Abstract
The method of the determination of Primary Cosmic Ray mass composition is presented. Data processing is based on the theoretical model representing the EAS spectrum vs the total number of muons as the superposition of the spectra corresponding to different kinds of primary nuclei. The method consists of two stages. At the first stage, the permissible intervals of primary nuclei fractions fi are determined on the base of the EAS spectrum vs the total number of muons (Eμ ≥ 235 GeV). At the second stage, the permissible intervals of fi are narrowed by fitting procedure. Within the framework of three components (protons, helium and heavy nuclei), the mass composition in the region 1015 – 1016 eV has been defined: fp = 0.235 ± 0.02, fHe = 0.290 ± 0.02, fH = 0.475 ± 0.03.
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