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Observationally, the quenching of star-forming galaxies appears to dependboth on their mass and environment. The exact cause of the environmentaldependence is still poorly understood, yet semi-analytic models (SAMs) ofgalaxy formation need to parameterise it to reproduce observations of galaxyproperties. In this work, we use hydrodynamical simulations to investigate thequenching of disk galaxies through ram-pressure stripping (RPS) as they fallinto galaxy clusters with the goal of characterising the importance of thiseffect for the reddening of disk galaxies. Our set-up employs a live model of agalaxy cluster that interacts with infalling disk galaxies on different orbits.We use the moving-mesh code AREPO, augmented with a special refinement strategyto yield high resolution around the galaxy on its way through the cluster in acomputationally efficient way. Our direct simulations differ substantially fromstripping models employed in current SAMs, which in most cases overpredict themass loss from RPS. Furthermore, after pericentre passage, as soon as rampressure becomes weaker, gas that remains bound to the galaxy is redistributedto the outer parts, an effect that is not captured in simplified treatements ofRPS. Star formation in our model galaxies is quenched mainly because the hotgas halo is stripped, depriving the galaxy of its gas supply. The cold gas diskis only stripped completely in extreme cases, leading to full quenching andsignificant reddening on timescale of ~200 Myr. On the other hand, galaxiesexperiencing only mild ram pressure actually show an enhanced star formationrate that is consistent with observations and are quenched on timescales > 1Gyr. Stripped gas in the wake is mixed efficiently with intracluster gasalready a few tens of kpc behind the disk, and this gas is free of residualstar formation.

Simulations of ram-pressure stripping in galaxy-cluster interactions