High-energy cosmic ray muons in the Earth’s atmosphere

Kochanov, A. A.; Sinegovskaya, T. S.; Sinegovsky, S. I.

doi:10.1134/s1063776113020143

Cited by 13 publications

(12 citation statements)

References 57 publications

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“…The calculation procedure was validated through the careful comparison with experiments of the calculated atmospheric hadron fluxes and the sea-level muon spectrum which covers the wide range of energies for different zenith angles [24,25]. Omitting details we give here a brief review of the calculation scheme aimed to introduce generalized Z-factors.…”

Section: A Outline Of the Calculation Methodsmentioning

confidence: 99%

“…In the case of the power-law cosmic-ray spectrum, the Feynman scaling for the hadron production cross sections and σ in hA = const, the function Z ab (E, h) is reduced to a constant or z ab (E) (see details in Refs. [25,33]). …”

Section: A Outline Of the Calculation Methodsmentioning

confidence: 99%

“…These models are widely employed to simulate extensive air showers (EAS) with the Monte Carlo method, and were also applied to compute the cosmic-ray hadron and muon fluxes [24,25]. Besides, in this work computation we employ also the old known hadronic model by Kimel & Mokhov (KM) [26] which was checked by comparison of the calculated atmospheric hadron and muon spectra with the experiment [24].…”

Section: Introductionmentioning

confidence: 99%

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High-energy neutrino fluxes and flavor ratio in the Earth’s atmosphere

Sinegovskaya¹,

Morozova²,

Sinegovsky³

2015

Phys. Rev. D

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We calculate the atmospheric neutrino fluxes in the energy range 100 GeV -10 PeV with the use of several known hadronic models and a few parametrizations of the cosmic ray spectra which take into account the knee. The calculations are compared with the atmospheric neutrino measurements by Frejus, AMANDA, IceCube and ANTARES. An analytic description is presented for the conventional (νµ +νµ) and (νe +νe) energy spectra, averaged over zenith angles, which can be used to obtain test data of the neutrino event reconstruction in neutrino telescopes. The sum of the calculated atmospheric νµ flux and the IceCube best-fit astrophysical flux gives the evidently higher flux as compared to the IceCube59 data, giving rise the question concerning the hypothesis of the equal flavor composition of the high-energy astrophysical neutrino flux. Calculations show that the transition from the atmospheric electron neutrino flux to the predominance of the astrophysical neutrinos occurs at 30 − 100 TeV if the prompt neutrino component is taken into consideration. The neutrino flavor ratio, extracted from the IceCube data, does not reveal the trend to increase with the energy as is expected for the conventional neutrino flux in the energy range 100 GeV -30 TeV. A depression of the ratio R νµ/νe possibly indicates that the atmospheric electron neutrino flux obtained in the IceCube experiment contains an admixture of the astrophysical neutrinos in the range 10 − 50 TeV.PACS numbers: 13.85. Tp, 95.85.Ry, 95.55.Vj

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Section: A Outline Of the Calculation Methodsmentioning

confidence: 99%

Section: A Outline Of the Calculation Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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High-energy neutrino fluxes and flavor ratio in the Earth’s atmosphere

Sinegovskaya¹,

Morozova²,

Sinegovsky³

2015

Phys. Rev. D

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“…Анизотропная компонента генерируется в распадах мюонов, пионов и каонов и имеет более мягкий спектр -это обычные (conventional) или (π, K)-нейтрино. Вторая, высокоэнергетическая компонента с более жестким спектром и слабой зависимостью от зенитного угла (квазиизотропная), генерируется в распадах тяжелых очарованных мезонов и барионов с коротким временем жизни (D, Λ c ) -это «прямые» или «быстрые» (prompt) нейтрино, которые должны дать заметный вклад при энергиях выше 400 ТэВ [Bugaev et al, 1989, Naumov et al, 1998].…”

Section: источники атмосферных нейтриноunclassified

“…Для сравнения на рис. 4, а показаны результаты расчета для другой модели рождения чарма -рекомбинационной кварк-партонной (RQPM) [Bugaev et al, 1989;Naumov, 1998]. Закрашенными треугольниками (рис.…”

Section: спектры и флейворное отношение атмосферных нейтриноunclassified

Behaviour of the high-energy neutrino flux in the Earth’s atmosphere

Kochanov¹,

Morozova

Синеговская³

et al. 2015

Solnechno-Zemnaya Fizika

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The processing of the IceCube experiment data, obtained during 988 days (2010-2013), revealed 37 high-energy neutrino-induced events with deposited energies 30 TeV - 2 PeV. The hypothesis of an astrophysical origin of these neutrinos is confirmed at the statistical confidence level of 5.7 standard deviations. To identify reliably the neutrino events, a thorough calculation of the atmospheric neutrino background is required. In this work we calculate the atmospheric neutrino spectra in the energy range 100 GeV - 10 PeV with usage of several hadronic models and a few parametrizations of the cosmic ray spectra, supported by experimental data, which take into account the knee. It is shown that rare decays of short-lived neutral каоns K0_s contribute more than a third of the total electron neutrino flux at the energies above 100 ТeV. The account for kaons production in pion-nucleus collisions increases the electron neutrino flux by 5-7 % in the energy range 10^2 -10^4 GeV. Calculated neutrino spectra agree on the whole with the measurement data. The neutrino flavor ratio, extracted from the IceCube data, possibly indicates that the conventional atmospheric electron neutrino flux obtained in the IceCube experiment contains an admixture of the astrophysical neutrinos in the range 20 − 50 TeV.

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High-energy atmospheric muon flux calculations in comparison with recent measurements

Kochanov

Morozova

Sinegovskaya

et al. 2019

J. Phys.: Conf. Ser.

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Recently the atmospheric muon spectra at high energies were reconstructed for two ranges of zenith angles, basing on the events collected with the IceCube detector. These measurements reach high energies at which the contribution to atmospheric muon fluxes from decays of short-lived hadrons is expected. Latest IceCube measurements of the high-energy atmospheric muon spectrum indicate the presence of prompt muon component at energies above 500 TeV.In this work, the atmospheric conventional muon flux in the energy range 10 GeV -10 PeV is calculated using a set of hadronic models in combination with known parameterizations of the cosmic ray spectrum by Zatsepin & Sokolskaya and by Hillas & Gaisser. The calculation of the prompt muons with use of the quark-gluon string model (QGSM) reproduces the muon data of IceCube experiment. Nevertheless, an additional contribution to the prompt muon component is required to describe the IceCube muon spectra, if a charm production model predicts the appreciably lower prompt lepton flux as compared with QGSM. This addition apparently originating from rare decay modes of the short-lived unflavored mesons η, η ′ , ρ, ω, φ, might ensure the competing contribution to the high-energy atmospheric muon flux.

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High-energy cosmic ray muons in the Earth’s atmosphere

Cited by 13 publications

References 57 publications

High-energy neutrino fluxes and flavor ratio in the Earth’s atmosphere

High-energy neutrino fluxes and flavor ratio in the Earth’s atmosphere

Behaviour of the high-energy neutrino flux in the Earth’s atmosphere

High-energy atmospheric muon flux calculations in comparison with recent measurements

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