  We present the first high-resolution N-Body/SPH simulations that follow the
evolution of low surface brightness disk satellites in a primary halo
containing both dark matter and a hot gas component. Tidal shocks turn the
stellar disk into a spheroid with low $v/\sigma$ and remove most of the outer
dark and baryonic mass. In addition, by weakening the potential well of the
dwarf, tides enhance the effect of ram pressure, and the gas is stripped down
to radius three times smaller than the stellar component A very low gas/stars
ratio results after several Gyr, similarly to what seen in dwarf spheroidal
satellites of the Milky Way and M31.
