Muons in EAS generated by cosmic gamma-rays with ultra-high energy

Châtelet, Éric; Procureur, J.; Stamenov, J. N.; Ushev, S. Z.

doi:10.1088/0954-3899/16/2/019

Cited by 15 publications

(7 citation statements)

References 20 publications

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“…Simulations based on the MOCCA [11] and CORSIKA [12] programs indicate that γ-ray showers contain, on average, 3-4% of the number of muons as showers initiated by protons of the same energy. These results, which agree with other calculations [13], are based on conventional electromagnetic and photoproduction couplings. The possibility of an anomalously high photoproduction cross section has been experimentally ruled out at HERA up equivalent laboratory energy of ∼ 2 × 10 13 eV [10].…”

supporting

confidence: 92%

Limits on the Isotropic Diffuse Flux of Ultrahigh EnergyγRadiation

et al. 1997

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Diffuse ultrahigh energy γ-radiation can arise from a variety of astrophysical sources, including the interaction of 10 20 eV cosmic rays with the 3 K microwave background radiation or the collapse of topological defects created in the early Universe. We describe a sensitive search for diffuse γrays at ultrahigh energies using the CASA-MIA experiment. An isotropic flux of radiation is not detected, and we place stringent upper limits on the fraction of the γ-ray component relative to cosmic rays (< 10 −4 ) at energies from 5.7 × 10 14 eV to 5.5 × 10 16 eV. This result represents the first comprehensive constraint on the γ-ray flux at these energies.

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confidence: 92%

Limits on the Isotropic Diffuse Flux of Ultrahigh EnergyγRadiation

et al. 1997

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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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“…These results on the muon content are based on the conventional values of the electromagnetic and the photo-production cross sections [71,103]. In the past there have been some reports indicating anomalously high muon content in the γ-ray signals reported from the binary X-ray sources such as the Cygnus X-3 and Hercules X-1 etc.…”

Section: High Energy Astroparticle Physics At Ooty and The Grapes-3 Ementioning

confidence: 99%

High Energy Astroparticle Physics at Ooty and the GRAPES-3 Experiment

Gupta¹

2014

Proceedings of the Indian National Science Academy

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The astroparticle studies at Ooty have their roots going way back into the fifties, when studies using cosmic rays were initiated with cloud chambers of progressively larger sizes as the primary detector and measuring device to obtain properties of hadrons at high energies. This study was subsequently strengthened with the installation of a total absorption calorimeter and a modest extensive air shower array to probe the composition of the primary cosmic rays to very high energies. The discovery of pulsars provided a thrust for the exploration of these compact objects as the sources of γ-rays at TeV energies with the aid of atmospheric Cerenkov detectors in the seventies. With the rapid technological advances occurring during the subsequent years in detectors, electronics and computers, physicists world-wide were able to set up very large and remarkably sensitive experiments that were hard to imagine a decade earlier. With the increasing sophistication and complexity the modern experiments require participation of very large teams of scientists. This development has made the formation of collaboration of large number of physicists both experimental and theoretical, engineers, technicians etc., from a number of institutions and universities, a prerequisite for setting up any major experimental facility. The GRAPES-3 experiment is a collaboration of 34 scientists from 13 institutions, including 8 from India and 5 from Japan. The GRAPES-3 experiment contains a dense extensive air shower array operating with ~ 400 scintillator detectors and a 560 m 2 tracking muon detector (Em > 1 GeV), at Ooty in India. 25 % of scintillator detectors are instrumented with two fast photomultiplier tubes (PMTs) for extending the dynamic range to ~ 5x10 3 particles m -2. The scintillators, signal processing electronics and data recording systems were fabricated in-house to cut costs and optimize performance. The muon multiplicity distribution of the EAS is used to probe the composition of primary cosmic rays below the 'knee', with an overlap with direct measurements. Search for multi-TeV γ-rays from point sources is done with the aid of the muon detector. A good angular resolution of 0.7 o at 30 TeV, is measured from shadow of the Moon on the isotropic flux of cosmic rays. Sensitive limit on the diffuse flux of 100 TeV γ-rays is placed by using muon detector to filter out the charged cosmic ray background. The tracking muon detector allows sensitive measurements on the coronal mass ejections and solar flares through Forbush decrease events. We have major expansion plans to enhance the sensitivity of the GRAPES-3 experiment in the areas listed above. PACS

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Muons in EAS generated by cosmic gamma-rays with ultra-high energy

Abstract: EAS initiated by primary gamma -quanta, with constant size at mountain altitude, are simulated using three-dimensional procedures based on the SM1 phenomenological interaction model. The criterion Nmu /(Nmu ) Show more

Cited by 15 publications

References 20 publications

Limits on the Isotropic Diffuse Flux of Ultrahigh EnergyγRadiation

Limits on the Isotropic Diffuse Flux of Ultrahigh EnergyγRadiation

Spatial and energy distribution of muons inγ-induced air showers

High Energy Astroparticle Physics at Ooty and the GRAPES-3 Experiment

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