  We report the results of N-body simulations of disrupting satellites aimed at
exploring whether the observed features of dSphs can be accounted for with
simple, mass-follows-light (MFL) models including tidal disruption. As a test
case, we focus on the Carina dwarf Spheroidal (dSph), which presently has the
most extensive data at large radius. We find that previous N-body, MFL
simulations of dSphs did not sufficiently explore the parameter space of
satellite mass, density and orbital shape to find adequate matches to Galactic
dSph systems, whereas with a systematic survey of parameter space we are able
to find tidally disrupting, MFL satellite models that rather faithfully
reproduce Carina's velocity profile, velocity dispersion profile and projected
density distribution over its entire sampled radius. The successful MFL model
satellites have very eccentric orbits, currently favored by Cold Dark Matter
(CDM) models, and central velocity dispersions that still yield an accurate
representation of the bound mass and observed central M/L~40 of Carina, despite
inflation of the velocity dispersion outside the dSph core by unbound debris.
Our survey of parameter space also allows us to address a number of commonly
held misperceptions of tidal disruption and its observable effects on dSph
structure and dynamics. The simulations suggest that even modest tidal
disruption can have a profound effect on the observed dynamics of dSph stars at
large radii. Satellites that are well-described by tidally disrupting MFL
models could still be fully compatible with L-CDM if for example they represent
a later stage in the evolution of luminous subhalos.
