  Ram pressure stripping is an important process in the evolution of both dwarf
galaxies and large spirals. Large spirals are severely stripped in rich
clusters and may be mildly stripped in groups. Dwarf galaxies can be severely
stripped in both clusters and groups. A model is developed that describes the
stripping of a satellite galaxy's outer H \textsc{i} disk and hot galactic
halo. The model can be applied to a wide range of environments and satellite
galaxy masses. 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. How the effectiveness of ram
pressure stripping depends on the density of the inter-group gas, the dark
matter halo concentrations, and the scale lengths and masses of the satellite
components is explored. The predictions of the model are shown to be well
matched to H \textsc{i} observations of spirals in a sample of nearby clusters.
The model is used to predict the range of H \textsc{i} gas fractions a
satellite of mass $M_{v,sat}$ can lose orbiting in a cluster of mass
$M_{v,gr}$.
