| Abstract : | Comprehensive observations and numerical simulations of galaxy clusters suggest that gas deficiency in the galaxies could be due to ram pressure stripping due to the high-pressure intra-cluster medium acting on the galactic discs. To extensively study the dependency of the gas evolution in disc galaxies, we take an analytical approach to study ram pressure stripping (RPS), using analytical models for galactic disc density profile and the distribution of halo gas. The question of interest for the authors is: How does RPS vary with the ambient medium and the galaxy's properties? Our numerical explorations give us the amount of gas removed from the galaxy along with its distribution as the galaxy moves past the ambient medium. We have explored the dependence of RPS on ambient medium parameters like: their morphology, baryonic mass fraction and redshift. The parameters explored for the disc galaxies are their mass, spin parameter, orbit, asymmetries (like spiral structures) and magnetic fields. We find that galaxies in cluster halos get stripped of gas more efficiently as compared to group and galaxy halos. The non-radial orbits and infalling galaxies not being face-on decrease the amount of gas removed. We observe that the density of the gas concentrations, scale lengths, the mass of the spiral galaxies, the number of arms, and the width of arms all affect how efficient ram pressure stripping is. For a magnetized galaxy we find that, up until the cluster’s core, a strong magnetic field enables gas retention in the disc of the spiral galaxy, upto radius comparable to the disc scale radius, implying that the stripping rates are suppressed by a strong magnetic field, all the way upto centers of cluster. This naturally explains the presence of gas rich galaxies in dense cluster environments. |
