  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
SNR-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 which 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 (1-5)E50 erg range.
