ar X iv : p hy si cs / 0 31 10 44 10 N ov 2 00 3 MODELING AND STUDY OF THE CERENKOV EFFECT

The studies realized in INRNE (Institute for Nuclear Research and Nuclear Energy) particulary in cosmic rays detection and construction of Muonic Cerenkov Telescope in University of Blagoevgrad [1] shows the need to develop a theoretical model based on observed phenomenon and to refine it for the detection system optimisation. The effect was introduced in EGS4 [2] code system. The first simulations were consecrated to different geometry's of water tank in total reflection. The model was compared with experimental data realised with gamma source 60 Co using the telescope. A simple atmospheric model is introduced in EGS4. The comparison between CORSIKA [3] and EGS4 codes was realised. A Muonic telescope (fig.1) is developed in INRNE and University of Blagoevgrad Bulgaria [1]. The destination is the registration of secondary muons and measuring the cosmic rays variations. The telescope is based on 18 water Cerenkov detectors split in 2 slabs of 3x3 cells. The dimensions of the tanks are 50x50x12cm. The penetrating muons creates Cerenkov photons unregistered by photomultipliers (fig.2). The telescope is under absorber so the electrons are rejected. The modelling of the processes and the development of theoretical model based on observed phenomenon is necessary to calibration and system optimisation. Most of the available codes permitting the simulation of Cerenkov effect are limited to one medium and geometry-Corsika code Fig.1 Muonic Cerenkov telescope Fig.2 Water Cerenkov detector