The loss of the intra-cluster medium in globular clusters

Abstract

Stars in globular clusters (GCs) lose a non negligible amount of mass during their post-main sequence evolution. This material is then expected to build up a substantial intra-cluster medium (ICM) within the GC. However, the observed gas content in GCs is a couple of orders of magnitude below these expectations. Here we follow the evolution of this stellar wind material through hydrodynamical simulations to attempt to reconcile theoretical predictions with observations. We test different mechanisms proposed in the literature to clear out the gas such as ram-pressure stripping by the motion of the GC in the Galactic halo medium and ionisation by UV sources. We use the code ramses to run 3D hydrodynamical simulations to study for the first time the ICM evolution within discretised multi-mass GC models including stellar winds and full radiative transfer. We find that the inclusion of both ram-pressure and ionisation is mandatory to explain why only a very low amount of ionised gas is observed in the core of GCs. The same mechanisms operating in ancient GCs that clear the gas could also be efficient at younger ages, meaning that young GCs would not be able to retain gas and form multiple generations of stars as assumed in many models to explain "multiple populations". However, this rapid clearing of gas is consistent with observations of young massive clusters.

11 pages, 5 figures, accepted for publication in MNRAS

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• Simulations of globular clusters within their parent galaxies: Metallicity spreads and anomalous precursor populations
• Accretion of sub-stellar companions as the origin of chemical abundance inhomogeneities in globular clusters
• How many explosions does one need? -- Quantifying supernovae in globular clusters from iron abundance spreads
• Ionising Feedback Effects on Star Formation in Globular Clusters with Multiple Stellar Populations
• Star Cluster Ecology: Revisiting the Origin of Iron and Age Complex Clusters