Connecting accelerator experiments and cosmic ray showers

Pierog, T.

doi:10.1051/epjconf/20135301004

Cited by 6 publications

(19 citation statements)

References 23 publications

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“…Specific predictions are then performed using different air showers simulation codes, such as AIRES [13] or CORSIKA [14], which incorporate different models to describe the hadronic interactions, such as QGSJET [15], EPOS [16] or SIBYLL [17], which were developed with emphasis in air shower physics. These models predict the main features of the interactions and are regularly updated [18,19] in order that they better account for the measurements performed at high energy hadron colliders, such as the 3 A more accurate estimate of the pion decay energy can be performed [11] using that the density of the atmosphere is approximately exponential, with ρ(z) = ρ 0 exp(−z/h 0 ), with h 0 ≃ 10 km. One has then that ρ(z) = X cos θ/h 0 for a shower with zenith θ after traversing a slant depth X.…”

Section: The Physics Of Air Showersmentioning

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: The Physics Of Air Showersmentioning

confidence: 99%

Progress in high-energy cosmic ray physics

Mollerach

Roulet

2018

Progress in Particle and Nuclear Physics

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“…Second, the retuning of the cosmic-rays hadronic MCs using LHC data supports a mixed composition of proton and heavier ions (α particles and/or iron) at the tail of the cosmic ray spectrum up to E CR ∼10 20 eV, with reduced model uncertainties (from ∼50 g/cm 2 to ∼20 g/cm 2 for the values of the X max shower maximum in the atmosphere) [11]. Upcoming LHC data studies will also help to solve the current disagreement between the observed and predicted number of muons at ground for the highest-energy showers.…”

Section: Discussionmentioning

confidence: 67%

“…Around the GZK cutoff, the CR data prefer a mixed proton-iron composition (Fig. 2, right), with reduced model uncertainties (from ∼50 g/cm 2 to ∼20 g/cm 2 for values of X max where the proton-iron difference is about 100 g/cm 2 ) [11].…”

Section: Epj Web Of Conferencesmentioning

confidence: 93%

“…1, left), corresponding to the Greisen-Zatsepin-Kuzmin (GZK) cutoff of CRs propagating through intergalactic space and dissociating in collisions with the microwave background [3] and/or to the maximum energy reachable in astrophysical accelerators [4]. The experimental determination of the primary UHECR energy and mass relies upon the comparison of the properties of the produced extensive air-showers [11]. Right: Schematic "microscopic" view of an extensive air shower produced by an ultrarelativistic cosmic ray (proton or Fe-ion) colliding with a nucleus in the upper atmosphere.…”

Section: Impact Of Lhc Data On Ultra-high-energy Cosmic Raysmentioning

confidence: 99%

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Impact of LHC Run-1 on particle astrophysics

d’Enterria

2014

EPJ Web of Conferences

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“…Then, the models used for shower simulation extrapolate low energy data taken from accelerator experiments by several orders of magnitude in order to reach the energy of the cosmic rays. Note that, at present, the hadronic interaction models are being updated in order to reproduce the Large Hadron Collider data, which reaches up to cosmic ray energies of the order of ∼ 2 × 10 16 eV (E cm = 7 TeV) [26][27][28][29][30][31][32][33].…”

Section: Introductionmentioning

confidence: 99%

A composition dependent energy scale and the determination of the cosmic ray primary mass in the ankle region

Supanitsky

Etchegoyen

Melo

et al. 2015

Astroparticle Physics

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At present there are still several open questions about the origin of the ultra high energy cosmic rays. However, great progress in this area has been made in recent years due to the data collected by the present generation of ground based detectors like the Pierre Auger Observatory and Telescope Array. In particular, it is believed that the study of the composition of the cosmic rays as a function of energy can play a fundamental role for the understanding of the origin of the cosmic rays.The observatories belonging to this generation are composed of arrays of surface detectors and fluorescence telescopes. The duty cycle of the fluorescence telescopes is ∼ 10 % in contrast with the ∼ 100 % of the surface detectors. Therefore, the energy calibration of the events observed by the surface detectors is performed by using a calibration curve obtained from a set of high quality events observed in coincidence by both types of detectors. The advantage of this method is that the reconstructed energy of the events observed by the surface detectors becomes almost independent of simulations of the showers because just a small part of the reconstructed energy (the missing energy), obtained from the fluorescence telescopes, comes from simulations. However, the calibration curve obtained in this way depends on the composition of the cosmic rays, which can introduce biases in composition analyses when parameters with a strong dependence on primary energy are considered. In this work we develop an analytical method to study these effects. We consider AMIGA (Auger Muons and Infill for the Ground Array), the low energy extension of the Pierre Auger Observatory corresponding to the surface detectors, to illustrate the use of the method. In particular, we study the biases introduced by an energy calibration dependent on composition on the determination of the mean value of the number of muons, at a given distance to the showers axis, which is one of the parameters most sensitive to primary mass and has an almost linear dependence with primary energy.

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Connecting accelerator experiments and cosmic ray showers

Cited by 6 publications

References 23 publications

Progress in high-energy cosmic ray physics

Progress in high-energy cosmic ray physics

Impact of LHC Run-1 on particle astrophysics

A composition dependent energy scale and the determination of the cosmic ray primary mass in the ankle region

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