High-energy cosmic-ray fluxes in the Earth atmosphere: Calculations vs experiments

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

doi:10.1016/j.astropartphys.2008.09.008

Cited by 47 publications

(52 citation statements)

References 79 publications

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“…In similar fashion meson cascade equations can be solved using the nucleon and meson sources [24]. The main pion sources in the atmospheric shower are the interactions of nucleons and pions with air nuclei and kaon decays.…”

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: Introductionmentioning

confidence: 99%

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

Sinegovskaya¹,

Morozova²,

Sinegovsky³

2015

Phys. Rev. D

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“…Between a few hundred GeV and 3 TeV, and again from 100 TeV to 1 PeV, there are large gaps where experimental measurements of individual primary fluxes are sparse and contain substantial uncertainties [20]. Especially the second region is of high importance to IceCube physics, because it corresponds to neutrino energies of tens of TeV where indications for astrophysical fluxes start to become visible.…”

Section: Cosmic Rays In the Icecube Energy Rangementioning

confidence: 99%

Characterization of the atmospheric muon flux in IceCube

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

Astroparticle Physics

101

117

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Muons produced in atmospheric cosmic ray showers account for the by far dominant part of the event yield in large-volume underground particle detectors. The IceCube detector, with an instrumented volume of about a cubic kilometer, has the potential to conduct unique investigations on atmospheric muons by exploiting the large collection area and the possibility to track particles over a long distance. Through detailed reconstruction of energy deposition along the tracks, the characteristics of muon bundles can be quantified, and individual particles of exceptionally high energy identified. The data can then be used to constrain the cosmic ray primary flux and the contribution to atmospheric lepton fluxes from prompt decays of short-lived hadrons.In this paper, techniques for the extraction of physical measurements from atmospheric muon events are described and first results are presented. The multiplicity spectrum of TeV muons in cosmic ray air showers for primaries in the energy range from the knee to the ankle is derived and found to be consistent with recent results from surface detectors. The single muon energy spectrum is determined up to PeV energies and shows a clear indication for the 2 emergence of a distinct spectral component from prompt decays of short-lived hadrons. The magnitude of the prompt flux, which should include a substantial contribution from light vector meson di-muon decays, is consistent with current theoretical predictions.The variety of measurements and high event statistics can also be exploited for the evaluation of systematic effects. In the course of this study, internal inconsistencies in the zenith angle distribution of events were found which indicate the presence of an unexplained effect outside the currently applied range of detector systematics. The underlying cause could be related to the hadronic interaction models used to describe muon production in air showers.

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“…In this case, due to the higher slope of the energy spectrum of the primary particles (a coefficient of the slope of the difference spectrum is γ = 2.75) the generation of secondary particles (π ± -mesons and K ± -mesons) with the highest energies is of importance. It was shown [8] that the QGSJET II-03 model [4] leads to a spectrum of vertical muons, the intensity of which is about a factor f = 1.5 times less than the data of collaborations L3 + Cosmic [9], MACRO [10] and LVD [11]. The result [8] was obtained as a solution of transport equations.…”

Section: Introductionmentioning

confidence: 99%

“…It was shown [8] that the QGSJET II-03 model [4] leads to a spectrum of vertical muons, the intensity of which is about a factor f = 1.5 times less than the data of collaborations L3 + Cosmic [9], MACRO [10] and LVD [11]. The result [8] was obtained as a solution of transport equations. The π ± and K ± mesons decay into µ ± -mesons.…”

Section: Introductionmentioning

confidence: 99%

Constraints of hadronic interaction models from the cosmic muon observations

Dedenko

Lukyashin

Fedorova

et al. 2015

EPJ Web of Conferences

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Abstract.A simple method of the vertical muon energy spectrum simulations has been suggested. These calculations have been carried out in terms of various models of hadronic interactions. The most energetic π ± -mesons and K ± -mesons produced in hadron interactions contribute mainly to this energy spectrum of muons due to the very steep energy spectrum of the primary particles. So, some constraints on the hadronic interaction models may be set from a comparison of calculated results with cosmic data on the vertical muon energy spectrum. This comparison showed that the most energetic secondary particles production is too high in the case of the QGSJET II-04 model and rather low in the case of the QGSJET II-03 model. These conclusion have been supported by the LHC data.

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High-energy cosmic-ray fluxes in the Earth atmosphere: Calculations vs experiments

Cited by 47 publications

References 79 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

Characterization of the atmospheric muon flux in IceCube

Constraints of hadronic interaction models from the cosmic muon observations

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