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Hadronic interactions and primary-cosmic-ray composition at energies around 10 15 – 10 16 eV …

1988; American Physical Society; Volume: 38; Issue: 5 Linguagem: Inglês

10.1103/physrevd.38.1404

1538-4500

J. R. Ren, A. X. Huo, S. L. Lu, S. Su, C. R. Wang, N. J. Chang, P. Y. Cao, J. Y. Li, B. T. Zou, S. Z. Wang, G. Z. Bai, Zuowen Liu, G. J. Li, Q. X. Geng, R. D. He, W. D. Zhou, M. Amenomori, H. Nanjo, N. Hotta, I. Ohta, K. Mizutani, K. Kasahara, T. Yuda, T. Shirai, N. Tateyama, S. Torii, M. Shibata, H. Sugimoto, K. Taira,

Particle physics theoretical and experimental studies

Gross features of gamma families observed at Mt. Kanbala (5500 m above sea level) and Mt. Fuji (3750 m) are summarized in comparison with a Monte Carlo simulation based on a plausible assumption about hadronic interactions and primary composition. Our analysis shows that the assumption of approximate Feynman scaling in the fragmentation region and a heavy-enriched primary composition in the energy range over 1015 eV is wholly compatible with the experimental data. That is, there is no evidence of strong violation of Feynman scaling in the fragmentation region at least up to 1016 eV. As to the primary cosmic rays, our data infer a steepening of proton spectrum at energies around 1014 eV. The proton component in the primary cosmic rays is estimated to occupy 15–20 % of the total flux at 1015 eV. Some other interesting implications on hadronic interactions are discussed with reference to the structures of gamma families.Received 18 November 1987DOI:https://doi.org/10.1103/PhysRevD.38.1404©1988 American Physical Society