An evaluation of the Richtmyer-Meshkov instability in supernova remnant formation

We present an initial evaluation of the role of the Richtmyer-Meshkov (RM) instability in supernova remnant (SNR) formation. Although the Rayleigh-Tay lor (RT) instability is most often considered in the canonical picture of S NR formation, the theoretical penetration depths for RM instability suggest that it could play a significant role in the early stages of SNR formation . We have used the code PROMETHEUS to perform a sequence of two-dimensional hydrodynamic simulations in order to test this possibility. Here we discus s a case in which we impose a large perturbation in the expanding ejecta be hind the reverse shock. The interaction of the reverse shock with the pertu rbation produces significant early RM growth, with spikes penetrating from the contact surface to near the forward shock. Then the RM instability weak ens, RT growth eventually dominates, and the perturbation of the forward sh ock diminishes. We conclude that RM instability growth due to the type of p erturbation we have studied might contribute to, but alone cannot account f or, the observed radio and X-ray structures that extend to the forward shoc k in such SNRs as supernova 1006.