We investigate the dynamical behaviour of disk galaxies orbiting withi
n the potential well of a galaxy cluster, We focus on the morphologica
l changes induced on halo+bulge+disk N-body galaxy models by cluster t
ides, as well as on possible modifications to the shape of their rotat
ion curves, Galaxy clusters are modelled as spherical potential wells
whose mass distribution is either static or evolves slowly in accordan
ce with a simple infall model, We find that galaxies can be totally di
srupted if they are on nearly radial orbits or if they are accreted in
to the cluster at high redshift, when clusters are denser, Less dramat
ic effects are seen for galaxies on less eccentric orbits or accreted
into the cluster at low redshift, although in many cases tides call le
ad to a significant rearrangement of the mass of the halo, a thickenin
g of the disk, and a declining rotation curve.