Finally, combining the results of local and high-redshift observations with the prediction of tuned models and simulations, we try to quantify the importance of this process on the evolution of galaxies of different mass, from dwarfs to giants, in various environments and at different epochs. We also discuss on the possible fate of the stripped material once removed from the perturbed galaxies and mixed with the ICM, and we try to estimate its contribution to the pollution of the surrounding environment. This indicates that the galaxy is having trouble holding onto the loosely bound. For example, NGC 4402 (right), which is currently falling into the Virgo cluster, shows several clear indicators that ram pressure stripping is at work: The disk of dust and gas appears bowed. We summarise the effects of this perturbing process on the baryonic components of galaxies, from the different gas phases (cold atomic and molecular, ionised, hot) to magnetic fields and cosmic rays, and describe their induced effects on the different stellar populations, with a particular attention to its role in the quenching episode generally observed in high-density environments. Evidence for ram pressure stripping can be found in many galaxy clusters. This review is aimed at describing this physical mechanism in different environments, from rich clusters of galaxies to loose and compact groups. the pressure exerted by the hot and dense intracluster medium (ICM) on galaxies moving at high velocity within the cluster gravitational potential well, is a key process able to remove their interstellar medium (ISM) and quench their activity of star formation. Among these, ram pressure stripping, i.e. First, the satellite experiences ram pressure stripping, which is gen- erally assumed to coincide with either initial infall or pericentric passage. Run a richer mixture at peak torque (or wherever peak cylinder pressure. Nowadays the process of ram-pressure stripping receives more and more attention. In each case we model the worst case scenario (i.e., maximum effect due to ram pressure). the surface mass density of the galactic gas. We also study variations with galaxy properties and redshift. Galaxies living in rich environments are suffering different perturbations able to drastically affect their evolution. 024 exh very rough 992 n comment: street strip, 9. 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.
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