The evolution of compact supernova remnants in a strongly magnetized medium

Two-dimensional simulations of the evolution of supernova remnants in a uniform, high-density medium are presented. The medium is magnetized, and its magnetic pressure is much larger than the thermal pressure. The evolution of the remnants is followed past full thermalization of the ejecta. A mechanism of self-collimation of the flow is identified, resulting in formation of jets that propagate along the magnetic field lines.