  We review progress in understanding the formation of galactic disks in the
standard cosmogonic scenario involving gravitational clustering of baryons and
dark matter and dissipative collapse of the baryons. This scenario accounts
remarkably well for the observed properties of galactic disks if they have
retained most of the specific angular momentum they acquired by tidal torques.
Early simulations, which included cooling of the gas but not star formation and
the associated feedback, indicated instead that most of the angular momentum of
the baryons would be transferred to the dark matter. Recent simulations
indicate that this angular-momentum problem can be solved partially, and in
some cases entirely, by feedback and other effects.
