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      Demonstrating of Cosmic Ray Characteristics by Estimating the Cherenkov Light Lateral Distribution Function for Yakutsk Array as a Function of the Zenith Angle

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          Abstract

          Cherenkov light lateral distribution function (CLLDF) in Extensive Air Showers (EAS) for different primary particles (e-, n , p, F, K and Fe) was simulated using CORSIKA code for conditions and configurations of Yakutsk EAS array with the fixed primary energy 3 PeV around the knee region at different zenith angles. Basing on the results of CLLDF numerical simulation, sets of approximated functions are reconstructed for different primary particles as a function of the zenith angle. A comparison of the parameterized CLLDF with that simulated with Yakutsk EAS array is verified. The parameterized CLLDF also is compared with that measured on the Yakutsk EAS array.

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          QGSJET-II: towards reliable description of very high energy hadronic interactions

          S Ostapchenko (2004)
          Since a number of years the QGSJET model has been successfully used by different groups in the field of high energy cosmic rays. Current work is devoted to the first general update of the model. The key improvement is connected to an account for non-linear interaction effects which are of crucial importance for reliable model extrapolation into ultra-high energy domain. The proposed formalism allows to obtain a consistent description of hadron-hadron cross sections and hadron structure functions and to treat non-linear effects explicitely in individual hadronic and nuclear collisions. Other ameliorations concern the treatment of low mass diffraction, employment of realistic nuclear density profiles, and re-calibration of model parameters using a wider set of accelerator data.
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            Flipping photons backward: reversed Cherenkov radiation

            Min Min Chen, Hongsheng Chen (2011)
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              Extensive Air Shower Simulations at the Highest Energies

              M. Dova, D. Heck, S. Sciutto … (2002)
              Air shower simulation programs are essential tools for the analysis of data from cosmic ray experiments and for planning the layout of new detectors. They are used to estimate the energy and mass of the primary particle. Unfortunately the model uncertainties translate directly into systematic errors in the energy and mass determination. Aiming at energies \(> 10^{19}\) eV, the models have to be extrapolated far beyond the energies available at accelerators. On the other hand, hybrid measurement of ground particle densities and calorimetric shower energy, as will be provided by the Pierre Auger Observatory, will strongly constrain shower models. While the main uncertainty of contemporary models comes from our poor knowledge of the (soft) hadronic interactions at high energies, also electromagnetic interactions, low-energy hadronic interactions and the particle transport influence details of the shower development. We review here the physics processes and some of the computational techniques of air shower models presently used for highest energies, and discuss the properties and limitations of the models.
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                Author and article information

                Journal
                Publication date Created: 2016-12-15
                Article
                DOI: 10.18052/www.scipress.com/ILCPA.67.21
                ArXiV ID: 1612.08603
                SO-VID: 220e09e8-2b6f-4cbe-a32f-cf036dc12cda
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                http://arxiv.org/licenses/nonexclusive-distrib/1.0/

                History
                Custom metadata
                Journal reference International Letters of Chemistry, Physics and Astronomy, Vol. 67, PP. 21-30, 2016
                Comments 10 pages, 7 figures, published in International Letters of Chemistry, Physics and Astronomy Journal
                Categories astro-ph.HE astro-ph.IM

                ScienceOpen disciplines: Instrumentation & Methods for astrophysics,High energy astrophysical phenomena
                Data availability:
                ScienceOpen disciplines: Instrumentation & Methods for astrophysics, High energy astrophysical phenomena

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