2016 International Conference on Ultra-High Energy Cosmic Rays

Session

Oct.11PM1

Oct.11PM1

11 Oct 2016, 14:20

Kyoto Research Park

Conveners

Oct.11PM1

• Radomir Smida (Karlsruhe Institute of Technology)

31. Cosmic Rays Energy Spectrum observed by the TALE detector

Tareq AbuZayyad (University of Utah)

11/10/2016, 14:20

We report on a cosmic ray energy spectrum measurement by the Telescope Array Low-Energy extension (TALE) fluorescence detector (FD). The TALE FD is an air fluorescence detector which is also sensitive to the Cerenkov light produced by shower particles. Low energy cosmic rays, in the PeV energy range, are detectable by TALE as "Cerenkov Events". Using these events, we measure the energy...

57. Cosmic ray physics with the KASCADE-Grande observatory

Juan Carlos Arteaga-Velazquez (Universidad Michoacana)

11/10/2016, 14:40

The existence of a knee at a few PeV in the all-particle cosmic ray energy spectrum has been well established by several experiments but its physical origin has eluded researches for a long time. It is believed that keys to disentangle the mystery could be found in the spectrum and the composition of cosmic rays between 1 PeV and 1 EeV. A first detailed look into the elemental chemical...

43. Results of CR energy spectrum and mass composition study with EAS Arrays in the Tunka Valley

Prof. Vasily Prosin (Skobeltsyn Inst. of Nucl.Phys. of Lomonosov Moscow Statte Univ.)

11/10/2016, 15:00

There are three extensive air showers (EAS) arrays aimed to the study of Cosmic Rays (CR) in the different energy ranges in the Tunka Valley. The first of them is Atmospheric Cherenkov Light Array Tunka-133, containing 175 single PMT detectors at the area of about 3 km2. It ‘s operating since 2009 and has the energy range 5•1015 – 1018 eV. The second one is a low threshold observatory...

9. Estimation of the invisible energy with the data collected by the Pierre Auger Observatory

Dr Analisa Gabriela Mariazzi (Instituto de Fisica La Plata - CONICET)

11/10/2016, 15:20

The determination of the primary energy of extensive air showers using the fluorescence technique requires an estimation of the energy carried away by particles that do not deposit all their energy in the atmosphere.
This estimation is typically made using Monte Carlo simulations and thus depends on the assumed primary particle mass and on model predictions for neutrino and muon production....