Superyoung EAS withN e&gt;107. The «Hadron» experiment

Adamov, D. S.; Arabkin, V. V.; Besshapov, S. P.; Cherdyntseva, K. V.; Chubenko, A. P.; Duboviy, A. G.; Djatlov, P. A.; Janseitova, J. K.; Zhukov, V.; Nam, R.A.; Nesterova, N. M.; Nikolskaya, N. M.; Pavlyuchenko, V. P.; Piscal, V. V.; Shaulov, S. B.; Stepanov, A. V.; Vildanov, N. G.; Vildanova, L. I.

doi:10.1007/bf02508142

Cited by 2 publications

(2 citation statements)

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“…The complex Tien Shan array (43.04 N, 76.93 E, P = 685 g·cm −2 ) comprises different EAS detectors: hadrons (the ionization calorimeter), electrons (scintillation and GM counters), muons (underground GM counters) and detectors of atmospheric Cherenkov light [5]. EAS were classified according to the total number of electrons N e (N e ∼ E 0 ) at the Tien Shan level.…”

Section: Experimental Results and Comparisons With Different Modelsmentioning

confidence: 99%

“…It was done using the Tien Shan complex array experimental data at PCR energies, E 0 = 0.5 − 10 PeV, and their extrapolation from 0.2 TeV (accelerator experiments with fixed targets). Our initial publications are to be found in references [1][2][3][4][5]. Experimental data of various components (mainly hadrons, electrons and Cherenkov light in the atmosphere) of extensive air showers (EAS) initiated by PCRs were compared with many different former and modern models.…”

Section: Introductionmentioning

confidence: 99%

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Inelastic proton-air cross section growth from 0.2 TeV to 10 PeV according to TIEN SHAN experimental cosmic ray data

Nesterova

2017

EPJ Web Conf.

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Abstract.Conclusions are made about the increase with energy of the inelastic proton air cross section σ p−air from 0.2 TeV (accelerator experiments with fixed targets) to 10 PeV (cosmic rays). Experimental data from the Tien Shan complex array on various components (mainly hadron, Cherenkov light, and electron) of extensive air showers at 0.5-10 PeV of primary cosmic rays are analyzed. They were compared with many results of different calculated models of cosmic ray interactions in the atmosphere. The analysis showed that the rise conforms to (7-9)% per one order of energy. These data correspond better to the QGSJET-II-04 version of the interaction model based on the recent LHC results. This model predicts better the slower rise of the crosssection than previous versions of QGSJET-II and some other models.

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Section: Experimental Results and Comparisons With Different Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%