On the relevance of chaos for halo stars in the solar neighbourhood II
  In a previous paper based on dark matter only simulations we show that, in
the approximation of an analytic and static potential describing the strongly
triaxial and cuspy shape of Milky Way-sized haloes, diffusion due to chaotic
mixing in the neighbourhood of the Sun does not efficiently erase phase space
signatures of past accretion events. In this second paper we further explore
the effect of chaotic mixing using multicomponent Galactic potential models and
solar neighbourhood-like volumes extracted from fully cosmological hydrodynamic
simulations, thus naturally accounting for the gravitational potential
associated with baryonic components, such as the bulge and disc. Despite the
strong change in the global Galactic potentials with respect to those obtained
in dark matter only simulations, our results confirm that a large fraction of
halo particles evolving on chaotic orbits exhibit their chaotic behaviour after
periods of time significantly larger than a Hubble time. In addition,
significant diffusion in phase space is not observed on those particles that do
exhibit chaotic behaviour within a Hubble time.
