TAIGA天体物理复合物数据的一级宇宙射线和平均质量组成

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TAIGA天体物理复合物数据的一级宇宙射线和平均质量组成

Primary Cosmic Rays Energy Spectrum and Mean Mass Composition by the Data of the TAIGA Astrophysical Complex

论文作者

Prosin, V., Astapov, I., Bezyazeekov, P., Bonvech, E., Borodin, A., Bulan, A., Chiavassa, A., Chernov, D., Dyachok, A., Gafarov, A., Garmash, A., Grebenyuk, V., Gress, O., Gress, E., Gress, T., Grinyuk, A., Grishin, O., Ivanova, A. D., Ivanova, A. L., Kalmykov, N., Kindin, V., Kiryuhin, S., Kokoulin, R., Komponiets, K., Korosteleva, E., Kozhin, V., Kravchenko, E., Kryukov, A., Kuzmichev, L., Lagutin, A., Lavrova, M., Lemeshev, Y., Lubsandorzhiev, B., Lubsandorzhiev, N., Lukanov, A., Lukyantsev, D., Malakhov, S., Mirgazov, R., Monkhoev, R., Okuneva, E., Osipova, E., Pakhorukov, A., Pan, A., Panasenko, L., Pankov, L., Panov, A. D., Petrukhin, A., Poddubny, I., Podgrudkov, D., Poleschuk, V., Ponomareva, V., Popova, E., Postnikov, E., Ptuskin, V., Pushnin, A., Raikin, R., Razumov, A., Rubtsov, G., Ryabov, E., Sagan, Y., Samoliga, V., Silaev, A., Silaev Jr, A., Sidorenkov, A., Skurikhin, A., Sokolov, A., Sveshnikova, L., Tabolenko, V., Tanaev, A., Tarashchansky, B., Ternovoy, M. Y., Tkachev, L., Togoo, R., Ushakov, N., Vaidyanathan, A., Volchugov, P., Volkov, N., Voronin, D., Zagorodnikov, A., Zhaglova, A., Zhurov, D., Yashin, I.

论文摘要

EAS最大$ x_ {max} $的平均深度对能量的校正依赖性是从Tunka-133阵列的数据中获得了7年，而Taiga-Hiscore阵列已有2年。参数$ \ langle \ ln a \ rangle $，表征平均质量copositon的参数是从这些结果中得出的。 $ 2 \ cdot 10^{14} $ - $ 2 \ cdot 10^{16} $ \，使用新参数$ q_ {100} $ CHERERENKOV LIGHT FLUX在核心距离100 m。} $ cherenkov ligt

The corrected dependence of the mean depth of the EAS maximum $X_{max}$ on the energy was obtained from the data of the Tunka-133 array for 7 years and the TAIGA-HiSCORE array for 2 years. The parameter $\langle\ln A\rangle$, characterizing the mean mass compositon was derived from these results. The differential energy spectrum of primary cosmic rays in the energy range of $2\cdot 10^{14}$ - $2\cdot 10^{16}$\,eV was reconstructed using the new parameter $Q_{100}$ the Cherenkov light flux at the core distance 100 m.}

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