Cosmic Ray Energy Spectrum and Mass Composition from 10^15 to 10^17 eV by Data of the Tunka EAS Cherenkov Array
Cosmic Ray Energy Spectrum and Mass Composition from 10^15 to 10^17 eV by Data of the Tunka EAS Cherenkov Array
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发表时间：
2005-11
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通讯作者：
N. Budnev;D. Chernov;O. Gress;T. Gress;E. Korosteleva;L. Kuzmichev;B. Lubsandorzhiev;L. Pankov;Y. Parfenov;V. Prosin;Y. Semeney;C. Spiering;R. Wischnewski;I. Yashin;S. Msu;Moscow;Russia Api Isu;Irkutsk;Russia Ras;R. Desy;Zeuthen;H Germany
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作者：
N. Budnev;D. Chernov;O. Gress;T. Gress;E. Korosteleva;L. Kuzmichev;B. Lubsandorzhiev;L. Pankov;Y. Parfenov;V. Prosin;Y. Semeney;C. Spiering;R. Wischnewski;I. Yashin;S. Msu;Moscow;Russia Api Isu;Irkutsk;Russia Ras;R. Desy;Zeuthen;H Germany
本文介绍了对EAS切伦科夫阵列Tunka-25实验数据的改进分析结果。在CORSIKA模拟的基础上，建立了一个新的函数来拟合0 ~ 350 m的切伦科夫光横向分布LDF，并将其应用于Tunka数据的分析。用两种方法估计了EAS的最大位置。一种基于脉冲FWHM，另一种基于光LDF。我们给出了10^15 - 10^17 eV能量范围内的一次能谱。讨论了利用EAS最大值的深度来确定平均质量组成的方法。
We present results of an improved analysis of the experimental data of the EAS Cherenkov array Tunka-25. A new function to fit the Cherenkov light lateral distribution LDF at core distances from 0 to 350 m has been developed on the base of CORSIKA simulations and applied to the analysis of Tunka data. Two methods to estimate the EAS maximum position have been used. The one is based on the pulse FWHM, the other on the light LDF. We present the primary energy spectrum in the energy range 10^15 - 10^17 eV. The use of the depth of the EAS maximum to determine the mean mass composition is discussed.