Formation of supernova remnants - The pre-blast-wave phase

Abstract

The effect of stellar structure on supernova remnant formation is studied with a series of computer models of a 10 to the 51st erg explosion in a 15 solar mass star. Immediately after the explosion shock wave travels down a steep density gradient, the material in the gradient goes into free expansion, forming a collapsible piston. At the outer edge of such a piston are two shock waves: the expanding supernova shock and a reverse shock moving back into the collapsible piston. Until the piston is completely collapsed it is Rayleigh-Taylor stable, but after collapse the inner material behaves as a massive piston and the interface is Rayleigh-Taylor unstable. If there is a significant mass in an external density gradient, the material between the supernova shock moving out through the interstellar medium and the reverse shock will be a significant source of X-rays during the pre-blast-wave phase of remnant formation.