PRIMARY ENERGY SPECTRUM AND MASS COMPOSITION DETERMINED WITH THE TUNKA EAS CHERENKOV ARRAY

Callibration of a homemade 4-fold Water Cherenkov Detector array, by detection of EAS events

How to Infer the Primary Energy Spectrum from Eas Observations Demonstrated with Kascade Data

The energy spectrum of primary cosmic rays in the energy range of 1014 1016 eV is infered from the information about the electron/photon and muon components from the KASCADE array. We combine the EAS simulation program CORSIKA and a detector simulation program, based on the GEANT package, with a multivariate statistical analysis program for an event-by-event analysis of real data. Approaches of...

An investigation of using hump in the Cherenkov photon lateral distribution for Gamma-Hadron separation

Simulation of gamma and hadron showers in the energy range 100GeV- 25TeV has been carried out. For a big ideal Cherenkov light array, characteristics of lateral distribution of Cherenkov photon density have been studied. Results from this ideal detector are compared with those simulated for a real TUNKA- like array to investigate experimental potential of using existence of a hump in lateral di...

callibration of a homemade 4-fold water cherenkov detector array, by detection of eas events

Measuring extensive air showers with Cherenkov light detectors of the Yakutsk array: The energy spectrum of cosmic rays

The energy spectrum of cosmic rays in the range E ∼ 1015 eV to 6 × 1019 eV has been studied using the air Cherenkov light detectors of the Yakutsk array. The total flux of photons produced by relativistic electrons (including positrons as well, hereafter) of extensive air showers in the atmosphere is used as the energy estimator of the primary particle initiating a shower. The resultant differe...