High-energy photoproduction in air showers

Krys, A.; Krys, E.; Wasilewski, A.

doi:10.1088/0954-3899/17/8/015

Cited by 7 publications

(2 citation statements)

References 3 publications

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“…They also reported a non-deficiency of muons in these data, seemingly inconsistent with a primary gamma ray hypothesis. In order to evaluate and discuss these data, many authors performed analytical or Monte Carlo calculations of the muon flux produced in gamma showers [10][11][12][13][14][15][16][17][18][19][20][21]. Most of these calculations were one-dimensional and all of them referred to gamma energies much larger than 10 TeV, appropriate to the Kiel experiment.…”

Section: Introductionmentioning

confidence: 99%

Spatial and energy distribution of muons inγ-induced air showers

Fassó

Poirier

2000

Phys. Rev. D

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The FLUKA Monte Carlo program is used to calculate the effects of hadroproduction by primary gamma rays incident upon the earth's atmosphere; for the results presented in this paper, only primary angles at 0 degrees from zenith are considered. The FLUKA code is believed to be quite accurate in reproducing experimental photon hadroproduction data in the 1 GeV to 10 TeV energy range studied. The charged pions which are so produced can decay to muons with sufficient energy to reach ground level. The number of these muons and their radial and energy distribution are studied for incident gamma ray energies from 1 GeV to 10 TeV. The number of these muons is not negligible; they can, in certain circumstances, be used to study potential sources of gamma rays like gamma ray bursts. It is found, for example, that a 10 TeV incident primary gamma ray produces, on average, 3.4 muons which reach ground level; the gamma ray energy which produces the maximum number of muons at ground level depends on the spectral index of the primary gamma spectrum, a constant which describes how the primary gamma flux rises with decreasing primary energy. An example: for a differential spectral index of 2.7, there is a broad maximum number of muons coming from ≈ 30 GeV primary gamma ray energy.PAC numbers: 95.75. Pq,98.70.Sa,98.70.Rz,13.60.Le

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Section: Introductionmentioning

confidence: 99%

Spatial and energy distribution of muons inγ-induced air showers

Fassó

Poirier

2000

Phys. Rev. D

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“…On general ground, there is a close relationship between the adopted model for photo-nuclear interactions and the muon distribution 𝐹 (𝐾 𝜇 ) with 𝐾 𝜇 = 𝑁 𝜇 /< 𝑁 𝜇 >. As an example, for models assuming a fast increase of the photo-nuclear cross-section, the number of muons expected in high-energy gamma and proton showers become comparable [59]. This imply that the detection of any gamma ray flux with the muon-poor technique would be impossible.…”

Section: Background Discrimination From the Groundmentioning

confidence: 99%

Detecting gamma-rays with moderate resolution and large field of view: Particle detector arrays and water Cherenkov technique

DuVernois¹,

Sciascio²

2022

Preprint

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The Earth is continuously bombarded by cosmic rays and gamma rays extending over an immense range of energies. Discovered in 1912 by Victor Hess, the cosmic radiation has been studied from balloons, from space, from the ground, and from underground. The resulting fields of cosmic ray astrophysics (focused on the charged particles), gamma-ray astrophysics, and neutrino astrophysics have diverged somewhat. But for the air showers in the GeV and TeV energy ranges, the ground-based detector techniques have considerable overlaps.Very high energy (VHE) gamma-ray astronomy is the observational study measuring the directions, flux, energy spectra, and time variability of the sources of these gamma rays. These measurements constrain the theoretical models of the sources and their interactions between the sources and detection at Earth. With the low flux of gamma rays, and the background of charged particle cosmic rays, the distinguishing characteristic of gamma-ray air shower detectors is large size and significant photon to charge particle discrimination.Air shower telescopes for gamma-ray astronomy consist of an array of detectors capable of measuring the passage of particles through the array elements. To maximize signal at energies of a TeV or so, the array needs to be built at high altitude as the maximum number of shower particles is high in the atmosphere. These detectors have included sparse arrays of shower counters, dense arrays of scintillators or resistive plate counters (RPC), buried muon detectors in concert with surface detectors, or many-interaction-deep Water Cherenkov Detectors (WCD).In general these detectors are sensitive over a large field of view, the whole of the sky is a typical sensitivity and perhaps 2/3 of the sky selected for clean analysis, but with only moderate resolution in energy, typically due to shower-to-shower fluctuations and the intrinsic sampling of the detector. These telescopes though, operate continuously, despite weather, moonlight, day or night, and without needing to be pointed to a specific target for essentially a 100% duty cycle. In this chapter we will examine the performance and characteristics of such detectors. These are contrasted with the Imaging Air Cherenkov Telescopes which also operate in this energy range, and both current and future proposed experiments are described.

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Detecting Gamma-Rays with Moderate Resolution and Large Field of View: Particle Detector Arrays and Water Cherenkov Technique

DuVernois

Sciascio

2023

Handbook of X-Ray and Gamma-Ray Astrophysics

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High-energy photoproduction in air showers

Cited by 7 publications

References 3 publications

Spatial and energy distribution of muons inγ-induced air showers

Spatial and energy distribution of muons inγ-induced air showers

Detecting gamma-rays with moderate resolution and large field of view: Particle detector arrays and water Cherenkov technique

Detecting Gamma-Rays with Moderate Resolution and Large Field of View: Particle Detector Arrays and Water Cherenkov Technique

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