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In the first paper we presented 27 hydrodynamical cosmological simulations ofgalaxies with total masses between $5 \times 10^8$ and$10^{10}\,\mathrm{M}_\odot$. In this second paper we use a subset of thesecosmological simulations as initial conditions (ICs) for more than fortyhydrodynamical simulations of satellite and host galaxy interaction. Ourcosmological ICs seem to suggest that galaxies on these mass scales have verylittle rotational support and are velocity dispersion ($\sigma$) dominated.Accretion and environmental effects increase the scatter in the galaxy scalingrelations (e.g. size - velocity dispersion) in very good agreement withobservations. Star formation is substantially quenched after accretion. Massremoval due to tidal forces has several effects: it creates a very flat stellarvelocity dispersion profiles, and it reduces the dark matter content at allscales (even in the centre), which in turn lowers the stellar velocity onscales 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 eitherbe destroyed or to end up in a very dark matter poor galaxy. Finally, we foundthat tidal effects always increase the "cuspyness" of the dark matter profile,even for haloes that infall with a core.

The edge of galaxy formation II: evolution of Milky Way satellite analogues after infall