  We follow the evolution of disk galaxies within a cluster that forms
hierarchically in a standard 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 luminous examples of low surface brightness (LSB) and high surface
brightness (HSB) galaxies. Whilst the models have the same total luminosity,
\sim L_*, they have very different internal mass profiles, core radii and disk
scale lengths, however they all lie at the same place on the Tully-Fisher
relation. Due to their ``soft'' central potentials, LSB galaxies evolve
dramatically under the influence of rapid encounters with dark matter halos,
substructure and strong tidal shocks from the global cluster potential - galaxy
harassment. As much as 90% of the LSB disk 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, with large
scale lengths and low central surface brightness.
