Particles of primary cosmic radiation generating extensive air showers of energy above 10{sup 20} eV in the atmosphere

Journal Article · Wed Dec 15 04:00:00 EST 2010 · Physics of Atomic Nuclei

DOI:https://doi.org/10.1134/S1063778810120185· OSTI ID:21426626

Glushkov, A V; Knurenko, S P; Makarov, I T; Pravdin, M I ^[1]; Podgrudkov, D A ^[2]; Sleptzov, I E ^[1]; Roganova, T M; Fedorova, G F ^[2]; Fedunin, E Yu ^[3]

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1. Russian Academy of Sciences, Institute of Cosmophysical Research and Aeronomy, Yakutsk Research Center, Siberian Division (Russian Federation)
2. Moscow State University, Skobeltsyn Institute of Nuclear Physics (Russian Federation)
3. Anturis (Russian Federation)

In order to construct the energy spectrum on the basis of data from the Yakutsk array, a method similar to that employed at the AGASA array is applied in addition to the standard approach based on experimental procedures. Moreover, a new, original, method underlying the calculation of the spectrum in the region of energies above 10{sup 20} eV is used to estimate energies. In order to compare data obtained at different arrays, it is proposed to harness the universal spectrum based on HiRes data. Within the QGSJET2 model, it is shown that a shower of energy 2 x 10{sup 20} eV was observed at the Yakutsk array. In the same energy region (above 2 x 10{sup 20} eV), the AGASA array recorded four showers, while the Fly's Eye array and Pierre Auger Observatory (PAO) recorded one shower each. These data do not confirm the conclusion that the flux of primary-cosmic-ray particles decreases because of the Greisen-Zatsepin-Kuzmin effect.

• OSTI ID: 21426626
• Journal Information: Physics of Atomic Nuclei, Journal Name: Physics of Atomic Nuclei Journal Issue: 12 Vol. 73; ISSN 1063-7788; ISSN PANUEO
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
COMPARATIVE EVALUATIONS
COSMIC RADIATION
COSMIC SHOWERS
ENERGY RANGE
ENERGY SPECTRA
EVALUATION
EXTENSIVE AIR SHOWERS
IONIZING RADIATIONS
MEASURING METHODS
PARTICLES
PEV RANGE
PRIMARY COSMIC RADIATION
RADIATIONS
SECONDARY COSMIC RADIATION
SHOWERS
SPECTRA