Gamma rays and cosmic rays in supernova remnants with radiative cooling

The evolution of supernova remnants (SRN's) is followed numerically taking into account the non-linear effects of particle acceleration in shock waves. These high energy particles produce neutral pions by collisions with the thermal plasma and these π 0 's decay into the observable γ-rays. The cosmic rays are treated as a fluid and the time variation of the adiabatic index during the remnant evolution of the cosmic rays as well as of the mean diffusion coefficient are estimated dynamically by a simplified theory. Several SNR models with different efficiencies for the conversion of the supernova explosion energy into cosmic rays depending on physical parameter are analyzed.