neutrinos in the region of E-nu less than or similar to 500 TeV. The values of the nu/(nu) over bar ratio are sensitive to variations in the pi(+)/pi(-), pi/K, and K+/K- meson ratios, which are determined by the cross sections for inclusive meson-production processes in hadron-nucleus (hA) collisions; the elemental composition of cosmic rays also exerts influence, through the p/n ratio, on the development of hadronic cascades and on the neutrino ratios. The difference in nu/(nu) over bar. and in the flavor ratio for a number of hadronic-interaction models is shown on the basis of calculating neutrino fluxes at energies in the range between 10(2) and 10(8) GeV. A comparison of the calculated results with new experimental data shows the reliability of this calculation, which, on the whole, reflects correctly the mechanism of atmospheric-neutrino production. The spectra of atmospheric muon neutrinos from calculations based on the Kimel-Mokhov, SIBYLL 2.1, and EPOS LHC models describe fairly well experimental results. At energies in the range of 1- 500 TeV, the curves calculated within these models combined with the Hillas-Gaisser spectrum are close to the best fit to data from measurements in the IceCube experiment.
引用
收藏
页码：491 / 497
页数：7
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