  The structure and evolution of wind-blown bubbles (WBBs) around massive stars
has primarily been investigated using an energy-conserving model of wind-blown
bubbles. While this model is useful in explaining the general properties of the
evolution, several problems remain, including inconsistencies between observed
wind luminosities and those derived using this formulation. Major difficulties
include the low X-ray temperature and X-ray luminosity, compared to the model.
In this paper, we re-examine the evolution, dynamics, and kinematics of WBBs
around massive stars, using published ionization gasdynamic simulations of
wind-blown bubbles. We show that WBBs can cool efficiently due to the presence
of various instabilities and turbulence within the bubble. The expansion of
WBBs is more consistent with a momentum-conserving solution, rather than an
energy-conserving solution. This compares well with the dynamics and kinematics
of observed wind bubbles. Despite the cooling of the bubble, the shocked wind
temperature is not reduced to the observed values. We argue that the X-ray
emission arise mainly from clumps and filaments within the hot shocked wind
region, with temperatures just above 10$^6$ K. The remainder of the plasma can
contribute to a lesser extent.
