  Clumping in hot star winds can significantly affect estimates of mass-loss
rates, the inferred evolution of the star and the environmental impact of the
wind. A hydrodynamical simulation of a colliding winds binary (CWB) with clumpy
winds reveals that the clumps are rapidly destroyed after passing through the
confining shocks of the wind-wind collision region (WCR) for reasonable
parameters of the clumps if the flow in the WCR is adiabatic. Despite large
density and temperature fluctuations in the post-shock gas, the overall effect
of the interaction is to smooth the existing structure in the winds. Averaged
over the entire interaction region, the resulting X-ray emission is very
similar to that from the collision of smooth winds. The insensitivity of the
X-ray emission to clumping suggests it is an excellent diagnostic of the
stellar mass-loss rates in wide CWBs, and may prove to be a useful addition to
existing techniques for deriving mass-loss rates, many of which are extremely
sensitive to clumping. Clumpy winds also have implications for a variety of
phenomena at the WCR: particle acceleration may occur throughout the WCR due to
supersonic MHD turbulence, re-acceleration at multiple shocks, and
re-connection; a statistical description of the properties of the WCR may be
required for studies of non-equilibrium ionization and the rate of electron
heating; and the physical mixing of the two winds will be enhanced, as seems
necessary to trigger dust formation.
