Investigating cosmic rays and air shower physics with IceCube/IceTop

Dembinski, H.-P.

doi:10.1051/epjconf/201714501003

Cited by 4 publications

(2 citation statements)

References 24 publications

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“…The most recent SIBYLL model including this effect finds indeed a significant enhancement in the number of muons produced in the shower [101]. Note that since the suppression of the electromagnetic component by an enhanced ρ 0 production is a cumulative effect, depending on the number of generations of hadronic interactions that happen before the charged pions decay, the muon excess is expected to be reduced for lower energy primaries, and indeed no indications of a significant muon excess have been reported at energies below 0.1 EeV (although there is always an interplay between the expected number of muons and the inferred CR composition) [102,103].…”

Section: Proton Cross Section and Air Shower Muon Contentmentioning

confidence: 99%

Progress in high-energy cosmic ray physics

Mollerach

Roulet

2018

Progress in Particle and Nuclear Physics

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We review some of the recent progress in our knowledge about high-energy cosmic rays, with an emphasis on the interpretation of the different observational results. We discuss the effects that are relevant to shape the cosmic ray spectrum and the explanations proposed to account for its features and for the observed changes in composition. The physics of air-showers is summarized and we also present the results obtained on the proton-air cross section and on the muon content of the showers. We discuss the cosmic ray propagation through magnetic fields, the effects of diffusion and of magnetic lensing, the cosmic ray interactions with background radiation fields and the production of secondary neutrinos and photons. We also consider the cosmic ray anisotropies, both at large and small angular scales, presenting the results obtained from the TeV up to the highest energies and discuss the models proposed to explain their origin.Comment: 48 pages, to appear in Progress in Particle and Nuclear Physics (2017

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Section: Proton Cross Section and Air Shower Muon Contentmentioning

confidence: 99%

Progress in high-energy cosmic ray physics

Mollerach

Roulet

2018

Progress in Particle and Nuclear Physics

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“…Although simulations using recent hadronic models can provide a good overall description of EAS, it has been observed by cosmic ray experiments that the hadronic models fail on describing the muon production in EAS. Measurements by HiRes-MIA [3], Pierre Auger Observatory [4][5][6][7], Telescope Array [8], KASCADE-Grande [9], IceTop/IceCube [10] and Sugar [11] show that there is an inconsistency between data and simulations for observables related to the muonic component of air showers. In particular, the number of muons (N µ ) obtained from simulations is observed to be significantly smaller than the measured ones, which is known as the "muon deficit problem".…”

Section: Introductionmentioning

confidence: 99%

Recent results from the cosmic ray program of the NA61/SHINE experiment

Prado

2019

EPJ Web Conf.

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NA61/SHINE is a fixed target experiment designed to study hadron-proton, hadron-nucleus and nucleus-nucleus interactions at the CERN Super-Proton-Synchrotron. In this paper we summarize the results from pion-carbon collisions recorded at beam momenta of 158 and 350 GeV/c. Hadron production measurements in this type of interactions is of fundamental importance for the understanding of the muon production in extensive air showers. In particular, production of (anti)baryons and ρ 0 are mechanisms responsible for increasing the number of muons which reaches the ground. The underestimation of the (anti)baryons or ρ 0 production rates in current hadronic interaction models could be one of the sources of the excess of muons observed by cosmic ray experiments. The results on the production spectra of π ± , K ± , p,p, Λ,Λ, K 0 S , ρ 0 , ω and K * 0 are presented, as well as their comparison to predictions of hadronic interaction models currently used in air shower simulations.

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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.

257

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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Investigating cosmic rays and air shower physics with IceCube/IceTop

Cited by 4 publications

References 24 publications

Progress in high-energy cosmic ray physics

Progress in high-energy cosmic ray physics

Recent results from the cosmic ray program of the NA61/SHINE experiment

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

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