Cosmic rays are high energy particles reaching our planet, whose spectrum  ranges from sub GeV up to 10^10 GeV energies. The bulk of the observed cosmic rays, probably up to PeV energies, is likely of galactic origin and is thought to be accelerated at supernova remnant shocks and to propagate diffusively through the Galaxy. The acceleration mechanism, the escape of accelerated particles from the sources and their subsequent propagation toward us and out of the Galaxy, are all pieces of the same complex puzzle, namely the origin of cosmic rays. A fascinating and yet not understood aspect of cosmic rays is the relative spectral shape of protons, electrons, antiprotons and positrons, which  the "standard picture" of the galactic origin of cosmic rays is unable to explain. 

The goal of this stage is  the study of theoretical models of galactic cosmic ray propagation. The student will learn  how to deal with the diffusion-convection equation and its applications to the cosmic ray physics, in particular to the estimation of the expected proton, antiproton, electron and positron fluxes, in different propagation scenarios.