Constraints of hadronic interaction models from the cosmic muon observations

Dedenko, L. G.; Lukyashin, A. V.; Fedorova, G. F.; Роганова, Т. М.

doi:10.1051/epjconf/20159910003

Cited by 13 publications

(10 citation statements)

References 20 publications

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“…atmospheric muons [27], and it has been reported in [28] that QGSJET-II-04 seems to overestimate the number of muons in this regime. Preliminary results of the KASCADE-Grande experiment (110 m a.s.l., 1022 g/cm 2 ) at E ∼ 10 17 eV suggest [29] that the atmospheric attenuation of the muon number (E µ 0.23 GeV, r/R 0 3) is underestimated by all high-energy hadronic interaction models studied there, including QGSJET-II-04.…”

Section: Discussionmentioning

confidence: 99%

No muon excess in extensive air showers at 100–500 PeV primary energy: EAS–MSU results

Fomin

Калмыков

Karpikov

et al. 2017

Astroparticle Physics

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Some discrepancies have been reported between observed and simulated muon content of extensive air showers: the number of observed muons exceeded the expectations in HiRes-MIA, Yakutsk and Pierre Auger Observatory data. Here, we analyze the data of the Moscow State University Extensive Air Shower (EAS-MSU) array on E µ 10 GeV muons in showers caused by ∼ (10 17 − 10 18 ) eV primary particles and demonstrate that they agree with simulations (QGSJET-II-04 hadronic interaction model) once the primary composition inferred from the surface-detector data is assumed.

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Section: Discussionmentioning

confidence: 99%

No muon excess in extensive air showers at 100–500 PeV primary energy: EAS–MSU results

Fomin

Калмыков

Karpikov

et al. 2017

Astroparticle Physics

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“…We are sorry that some our results of models testing in [33][34][35] are not correct. We do apologize for our mistake in input data for the atmosphere.…”

Section: Introductionmentioning

confidence: 79%

“…As the energy per nucleon is of importance only the energy spectra of the primary protons and helium nuclei should be taken into account. We had used approximations (1) for (dI p /dE) and (dI He /dE) suggested in [37].…”

Section: Methodsmentioning

confidence: 99%

Testing of the VENUS 4.12, DPMJET 2.55, QGSJET II-03 and SIBYLL 2.3 hadronic interaction models via help of the atmospheric vertical muon spectra

et al. 2017

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Abstract.Uncertainties of the model energy spectra of the most energetic secondary π ± -mesons (and K ± -mesons) are discussed. Computer simulations of the partial energy spectra of the atmospheric vertical muons induced by primary cosmic particles with various fixed energies in interval 10 2 −10 7 GeV in terms of the VENUS 4.12, DPMJET 2.55, QGSJET II-03 and SIBYLL 2.3 models had been carried out with help of CORSIKA package. These partial spectra should be convoluted with the contemporary spectra of the primary cosmic particles. Results of simulations are compared with the contemporary atmospheric vertical muon flux data. Comparison shows that all models underestimate production of secondary π ± -mesons (and K ± -mesons) by factor of ∼ 2 at the most high energies. This underestimation induces more rapid development of extensive air showers in the atmosphere and results in uncertainties in estimates of energy and composition of the primary cosmic particles.

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“…We are sorry that our testing of some models in [26][27][28] are not correct. We do apologize for our mistake in input data for the atmosphere!…”

Section: Introductionmentioning

confidence: 89%

Testing the QGSJET01 and QGSJETII-04 models with the help of atmospheric muons

et al. 2017

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Abstract. More accurate original calculations of the atmospheric vertical muon energy spectra at energies 10 2 − 10 5 GeV have been carried out in terms of the QGSJET01 and QGSJETII-04 models. The GaisserHonda approximations of the measured energy spectra of primary protons, helium and nitrogen nuclei have been used. The CORSIKA package has been used to simulate cascades in the standard atmosphere induced by different primary particles with various fixed energies E. Statistics of simulated cascades for secondary particles with energies (0.01 − 1) · E was increased up to 10 6 . It has been shown that predictions of the QGSJET01 and QGSJETII-04 models for these muon fluxes are below the data of the classical experiments L3 + Cosmic, MACRO and LVD by factors of ∼ 1.7-2 at energies above 10 2 GeV. It has been concluded that these tested models underestimate the production of the most energetic secondary particles, namely, π -mesons and K -mesons, in interactions of primary protons and other primary nuclei with nuclei in the atmosphere by the same factors.

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Constraints of hadronic interaction models from the cosmic muon observations

Cited by 13 publications

References 20 publications

No muon excess in extensive air showers at 100–500 PeV primary energy: EAS–MSU results

No muon excess in extensive air showers at 100–500 PeV primary energy: EAS–MSU results

Testing of the VENUS 4.12, DPMJET 2.55, QGSJET II-03 and SIBYLL 2.3 hadronic interaction models via help of the atmospheric vertical muon spectra

Testing the QGSJET01 and QGSJETII-04 models with the help of atmospheric muons

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