Cosmic Ray Showers

Greisen, K.

doi:10.1146/annurev.ns.10.120160.000431

Cited by 532 publications

(315 citation statements)

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“…The development of the corresponding electromagnetic cascade [16] is best described as a function of traversed air mass, usually referred to as the slant depth X. It is obtained by integrating the density of air along the direction of arrival of the air shower through the curved atmosphere,…”

Section: Introductionmentioning

confidence: 99%

Depth of maximum of air-shower profiles at the Pierre Auger Observatory. I. Measurements at energies above1017.8 eV

Aab¹,

Abreu²,

Aglietta³

et al. 2014

Phys. Rev. D

363

316

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We report a study of the distributions of the depth of maximum, Xmax, of extensive air-shower profiles with energies above 10 17.8 eV as observed with the fluorescence telescopes of the Pierre Auger Observatory. The analysis method for selecting a data sample with minimal sampling bias is described in detail as well as the experimental cross-checks and systematic uncertainties. Furthermore, we discuss the detector acceptance and the resolution of the Xmax measurement and provide parameterizations thereof as a function of energy. The energy dependence of the mean and standard 4 deviation of the Xmax-distributions are compared to air-shower simulations for different nuclear primaries and interpreted in terms of the mean and variance of the logarithmic mass distribution at the top of the atmosphere.

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Section: Introductionmentioning

confidence: 99%

Depth of maximum of air-shower profiles at the Pierre Auger Observatory. I. Measurements at energies above1017.8 eV

Aab¹,

Abreu²,

Aglietta³

et al. 2014

Phys. Rev. D

363

316

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“…IceTop tanks are not only sensitive to the number of charged particles, but also detect photons via electron-positron pair production. That is different from a scintillator array, which is relatively insensitive to the photonic part of the signal resulting in a lateral charge distribution which can be described by the NKG function [28,29]. Therefore, for IceTop an empirical lateral distribution function was derived from simulations [30,31].…”

Section: Time and Charge Distribution Of Air Shower Signalsmentioning

confidence: 99%

IceTop: The surface component of IceCube

Abbasi

Abdou

Ackermann³

et al. 2013

Nuclear Instruments and Methods in Physics Research Section A:

242

220

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IceTop, the surface component of the IceCube Neutrino Observatory at the South Pole, is an air shower array with an area of 1 km 2 . The detector allows a detailed exploration of the mass composition of primary cosmic rays in the energy range from about 100 TeV to 1 EeV by exploiting the correlation between the shower energy measured in IceTop and the energy deposited by muons in the deep ice. In this paper we report on the technical design, construction and installation, the trigger and data acquisition systems as well as the software framework for calibration, reconstruction and simulation. Finally the first experience from commissioning and operating the detector and the performance as an air shower detector will be discussed.

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“…from the shower axis, whereas the corresponding radius for muons is 360m. (Greisen, 1960). This suggests that the number of muons which will radiate coherently will be very small, and that it is probably reasonable to ignore the contribution to the radio emission from muons.…”

Section: 7mentioning

confidence: 99%

Radio Emission from Extensive Air Showers

1971

Nature

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Cosmic Ray Showers

Cited by 532 publications

References 0 publications

Depth of maximum of air-shower profiles at the Pierre Auger Observatory. I. Measurements at energies above1017.8 eV

Depth of maximum of air-shower profiles at the Pierre Auger Observatory. I. Measurements at energies above1017.8 eV

IceTop: The surface component of IceCube

Radio Emission from Extensive Air Showers

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