Angular momentum evolution of galaxies: the perspective of
  hydrodynamical simulations
  Until a decade ago, galaxy formation simulations were unable to
simultaneously reproduce the observed angular momentum (AM) of galaxy disks and
bulges. Improvements in the interstellar medium and stellar feedback modelling,
together with advances in computational capabilities, have allowed the current
generation of cosmological galaxy formation simulations to reproduce the
diversity of AM and morphology that is observed in local galaxies. In this
review I discuss where we currently stand in this area from the perspective of
hydrodynamical simulations, specifically how galaxies gain their AM, and the
effect galaxy mergers and gas accretion have on this process. I discuss results
which suggest that a revision of the classical theory of disk formation is
needed, and finish by discussing what the current challenges are.
