Abstract
Computation of solar energetic particles propagation in the magnetosphere and atmosphere of the Earth is very important for ground level enhancement analysis. Detailed simulations of solar energetic particles events starting from asymptotic direction computation and NM detector response make it possible to build a strategy for inverse problem solution i.e. obtaining the characteristics of solar energetic particles on the basis on ground measurements. In this study a simulation of cosmic ray atmospheric cascade is carried out with PLANETOCOSMICS code. Energy spectra of secondary particles, namely neutrons and protons are obtained at various altitudes in the rigidity range of 0.7 GV to 1 TV of primary particles. Considering updated results for NM-64 detection efficiency the specific yield function for the standard neutron monitor is obtained for vertically and obliquely incident primary particles. The obtained results and applications are discussed.
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