The evolution of intracluster medium in stellar clusters
  Stars in globular clusters lose mass through slow stellar winds that are
retained by the stellar cluster and contribute to build up a non negligible
intracluster medium over time. However, all the observations so far found only
a negligible amount of gas in GCs. We propose here to test different mechanisms
such as ram-pressure stripping by the motion of the GC in the galactic halo
medium and the inclusion of ionising sources to explain the lack of gas in GCs.
We use full 3D hydrodynamical simulations taking into account stellar winds,
ionising radiation, radiative heating and radiative pressure. We find that the
combining effect of ram-pressure and ionisation are able to explain the
negligible amount of gas observed in the core of intermediate-mass and massive
GCs.
