[en] The primary cosmic ray consist of protons (90%), helium nuclei (9%) and other heavy nuclei (1%) which are accelerated to enormous energies by supernova explosion and other cosmic phenomena with energy range 1 GeV to 108 TeV. Upon entering the atmosphere, the primary cosmic particles interact with nuclei of the air molecules roughly at 15 km above sea level. These interactions lead to the production of shower of hadrons mainly pions and kaons with small percentage of heavier hadrons. The shower of these particles move downwards with many of them decaying to muon and muon neutrinos. Obtained in this work are obtained muon distributions at sea level using CORSIKA (COsmic Ray SImulations for KAscade) and compared with experimental data