Abstract
The main purpose of the Sphere Antarctica project is connected to the fundamental problems of the cosmic ray physics and general astrophysics - the determination of the energy and mass composition of cosmic ray particles of ultra high and extremely high energies 10(18) - 10(20) eV. In the energy region above 6 . 10(19) eV modern experiments (Telescope Array and Pierre Auger Observatory) observed anisotropy and the clustering of arrival directions of cosmic rays in some areas.
The scientific importance of this problem stems from the lack of generally accepted acceleration mechanism of the CR particles above 3 . 10(18) eV, the unknown nature of the sources of such particles, the inconsistencies of the results of major experiments in the part of the mass of CR composition and the discrepancy of experimental and model data. Scientific novelty of this project is in the methodology registration of the extensive air showers over a large area similar to 600 km(2) from an altitude 30 km, that allows to measure the two optical components of the shower Vavilov-Cherenkov radiation and fluorescence light by the same SiPM sensitive elements of the detector simultaneously.