Introduction of the Muonic and Cerenkov Effects in the EGS4 Code

Abstract

Some studies have been made in order to study the cosmic rays solar component variations. It’s a method particularly interesting to obtain information about the solar activity. Actually, we search more precisely to measure the flux of the secondary muons created by cosmic rays during their interactions in the atmosphere. In this aim, a muonic Cerenkov Telescope developed by the INRNE (Institute for Nuclear Research and for Nuclear Energy) and the SWU “Neofit Rilsky”- Blagoevgrad Bulgaria is used [1], The Experimental measures are made with a coincidence geometry. However, the electronic noise is very important. That ’s why, in this work, an absolute calibration and a signal modelling is realised to diminish the discrepancies of the results. In a first part, we redefine rapidly the Cerenkov effect and the model introduced inside the EGS4 Monte Carlo Code in order to simulate it. This approach permits the development of new technics for the registration of cosmic rays based on Cerenkov light in the atmosphere and the estimation of atmospheric transparency. In a second part we describe the telescope used and the comparison between the experimental and theoretical results obtained.