  Winds from massive stars (> 8 solar masses) result in the formation of
wind-blown "bubbles" around these stars. In this paper we study, via
two-dimensional numerical hydrodynamic simulations, the onset and growth of
turbulence during the formation and evolution of these wind-blown "bubbles".
Our simulations reveal the formation of vortex rolls during the Main-Sequence
stage of the evolution, and Rayleigh-Taylor instabilities in the subsequent
stages due to accelerating and/or decelerating wind-blown shells. The bubble
shows a very turbulent interior just prior to the death of the star, with a
significant percentage of the internal energy expended in non-radial motions.
This would affect the subsequent evolution of the resultant supernova shock
wave. We discuss the implications of these results, show how the ratio of
kinetic energy in radial versus non-radial motions varies throughout the
evolution, and discuss how these results would carry over to three dimensions.
