  A simple and natural explanation for the dynamics and morphology of the Local
Group Dwarf Spheroidal galaxies, Draco (Dra) and Ursa Minor (UMi), is that they
are weakly unbound stellar systems with no significant dark matter component. A
gentle, but persistent, Milky Way (MW) tide has left them in their current
kinematic and morphological state. This short paper reviews the parametric
tidal interaction model which accounts for their behavior and discusses new
statistical evidence from the observed stellar distribution in Dra which
implies that its total mass is not dominated by collisionless dark matter (DM).
