Figure 6: (a) Ratio between the line-of-sight velocity dispersions for component and ( ) as a function of the projected distance from the center of the dwarf. The mos distant bin considered has at least 20 particles from each component (and more for for bins closer in). (b) The upper panel shows the fraction of mass (compared to the initial value) that remains bound to the satellite as a function of time for orbit 2. Dotted, red solid and blue-dashed curves are used to indicate the dark matter, and stellar components and respectively. In the bottom the evolution with time of the ratio between the velocity dispersions of and is shown for two regions within the dwarf: stars within two core radii (magenta dashed) and stars approximately lying closer to the tidal radius (green solid). These ratios have been normalized to the original values ( , thin black line in the right panel).