  The properties of star cluster winds in the supercritical, catastrophic
cooling regime are discussed. We demonstrate that strong radiative cooling may
inhibit superwinds and, after a rapid phase of accumulation of the ejected
material within the star-forming volume, a new stationary isothermal regime,
supported by the ionizing radiation from the central cluster, is established.
The expected appearance of this core/halo supernebula in the visible line
regime and possible late evolutionary tracks for super-star cluster winds, in
the absence of ionizing radiation, are thoroughly discussed.
