  Massive Stars (> 8 solar masses) lose mass in the form of strong winds. These
winds accumulate around the star, forming wind-blown bubbles. When the star
explodes as a supernova (SN), the resulting shock wave expands within this
wind-blown bubble, rather than the interstellar medium. The properties of the
resulting remnant, its dynamics and kinematics, the morphology, and the
resulting evolution, are shaped by the structure and properties of the
wind-blown bubble. In this article we focus on Kes 27, a supernova remnant
(SNR) that has been proposed by Chen et al (2008) to be evolving in a
wind-blown bubble, explore its properties, and investigate whether the
properties could be ascribed to evolution of a SNR in a wind-blown bubble. Our
initial model does not support this conclusion, due to the fact that the
reflected shock is expanding into much lower densities.
