Yu. F. Novoseltsev, R. V. Novoseltseva, G. M. Vereshkov
The method of a determination of the Primary Cosmic Ray mass composition is
presented. Data processing is based on the theoretical model representing the
integral muon multiplicity spectrum 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 f_i are determined on the base of the EAS spectrum vs the total
number of muons (E_mu > 235 GeV). At the second stage, the permissible
intervals of f_i are narrowed by fitting procedure. We use the experimental
data on high multiplicity muon events (n_mu > 114) collected at the Baksan
underground scintillation telescope. Within the framework of three components
(protons, helium and heavy nuclei), the mass composition in the region
10^15-10^16 eV has been defined: f_p = 0.235 +- 0.02, f_He = 0.290 +- 0.02$,
f_H = 0.475 +- 0.03.
View original:
http://arxiv.org/abs/1108.4245
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