  We follow the evolution of disk galaxies within a cluster that forms
hierarchically in a cold dark matter N-body simulation. At a redshift z=0.5 we
select several dark matter halos that have quiet merger histories and are about
to enter the newly forming cluster environment. The halos are replaced with
equilibrium high resolution model spirals that are constructed to represent
examples of low surface brightness (LSB) and high surface brightness (HSB)
galaxies. Varying the disk and halo structural parameters reveals that the
response of a spiral galaxy to tidal encounters depends primarily on the
potential depth of the mass distribution and the disk scale length. LSB
galaxies, characterised by slowly rising rotation curves and large scale
lengths, evolve dramatically under the influence of rapid encounters with
substructure and strong tidal shocks from the global cluster potential ---
galaxy harassment. We find that up to 90% of their stars are tidally stripped
and congregate in large diffuse tails that trace the orbital path of the galaxy
and form the diffuse intra-cluster light. The bound stellar remnants closely
resemble the dwarf spheroidals (dE's) that populate nearby clusters. HSB
galaxies are stable to the chaos of cluster formation and tidal encounters.
These disks lie well within the tidally limited dark matter halos and their
potentials are more concentrated. Although very few stars are stripped, the
scale height of the disks increases substantially and no spiral features
remain, therefore we speculate that these galaxies would be identified as S0
galaxies in present day clusters.
