![]() ![]() = and H I, also implying recent changes in the distributions of gas and star formation. In each case we model the worst case scenario (i.e., maximum effect due to ram pressure). We also study variations with galaxy properties and redshift. Most spectacularly, star clusters can form downstream in stripped-off massive gas clouds in the case of strong RP. We use an analytical approach to study ram pressure stripping with simple models for discs and halo gas distribution to study the phenomena in cluster, group and galaxy halos. When gas clouds are still bound against stripping but lifted from a thin disc and fall back, more ยป their new stars form an ellipsoidal (young) stellar population already with a larger velocity dispersion without the necessity of harassment. Under some conditions, RP can compress the gas, so that it is unexpectedly retained in the central DG region and forms stars. We demonstrated that SF can be either suppressed or triggered by RP depending on the ICM density and the DGs mass. Using a series of numerical simulations, we quantify the dependence of the stripped-off gas on the velocity of the infalling DGs and on the ambient ICM density. Since cluster early-type DGs also show a large variety of internal structures (unexpected central gas reservoirs, blue stellar cores, composite radial stellar profiles), we aim in this study to investigate how ram pressure (RP) affects the interstellar gas content and therefore the star formation (SF) activity. Ram-pressure stripping as the dominant mechanism is also. Previous numerical simulations based on various approaches suggested that, except for near edge-on disk orientations, the amount of stripping depends very little on the inclination angle. In a few objects in close by galaxy clusters and the field, RPS has been observed. 2006, 2007, 2010), indicating that the other gas phases can also be perturbed during the interaction. Context:Ram pressure stripping of galaxies in clusters can yield gas deficient disks. ![]() step: is the stepwidth for the numerical solution of the equation of motion of each particle. For dwarf galaxies (DGs) within a cluster, the transformation from gaseous to gas-poor systems by RPS is not easily observed and must happen in the outskirts of clusters. Simulation of a galaxy undergoing ram pressure stripping. ABSTRACT Ram-pressure stripping (RPS) is a well observed phenomenon of massive spiral galaxies passing through the hot intracluster medium (ICM) of galaxy clusters. ![]()
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