  Results of a study of the theoretically predicted and observed X-ray
properties of local massive star clusters are presented, with a focus on
understanding the mass and energy flow from these clusters into the ISM via a
cluster wind. A simple theoretical model, based on the work of Chevalier &
Clegg (1985), is used to predict the theoretical cluster properties, and these
are compared to those obtained from recent Chandra observations. The model
includes the effect of lower energy transfer efficiency and mass-loading. In
spite of limited statistics, some general trends are indicated; the observed
temperature of the diffuse X-ray emission is lower than that predicted from the
stellar mass and energy input rates, but the predicted scaling of X-ray
luminosity with cluster parameters is seen. The implications of these results
are discussed.
