  We study numerical simulations of satellite galaxy disruption in a potential
resembling that of the Milky Way. Our goal is to assess whether a merger origin
for the stellar halo would leave observable fossil structure in the phase-space
distribution of nearby stars. We show how mixing of disrupted satellites can be
quantified using a coarse-grained entropy. Although after 10 billion years few
obvious asymmetries remain in the distribution of particles in configuration
space, strong correlations are still present in velocity space. We briefly
describe how we can understand these effects based on the conservation of
fine-grained phase-space density in an action-angle formalism. We also discuss
the implications of our results on the known properties of the stellar halo.
