A Numerical Model of the Structure and Evolution of Young Supernova Remnants

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Abstract
The evolution of the structure and radio emission of a young supernova remnant is discussed in terms of a fluid dynamic model of a supernova explosion. The interaction between the interstellar medium and the ejected material leads to a convective instability, which makes sufficient turbulent energy available to account for the observed synchrotron radio emission. From a study of different models of the ejected material it is found that the energy in the convection zone and the eventual radio source structure are insensitive to the initial conditions imposed on the explosion. The predicted radio emission rises to a maximum when the mass of interstellar material ‘swept up’ is of the same order as the ejected mass, and then decays due to adiabatic expansion of the convection zone.

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