  We examine the problem tidally-induced mass loss from collisionless systems
such as dark matter haloes. We develop a model for tidal mass loss, based upon
the phase space distribution of particles, which accounts for how both tidal
and Coriolis torques perturb the angular momentum of each particle in the
system. This allows us to study how both the density profile and velocity
anisotropy affect the degree of mass loss--we present basic results from such a
study. Our model predicts that mass loss is a continuous process even in a
static tidal field, a consequence of the fact that mass loss weakens the
potential of the system making it easier for further mass loss to occur. We
compare the predictions of our model with N-body simulations of idealized
systems in order to check its validity. We find reasonable agreement with the
N-body simulations except for in the case of very strong tidal fields, where
our results suggest that a higher-order perturbation analysis may be required.
The continuous tidally-induced mass loss predicted by our model can lead to
substantial reduction in satellite mass in cases where the traditional
treatment predicts no mass loss. As such, our results may have important
consequences for the orbits and survival of low mass satellites in dark matter
haloes.
