How to deal with PCR composition problem at $E_0 \gtrsim 10^{17}$ eV

TL;DR

This paper discusses a muon tracker technique utilizing MC simulations to address the primary cosmic ray composition problem in the energy range of 10^{17} to 10^{18} eV, with potential for extension to higher energies.

Contribution

It introduces a muon tracker approach based on MC simulations for determining cosmic ray composition at high energies, adaptable to various observation levels and models.

Findings

Method demonstrated using CORSIKA6.990 simulations.

Potential to extend to higher primary energies.

Applicable to different observation levels and interaction models.

Abstract

Basic ideas of muon tracker technique for the solution of primary cosmic ray (PCR) composition problem in the energy range $10^{17}-10^{18}$ eV are presented. The approach uses MC simulation data made with CORSIKA6.990 for "Pamir-XXI" site conditions. Similar technology can certainly be developed for other observation levels and interaction models. One can probably extend it to much higher primary energies.