arXiv 1109.35762011-09-16astro-ph.HEhep-exhep-ph

大气中微子的高能谱和天顶角分布

High-energy spectrum and zenith-angle distribution of atmospheric neutrinos

S. I. Sinegovsky, O. N. Petrova, T. S. Sinegovskaya

备注：: Talk presented at the 32nd ICRC (Beijing, China, 11-18 Aug. 2011), 4 pages, 7 figures
DOI：: 10.7529/ICRC2011/V04/0487

摘要：

宇宙射线粒子与空气原子核碰撞产生的介子衰变产生的高能中微子，构成了天体物理中微子探测问题的背景。核子-核碰撞中π介子，特别是K介子产生截面的高能行为的不确定性可能会对中微子通量的计算产生实质性的影响。本文计算了10 GeV ~ 10 PeV的μ子和电子大气中微子的能谱和天顶角分布。计算使用已知的强子模型（QGSJET-II-03，SIBYLL 2.1，Kimel & Mokhov）的两个主要的光谱参数化，由Gaisser & Honda和Zatsepin & Sokolskaya。计算的μ介子中微子谱与IceCube 40实验数据的比较清楚地表明，即使在能量超过100 TeV的提示中微子的贡献是不那么明显，因为纠缠的不确定性的奇怪（K介子）和魅力（D介子）粒子生产截面。给出了中微子通量计算的解析描述。

英文摘要：

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.

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