The Energy Spectrum and the Chemical Composition of Primary Cosmic Rays with Energies from 1014 to 1016 eV
The Energy Spectrum and the Chemical Composition of Primary Cosmic Rays with Energies from 1014 to 1016 eV
复制标题
能量1014~1016 eV的初级宇宙线的能谱和化学成分
DOI：
10.1086/422510
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发表时间：
2004
期刊：
影响因子：
--
通讯作者：
A. Velarde
中科院分区：
文献类型：
--
作者：
S. Ogio;F. Kakimoto;Y. Kurashina;O. Burgoa;D. Harada;H. Tokuno;H. Yoshii;A. Morizawa;E. Gotoh;H. Nakatani;K. Nishi;S. Shimoda;N. Tajima;Y. Yamada;T. Kaneko;K. Murakami;Y. Toyoda;Y. Matsubara;Y. Mizumoto;Y. Shirasaki;Y. Tsunesada;P. Miranda;A. Velarde
我们在玻利维亚的查卡尔塔亚山测量了一次能量超过6 TeV的大范围空气簇射。这些数据是从2000年3月开始由称为最小空气簇射（MAS）阵列的空气簇射阵列收集的。我们应用等强度分析方法，广泛的空气阵雨扩展到其最大发展的区域。我们在模拟中改变了质子和铁的混合物，并将其与数据进行比较，以确定质子的混合比作为初级能量的函数。利用这一点，我们导出了1014至5 × 1016 eV的初级能谱。因此，我们得出结论，幂律指数的光谱逐渐变化约1015.5 eV和所获得的质子比随能量的增加而降低。我们直接测量了由膝盖周围的能量初级产生的空气簇射的纵向发展。我们发现初级宇宙射线的平均质量数随着能量超过1014.5 eV而稳定增加，并且膝盖周围的主要成分不是质子。
We have measured extensive air showers with primary energies above 6 TeV at Mount Chacaltaya in Bolivia. The data were collected by an air shower array called the Minimum Air Shower (MAS) array starting in 2000 March. We applied an equi-intensity analysis method to the extensive air showers extended over the region of their maximum development. We varied the mixture of protons and iron in our simulations and compared these to the data to determine the mixing ratio of protons as a function of the primary energy. Using this, we derived the primary energy spectrum from 1014 to 5 × 1016 eV. Consequently, we conclude that the power-law index of the spectrum changes gradually around 1015.5 eV and that the obtained proton ratio decreases with increasing energy. We directly measured the longitudinal development of air showers generated by primaries with energies around the knee. We found that the average mass number of primary cosmic rays shows a steady increase with energy above 1014.5 eV and that the dominant component around the knee is not protons.