  By means of simple numerical models we discuss whether "collisionless stellar
evaporation" from cluster elliptical galaxies could be an effective mechanism
for the production of intracluster stellar populations. The effectiveness of
this mechanism is due to the fact that, for realistic galaxy and cluster
models, the galaxy oscillation periods near equilibrium configurations in the
cluster tidal field are of the same order of stellar orbital times in the
external parts of the galaxies themselves. With the aid of Monte-Carlo
simulations we explore the evolution of stellar orbits in oscillating galaxies
placed near different equilibrium positions. We found that, over an Hubble
time, the main effect is a substantial expansion of the galactic outskirts,
particularly affecting the galaxy at the cluster center and those orbiting near
the cluster core radius: overall, approximately the 10% of the galaxy mass is
affected. Thus, the proposed mechanism could be of some importance in the
shaping of the halo of cD galaxies and in making easier ``galaxy harassment''
in the formation of the intracluster stellar population.
