  We present new three dimensional, hydrodynamic simulations of the ram
pressure stripping of disc galaxies via interaction with an hot intracluster
medium (ICM). The simulations were carried with the smoothed-particle
hydrodynamics, adaptive mesh 'Hydra' code (SPH-A$P^3$M), with model galaxies
consisting of dark halo, and gas and stellar disc components. The simulations
also include radiative cooling, which is important for keeping the warm,
diffuse gas of moderate density from being unrealistically heated by the ICM.
We examine the role that wind velocity, density and galaxy tilt play in gas
stripping.
  The onset of the ICM wind has a profound effect on the disc gas that is not
immediately stripped. This remnant disc is displaced relative to the halo
center and compressed. This can trigger gravitational instability and the
formation of numerous flocculent spirals. These waves transport angular
momentum outward, resulting in further compression of the inner disc and the
formation of a prominent gas ring. This 'annealing' process makes the inner
disc, which contains much of the total gas mass, resistant to further
stripping, but presumably susceptible to global starbursts.
  When the mass loss and annealing processes go to completion we find that the
total amount of mass lost from a fixed target galaxy is well fit by a simple
power-law function of a dimensionless parameter that combines the ram pressure
and internal properties of the galaxy. (abs. abbreviated)
