The edge of galaxy formation II: evolution of Milky Way satellite
  analogues after infall
  In the first paper we presented 27 hydrodynamical cosmological simulations of
galaxies with total masses between $5 \times 10^8$ and
$10^{10}\,\mathrm{M}_\odot$. In this second paper we use a subset of these
cosmological simulations as initial conditions (ICs) for more than forty
hydrodynamical simulations of satellite and host galaxy interaction. Our
cosmological ICs seem to suggest that galaxies on these mass scales have very
little rotational support and are velocity dispersion ($\sigma$) dominated.
Accretion and environmental effects increase the scatter in the galaxy scaling
relations (e.g. size - velocity dispersion) in very good agreement with
observations. Star formation is substantially quenched after accretion. Mass
removal due to tidal forces has several effects: it creates a very flat stellar
velocity dispersion profiles, and it reduces the dark matter content at all
scales (even in the centre), which in turn lowers the stellar velocity on
scales around 0.5 kpc even when the galaxy does not lose stellar mass.
Satellites that start with a cored dark matter profile are more prone to either
be destroyed or to end up in a very dark matter poor galaxy. Finally, we found
that tidal effects always increase the "cuspyness" of the dark matter profile,
even for haloes that infall with a core.
