  We investigate the physical mechanisms of tidal heating and satellite
disruption in cold dark matter host haloes using N-body simulations based on
cosmological initial conditions. We show the importance of resonant shocks and
resonant torques with the host halo to satellite heating. A resonant shock
(torque) couples the radial (tangential) motion of a satellite in its orbit to
its phase space. For a satellite on a circular orbit, an ILR-like resonance
dominates the heating and this heating results in continuous satellite mass
loss. We estimate the requirements for simulations to achieve these dynamics
using perturbation theory. Both resonant shocks and resonant torques affect
satellites on eccentric orbits. We demonstrate that satellite mass loss is an
outside-in process in energy space; a satellite's stars and gas are thus
protected by their own halo against tidal stripping. We simulate the evolution
of a halo similar to the Large Magellanic Cloud (LMC) in our Galactic dark
matter halo and conclude that the LMC stars have not yet been stripped.
Finally, we present a simple algorithm for estimating the evolution of
satellite mass that includes both shock heating and resonant torques.
