The model is used to predict the range of H I gas fractions that a satellite of mass M v,sat can lose orbiting in a cluster of mass M v,gr.
The predictions of the model are shown to be well matched to H I observations of spirals in a sample of nearby clusters. How the effectiveness of ram pressure stripping depends on the density of the intergroup gas, the dark matter halo concentrations, and the scale lengths and masses of the satellite components is explored. Our results suggest that if there is any ram pressure stripping induced enhancement, it is at best locally modest, and galaxies undergoing enhancement make up a. The density of the ambient medium decreases as we decrease the mass, suppressing the effect of ram pressure. Interaction between the intracluster medium and the interstellar media of galaxies via ram-pressure stripping (RPS) has ample support from both observations. Whether ram pressure stripping of the outer disk or hot galactic halo occurs is found to depend primarily on the ratio of the satellite galaxy mass to the mass of the host group or cluster. We next describe ram pressure stripping in a group environment where the halo mass of the group is assumed to be 2 × 10 13.5 M. The model can be applied to a wide range of environments and satellite galaxy masses. A model is developed that describes the stripping of a satellite galaxy's outer H I disk and hot galactic halo. Dwarf galaxies can be severely stripped in both clusters and groups. This approach closely reproduces results from SPH simulations. This parameter pair fully describes the gas mass fraction that is stripped from a given galaxy. Large spirals are severely stripped in rich clusters and may be mildly stripped in groups. For shorter pulses the outcome depends on the time-integrated ram pressure. Dwarf galaxies can be severely stripped in both clusters and groups. The Astrophysical Journal Ram pressure stripping is an important process in the evolution of both dwarf galaxies and large spirals.
We solved the model equations numerically in two dimensions and extended the range of parameters beyond the range. Our equations differ from those of Gaetz, Salpeter, and Shaviv in the treatment of the motion of stars in the galaxy. Large spirals are severely stripped in rich clusters and may be mildly stripped in groups. We examine the physical assumptions and the basic hydrodynamic equations of the ram pressure stripping model for elliptical galaxies in clusters of galaxies. For turbulent stripping, he found a mass stripping rate of 1 where r 10 r10 kpc, ICM 10 -3n-3mH g cm -3 and v 1000 v3 km s -1. Ram pressure stripping is an important process in the evolution of both dwarf galaxies and large spirals. Nulsen (1982) has studied the effects of transport processes and turbulence on the flow of gas past a galaxy and has found that they could produce more stripping of gas than ram pressure alone.
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