Shuhei Yoshida

Measurement of the cosmic-ray energy spectrum and composition from 1017 to 1018.3 eV using a hybrid technique

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 Flys 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 Flys Eye measurements and supports the previously found steepening near 4 times 10^{17} eV .

Evidence for Changing of Cosmic Ray Composition between 10**17-eV and 10**18-eV from Multicomponent Measurements

The average mass composition of cosmic rays with primary energies between

The cosmic ray energy spectrum above 3 × 1018 eV measured by the Akeno Giant Air Shower Array

10^{17}

Measurement of the Cosmic Ray Energy Spectrum and Composition from 10^{17} to 10^{18.3} eV Using a Hybrid Fluorescence Technique

eV and

A measurement of the average longitudinal development profile of cosmic ray air showers between 1017 and 1018 eV

10^{18}

Atmospheric studies using the high-resolution fly's eye xenon flasher array

eV has been studied using a hybrid detector consisting of the High Resolution Flys Eye (HiRes) prototype and the MIA muon array. Measurements have been made of the change in the depth of shower maximum,

Atmospheric Monitoring for Fluorescence Detector Experiments

X_{max}

Anisotropy of cosmic-ray arrival direction at 1018eV observed by AGASA

, and in the change in the muon density at a fixed core location,

QSO 0133+476

rho_mu(600m)

Comet P/2000 EC_98 = (60558)

, as a function of energy. The composition has also been evaluated in terms of the combination of