Feedback from Winds and Supernovae in Massive Stellar Clusters
  We simulate the effects of massive star feedback, via winds and SNe, on
inhomogeneous molecular material left over from the formation of a massive
stellar cluster. We use 3D hydrodynamic models with a temperature dependent
average particle mass to model the separate molecular, atomic, and ionized
phases. We find that the winds blow out of the molecular clump along
low-density channels, and gradually ablate denser material into these. However,
the dense molecular gas is surprisingly long-lived and is not immediately
affected by the first star in the cluster exploding.
