| Abstract : | The environment of a galaxy plays a significant role in shaping the distribution of matter around it. Due to the motion of a galaxy through its host intracluster medium (ICM), it experiences ram pressure. This strips the gaseous component of the galaxy without perturbing its stellar distribution. Ram pressure stripping (RPS) can result in long tails of ionized gas in the wake of its path, with the most spectacular cases referred to as ‘jellyfish galaxies’. RPS is the most plausible mechanism to suppress star formation in such galaxies. In our recent work (Ghosh et al. 2023; submitted to MNRAS), we carry out 3D hydrodynamical simulations of RPS (without radiative cooling) of a galaxy, including both the interstellar and circumgalactic media (ISM and CGM, respectively). For a satellite galaxy, previous simulations often assumed the CGM to be entirely stripped/evaporated, an assumption we find is not always justified. For a typical galaxy like JO206, we find that the CGM survives long at cluster outskirts (> 2Gyr). At smaller cluster-centric distances, 90% of the CGM mass is lost in about 500 Myr. Being loosely bound, the gravitational restoring force on the CGM is mostly negligible, and the CGM-ICM interaction is analogous to ‘cloud-wind interaction’. In my talk, I will discuss the distinct regimes that emerge for CGM stripping depending on χ, the ratio of CGM to ICM density. I would elaborate on the 'cloud crushing' (χ > 1) and the relatively unexplored 'bubble drag' (χ < 1) regimes. We find that the disk stripping criterion still depends on the ram pressure and follows the classic Gunn and Gott 1972 condition. The stripped tails of satellites are found to have contributions from both the disk and trailing CGM. |
