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The method of a determination of the Primary Cosmic Ray mass composition ispresented. Data processing is based on the theoretical model representing theintegral muon multiplicity spectrum as the superposition of the spectracorresponding to different kinds of primary nuclei. The method consists of twostages. At the first stage, the permissible intervals of primary nucleifractions f_i are determined on the base of the EAS spectrum vs the totalnumber of muons (E_mu > 235 GeV). At the second stage, the permissibleintervals of f_i are narrowed by fitting procedure. We use the experimentaldata on high multiplicity muon events (n_mu > 114) collected at the Baksanunderground scintillation telescope. Within the framework of three components(protons, helium and heavy nuclei), the mass composition in the region10^15-10^16 eV has been defined: f_p = 0.235 +- 0.02, f_He = 0.290 +- 0.02$,f_H = 0.475 +- 0.03.

On the mass composition of primary cosmic rays in the energy region 10^15-10^16 eV