2D hydrodynamic simulations of super star cluster winds in a bimodal regime

It is shown that the winds of very massive and compact clusters evolve in a special bimodal way, such that in which the material deposited by stars into the inner cluster region becomes thermally unstable, forms cold dense clumps, and eventually feeds further episodes of star formation, while the material deposited into the outer region creates a quasi-stationary wind. We perform 2D numerical simulations of such winds using the finite difference hydrodynamic code ZEUS for which the cooling routine has been modified to make it suitable for modelling extremely fast cooling regions. We explore how the fraction of the deposited mass which is accumulated inside the cluster depends on the cluster parameters.