  Here we present a self-consistent stationary solution for spherically
symmetric winds driven by massive star clusters under the impact of radiative
cooling. We demonstrate that cooling may modify drastically the distribution of
temperature if the rate of injected energy approaches a critical value. We also
prove that the stationary wind solution does not exist whenever the energy
radiated away at the star cluster center exceeds ~ 30% of the energy deposition
rate. Finally we thoroughly discuss the expected appearance of super-star
cluster winds in the X-ray and visible line regimes. The three solutions here
found: the quasi-adiabatic, the strongly radiative wind and the inhibited
stationary solution, are then compared to the winds from Arches cluster, NGC
4303 central cluster and to the supernebula in NGC 5253.
