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

Fomin, Yu. A.; Калмыков, Н. Н.; Karpikov, I.; Куликов, Г. В.; Kuznetsov, M.; Рубцов, Г.; Сулаков, В. П.; Troitsky, S.

doi:10.1016/j.astropartphys.2017.04.001

Cited by 48 publications

(37 citation statements)

References 35 publications

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“…We note that, as discussed in Ref. [19], it agrees well with the composition obtained from the EAS-MSU surface-detector data [18]. More details on the MC set with hadronic primaries may be found in Ref.…”

supporting

confidence: 74%

“…The primary composition is the same as determined in Ref. [19] by fitting the observed distribution of the muon densities: 46% protons and 54% iron. The distributions of S, N e , R, θ and muon density at 100 meters ρ µ (100) are shown in Figures 7-11.…”

Section: Appendix Distribution Of Eas Parameters For Data and Monte-mentioning

confidence: 99%

“…Indeed, it is known that hadronicinteraction models used in the air-shower simulations are not perfect, in particular in the part related to the description of the muon content of EAS. While our previous study indicates [19] that the bulk of E > 10 GeV muon data of the EAS-MSU experiment is well described by the QGSJET-II-04 simulations, assuming the primary chemical composition implied by the surface-detector studies, this is not directly tested for muon-poor showers.…”

Section: A Systematic Uncertaintiesmentioning

confidence: 99%

“…For this study, the primary composition has been determined in Ref. [19] by fitting the observed distribution of the muon densities. The assumed fraction of protons is 46 ± 6%.…”

mentioning

confidence: 99%

“…[19] is the lower N e threshold which is chosen to cover a wider range of energies of potential photons. The extension of the N e range requires a new comparison of data to Monte-Carlo to validate the simulations.…”

mentioning

confidence: 99%

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Constraints on the flux of ∼(1016−1017.5) eV
Fomin
¹
,
Калмыков
²
,
Karpikov
³

et al. 2017
Phys. Rev. D
32
2
11
0
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supporting

confidence: 74%

Section: Appendix Distribution Of Eas Parameters For Data and Monte-mentioning

confidence: 99%

Section: A Systematic Uncertaintiesmentioning

confidence: 99%

“…For this study, the primary composition has been determined in Ref. [19] by fitting the observed distribution of the muon densities. The assumed fraction of protons is 46 ± 6%.…”

mentioning

confidence: 99%

mentioning

confidence: 99%

See 3 more Smart Citations

Constraints on the flux of ∼(1016−1017.5) eV
Fomin
¹
,
Калмыков
²
,
Karpikov
³

et al. 2017
Phys. Rev. D
32
2
11
0
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The Muon Puzzle in cosmic-ray induced air showers and its connection to the Large Hadron Collider

Albrecht

Cazón

Dembinski

et al. 2022

Astrophys Space Sci

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High-energy cosmic rays are observed indirectly by detecting the extensive air showers initiated in Earth’s atmosphere. The interpretation of these observations relies on accurate models of air shower physics, which is a challenge and an opportunity to test QCD under extreme conditions. Air showers are hadronic cascades, which give rise to a muon component through hadron decays. The muon number is a key observable to infer the mass composition of cosmic rays. Air shower simulations with state-of-the-art QCD models show a significant muon deficit with respect to measurements; this is called the Muon Puzzle. By eliminating other possibilities, we conclude that the most plausible cause for the muon discrepancy is a deviation in the composition of secondary particles produced in high-energy hadronic interactions from current model predictions. The muon discrepancy starts at the TeV scale, which suggests that this deviation is observable at the Large Hadron Collider. An enhancement of strangeness production has been observed at the LHC in high-density events, which can potentially explain the puzzle, but the impact of the effect on forward produced hadrons needs further study, in particular with future data from oxygen beam collisions.

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The Giant Radio Array for Neutrino Detection (GRAND): Science and design

Álvarez-Muñiz

Batista

Balagopal

et al. 2019

Sci. China Phys. Mech. Astron.

255

279

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The Giant Radio Array for Neutrino Detection (GRAND) 1 is a planned large-scale observatory of ultra-highenergy (UHE) cosmic particles -cosmic rays, gamma rays, and neutrinos with energies exceeding 10 8 GeV. Its ultimate goal is to solve the long-standing mystery of the origin of UHE cosmic rays. It will do so by detecting an unprecedented number of UHECRs and by looking with unmatched sensitivity for the undiscovered UHE neutrinos and gamma rays associated to them. Three key features of GRAND will make this possible: its large exposure at ultra-high energies, sub-degree angular resolution, and sensitivity to the unique signals made by UHE neutrinos.The strategy of GRAND is to detect the radio emission coming from large particle showers that develop in the terrestrial atmosphereextensive air showers -as a result of the interaction of UHE cosmic rays, gamma, rays, and neutrinos. To achieve this, GRAND will be the largest array of radio antennas ever built. The relative affordability of radio antennas makes the scale of construction possible. GRAND will build on years of progress in the field of radio-detection and apply the large body of technological, theoretical, and numerical advances, for the first time, to the radio-detection of air showers initiated by UHE neutrinos.The design of GRAND will be modular, consisting of several independent sub-arrays, each of 10 000 radio antennas deployed over 10 000 km 2 in radio-quiet locations. A staged construction plan ensures that key techniques are progressively validated, while simultaneously achieving important science goals in UHECR physics, radioastronomy, and cosmology early during construction.Already by 2025, using the first sub-array of 10 000 antennas, GRAND could discover the long-sought cosmogenic neutrinos -produced by interactions of ultra-high-energy cosmic-rays with cosmic photon fields -if their flux is as high as presently allowed, by reaching a sensitivity comparable to planned upgraded versions of existing experiments. By the 2030s, in its final configuration of 20 sub-arrays, GRAND will reach an unparalleled sensitivity to cosmogenic neutrino fluxes of 4 • 10 −10 GeV cm −2 s −1 sr −1 within 3 years of operation, which will guarantee their detection even if their flux is tiny. Because of its sub-degree angular resolution, GRAND will also search for point sources of UHE neutrinos, steady and transient, potentially starting UHE neutrino astronomy. Because of its access to ultra-high energies, GRAND will chart fundamental neutrino physics at these energies for the first time.GRAND will also be the largest detector of UHE cosmic rays and gamma rays. It will improve UHECR statistics at the highest energies ten-fold within a few years, and either discover UHE gamma rays or improve their limits ten-fold. Further, it will be a valuable tool in radioastronomy and cosmology, allowing for the discovery and follow-up of large numbers of radio transients -fast radio bursts, giant radio pulses -and for precise studies of the epoch of reionization.Following the disc...

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

Cited by 48 publications

References 35 publications

Constraints on the flux of ∼(1016−1017.5) eV
Fomin
¹
,
Калмыков
²
,
Karpikov
³

et al. 2017
Phys. Rev. D
32
2
11
0
View full text Add to dashboard Cite

Constraints on the flux of ∼(1016−1017.5) eV
Fomin
¹
,
Калмыков
²
,
Karpikov
³

et al. 2017
Phys. Rev. D
32
2
11
0
View full text Add to dashboard Cite

The Muon Puzzle in cosmic-ray induced air showers and its connection to the Large Hadron Collider

The Giant Radio Array for Neutrino Detection (GRAND): Science and design

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

Cited by 48 publications

References 35 publications

Constraints on the flux of ∼(1016−1017.5) eVFomin1, Калмыков2, Karpikov3 et al. 2017Phys. Rev. D322110View full textAdd to dashboardCite

Constraints on the flux of ∼(1016−1017.5) eVFomin1, Калмыков2, Karpikov3 et al. 2017Phys. Rev. D322110View full textAdd to dashboardCite

The Muon Puzzle in cosmic-ray induced air showers and its connection to the Large Hadron Collider

The Giant Radio Array for Neutrino Detection (GRAND): Science and design

Contact Info

Product

Resources

About

Constraints on the flux of ∼(1016−1017.5) eV
Fomin
¹
,
Калмыков
²
,
Karpikov
³

et al. 2017
Phys. Rev. D
32
2
11
0
View full text Add to dashboard Cite

Constraints on the flux of ∼(1016−1017.5) eV
Fomin
¹
,
Калмыков
²
,
Karpikov
³

et al. 2017
Phys. Rev. D
32
2
11
0
View full text Add to dashboard Cite