Speaker
Dr
William Chantereau
(ARI (LJMU))
Description
Stars in old stellar clusters lose a non negligible amount of mass during their evolution. This material is then expected to build up a substantial intra-cluster medium. However, the observed gas content in these old stellar clusters is a couple of orders of magnitude below these expectations. We follow the evolution of the stellar wind material thanks to hydrodynamical simulations taking into account the ram-pressure stripping by the motion of the stellar cluster in the galactic halo medium and the inclusion of ionising sources to reconcile theoretical predictions with observations.
