关于10^15-10^16能区初级宇宙射线的质量组成eV
On the mass composition of primary cosmic rays in the energy region 10^15-10^16 eV
摘要：
本文介绍了一种测定初级宇宙线质量成分的方法。数据处理的理论模型是将积分μ子多重数谱表示为对应于不同原始核的μ子多重数谱的叠加。该方法包括两个阶段。在第一阶段，根据EAS谱与μ子总数（E_mu > 235 GeV）的关系，确定了初始核分数的允许区间f_i。在第二阶段，用拟合方法缩小f_i的容许区间。我们使用的实验数据的高多重μ介子事件（n_mu > 114）在Baksan地下闪烁望远镜收集。在三组分（质子、氦和重核）的框架下，定义了10^15-10^16 eV区域的质量组成：f_p = 0.235 +-0.02，f_He = 0.290 +-0.02$，f_H = 0.475 +-0.03。
英文摘要：
The method of a determination of the Primary Cosmic Ray mass composition is presented. Data processing is based on the theoretical model representing the integral muon multiplicity spectrum as the superposition of the spectra corresponding to different kinds of primary nuclei. The method consists of two stages. At the first stage, the permissible intervals of primary nuclei fractions f_i are determined on the base of the EAS spectrum vs the total number of muons (E_mu > 235 GeV). At the second stage, the permissible intervals of f_i are narrowed by fitting procedure. We use the experimental data on high multiplicity muon events (n_mu > 114) collected at the Baksan underground scintillation telescope. Within the framework of three components (protons, helium and heavy nuclei), the mass composition in the region 10^15-10^16 eV has been defined: f_p = 0.235 +- 0.02, f_He = 0.290 +- 0.02$, f_H = 0.475 +- 0.03.
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