2003ApJ...584..284V

Numerical simulations of the interaction between supernova ejecta and a stellar wind are presented. We follow the temporal evolution of the shock fronts that are formed through such an interaction and determine the velocities, temperatures, and densities. We model the X-ray emission from the supernova remnant-stellar wind collision region, and we compare it with recent results from X-ray observations carried out with the Chandra satellite of the SMC supernova remnant SNR 0057-7226, which could be interacting with the wind of the Wolf-Rayet system HD 5980. The simulations predict the presence of shell-like regions of enhanced X-ray emission that are consistent with the presence of X-ray-emitting arcs in the Chandra image. Also, the observed X-ray luminosity is comparable to the X-ray luminosities we obtain from the simulations for a supernova with an initial energy in the 1-5x10⁵⁰ ergs range.