  In recent years, realistic hydrodynamical simulations of galaxies like the
Milky Way have become available, enabling a reliable estimate of the dark
matter density and velocity distribution in the Solar neighborhood. We review
here the status of hydrodynamical simulations and their implications for the
interpretation of direct dark matter searches. We focus in particular on: the
criteria to identify Milky Way-like galaxies; the impact of baryonic physics on
the dark matter velocity distribution; the possible presence of substructures
like clumps, streams, or dark disks; and on the implications for the direct
detection of dark matter with standard and non-standard interactions.
