Mass composition of cosmic rays determined by the muon fraction with 
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 in air showers with energy greater than 5 EeV

Кнуренко, С. П.; Petrov, Igor

doi:10.1103/physrevd.102.023036

Cited by 11 publications

(7 citation statements)

References 42 publications

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“…In Figure 2: Dependence of muon flux density 〈ρ µ (600)〉 on energy E 0 . Lines are calculation for QGSjetII-04 and EPOS LHC for proton and iron nucleus our opinion, this can be done using formula (1), where E 0 is determined by the parameter ρ µ (600) [17].…”

Section: Correlation Of ρ µ (600) With Air Shower Energymentioning

confidence: 99%

Muons in showers with energy $E_{0} \geq$ 5 EeV and QGSjetII-04 and EPOS LHC models of hadronic interactions. Is there a muon deficit in the models?

Кнуренко¹,

Petrov²

2022

Preprint

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The paper presents data on the muon component with a threshold thr ≥ 1 GeV. Air showers were registered at the Yakutsk array during almost 50 years of continuous air shower observations. The characteristics of muons are compared with calculations of QGSjetII-04 and EPOS LHC models for a proton and an iron nucleus. There is a muon deficit in the models, at energies greater than 5 EeV. To make an agreement between experimental data and simulations on muons, further tuning of the models is required.

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Section: Correlation Of ρ µ (600) With Air Shower Energymentioning

confidence: 99%

Muons in showers with energy $E_{0} \geq$ 5 EeV and QGSjetII-04 and EPOS LHC models of hadronic interactions. Is there a muon deficit in the models?

Кнуренко¹,

Petrov²

2022

Preprint

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“…The mass composition of the primary UHECRs is still a matter of debate even if it was extensively studied by combining different complementary techniques [19][20][21][22][23]. The most reliable parameter from the EAS used to infer the mass composition proved to be X max , the atmospheric depth where the energy deposit profile of the secondary particles reaches its maximum [24].…”

Section: Introductionmentioning

confidence: 99%

Mass Composition of UHECRs from Xmax Distributions Recorded by the Pierre Auger and Telescope Array Observatories

Arsene

2021

Universe

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In this paper we infer the mass composition of the ultra high energy cosmic rays (UHECRs) from measurements of Xmax distributions recorded at the Pierre Auger (2014) and Telescope Array (TA) (2016) Observatories, by fitting them with all possible combinations of Monte Carlo (MC) templates from a large set of primary species (p, He, C, N, O, Ne, Si and Fe), as predicted by EPOS-LHC, QGSJETII-04 and Sibyll 2.1 hadronic interaction models. We use the individual fractions of nuclei reconstructed from one experiment in each energy interval to build equivalent MC Xmax distributions, which we compare with the experimental Xmax distributions of the other experiment, applying different statistical tests of compatibility. The results obtained from both experiments confirm that the mass composition of the UHECRs is dominated (≳70%) by protons and He nuclei in the energy range investigated lgE(eV) = [17.8–19.3] (Auger) and lgE(eV) = [18.2–19.0] (TA). The indirect comparisons between the Xmax distributions recorded by the two experiments show that the degree of compatibility of the two datasets is good, even excellent in some high energy intervals, especially above the ankle (lgE(eV)∼18.7). However, our study reveals that, at low energies, further effort in data analysis is required in order to harmonize the results of the two experiments.

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“…In this paper, we focus exclusively on the pulse shape of the Cherenkov radiation signal from EAS. Residual aspects concerning other components of the phenomenon are covered in previous papers of the Yakutsk array group [6,[17][18][19][20].…”

Section: Introductionmentioning

confidence: 99%

Measuring temporal characteristics of the Cherenkov radiation signal from extensive air showers of cosmic rays with a wide field-of-view telescope addendum to the Yakutsk array

Ivanov,

Matarkin,

Timofeev

2021

Preprint

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A wide field-of-view Cherenkov telescope has been working in the surroundings of the Yakutsk array experiment since 2012. Its main function is to measure the waveform of the Cherenkov radiation signal induced by extensive air showers of cosmic rays. Analysis of the dataset collected by telescope is intended for the reconstruction of the parameters of the development of the shower in addition to the main shower characteristics measured by the rest of the array detectors. In this paper, the observed duration of the Cherenkov radiation signal as a function of the shower core distance is used to estimate the depth of the shower maximum in a different way, based on the results of model simulations.

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Mass composition of cosmic rays determined by the muon fraction with ϵthr≥1 GeV in air showers with energy greater than 5 EeV

Cited by 11 publications

References 42 publications

Muons in showers with energy $E_{0} \geq$ 5 EeV and QGSjetII-04 and EPOS LHC models of hadronic interactions. Is there a muon deficit in the models?

Muons in showers with energy $E_{0} \geq$ 5 EeV and QGSjetII-04 and EPOS LHC models of hadronic interactions. Is there a muon deficit in the models?

Mass Composition of UHECRs from Xmax Distributions Recorded by the Pierre Auger and Telescope Array Observatories

Measuring temporal characteristics of the Cherenkov radiation signal from extensive air showers of cosmic rays with a wide field-of-view telescope addendum to the Yakutsk array

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