Hydrodynamics of the matter reinserted within super stellar clusters

We present semianalytic and numerical models that take into account the effect of radiative cooling on the hydrodynamics of the matter reinserted by strong stellar winds and supernovae within the volume occupied by young, massive, and compact super stellar clusters. We first corroborate the location of the threshold line in the plane of mechanical energy input rate versus cluster size found by Silich et al. This line separates clusters that are able to drive a quasi-adiabatic or strongly radiative wind from those in which catastrophic cooling occurs within the cluster volume. Then we show that clusters above the threshold line exhibit a bimodal behavior in which the central, densest zones cool rapidly and accumulate the injected matter to eventually feed further generations of star formation, while the outer zones are still able to drive a stationary wind. The results are presented as a series of universal dimensionless diagrams, from which one can infer the sizes of the two zones, the fraction of the deposited mass that goes into each, and the mechanical luminosity of the resultant winds for clusters of all sizes and energy input rates, regardless the assumed adiabatic terminal speed (V-A,V-infinity).