Dusty supernovae running the thermodynamics of the matter reinserted
  within young and massive super stellar clusters
  Following the observational and theoretical evidence that points at core
collapse supernovae as major producers of dust, here we calculate the
hydrodynamics of the matter reinserted within young and massive super stellar
clusters under the assumption of gas and dust radiative cooling. The large
supernova rate expected in massive clusters allows for a continuous
replenishment of dust immersed in the high temperature thermalized reinserted
matter and warrants a stationary presence of dust within the cluster volume
during the type II supernova era. We first show that such a balance determines
the range of dust to gas mass ratio and this the dust cooling law. We then
search for the critical line that separates stationary cluster winds from the
bimodal cases in the cluster mechanical luminosity (or cluster mass) vs cluster
size parameter space. In the latter, strong radiative cooling reduces
considerably the cluster wind mechanical energy output and affects particularly
the cluster central regions, leading to frequent thermal instabilities that
diminish the pressure and inhibit the exit of the reinserted matter. Instead
matter accumulates there and is expected to eventually lead to gravitational
instabilities and to further stellar formation with the matter reinserted by
former massive stars. The main outcome of the calculations is that the critical
line is almost two orders of magnitude or more, depending on the assumed value
of the adiabatic wind terminal speed, lower than when only gas radiative
cooling is applied. And thus, many massive clusters are predicted to enter the
bimodal regime.
