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Measurement of the Cosmic‐Ray Energy Spectrum and Composition from 10 17 to 10 18.3 eV Using a Hybrid Technique

2001; IOP Publishing; Volume: 557; Issue: 2 Linguagem: Inglês

10.1086/322240

1538-4357

T. Abu‐Zayyad, K. Belov, D. J. Bird, J. Boyer, Zhen Cao, M. Catanese, Guoqi Chen, R. W. Clay, C. E. Covault, H. Y. Dai, B. R. Dawson, J. W. Elbert, B. Fick, L. Fortson, Jim Fowler, K. Gibbs, M. A. K. Glasmacher, K. D. Green, Y. Ho, Audrey Huang, C. C. H. Jui, M. Kidd, D. Kieda, B. Knapp, Seung Hwan Ko, C. G. Larsen, W. Lee, E. C. Loh, E. J. Mannel, J. Matthews, J. N. Matthews, B. J. Newport, D. Nitz, R. A. Ong, K. M. Simpson, J. D. Smith, D. Sinclair, P. Sokolsky, P. Sommers, C. Song, J. K. K. Tang, S. B. Thomas, J. C. van der Velde, L. R. Wiencke, C. R. Wilkinson, S. Yoshida, X. Z. Zhang,

Particle physics theoretical and experimental studies

We study the spectrum and average mass composition of cosmic rays with primary energies between 10^{17} eV and 10^{18} eV using a hybrid detector consisting of the High Resolution Fly's Eye (HiRes) prototype and the MIA muon array. Measurements have been made of the change in the depth of shower maximum as a function of energy. A complete Monte Carlo simulation of the detector response and comparisons with shower simulations leads to the conclusion that the cosmic ray intensity is changing f rom a heavier to a lighter composition in this energy range. The spectrum is consistent with earlier Fly's Eye measurements and supports the previously found steepening near 4 \times 10^{17} eV .