Kuzyo T. Magneto-hydrodynamic simulations of strong shock waves in the interstellar medium

The evolution of supernova remnants in the interstellar magnetic field is studied using magneto-hydrodynamic simulations of a strong non-relativistic shock wave from a supernova explosion in the interstellar medium. The role of the magnetic field in the dynamics of supernova remnants has been explored for the first time from the early free expansion up to the well-developed radiative stage. The evolution of post-adiabatic supernova remnants has been studied with a proper treatment of the interstellar magnetic field. The strength and direction of the magnetic field was found to have a major impact on the evolution of radiative shocks and the post-shock gas dynamics. We have shown the effect of different diffusion models on the evolution of spectrum of cosmic rays accelerated on the shock front. Also, we have developed a model-independent method of magnetic field strength estimation in supernova remnants with bilateral morphology.