  One mechanism for the external destruction of protoplanetary discs in young
dense clusters is tidal disruption during the flyby of another cluster member.
The degree of mass loss in such an encounter depends, among other parameters,
on the distribution of the material within the disc. Previous work showed that
this is especially so in encounters that truncate large parts of the outer
disc. The expectation is that the number of completely destroyed discs in a
cluster depends also on the mass distribution within the discs. Here we test
this hypothesis by determining the influence of encounters on the disc fraction
and average disc mass in clusters of various stellar densities for different
mass distributions in the discs. This is done by performing Nbody6 simulation
of a variety of cluster environments, where we track the encounter dynamics and
determine the mass loss due to these encounters for different disc-mass
distributions. We find that although the disc mass distribution has a
significant impact on the disc losses for specific star-disc encounters, the
overall disc frequency generally remains rather unaffected. The reason is that
in single encounters the dependence on the mass distribution is strongest if
both stars have very different masses. Such encounters are rather infrequent in
sparse clusters. In dense clusters such encounters are more common, however,
here the disc frequency is largely determined by encounters between low-mass
stars such that the overall disc frequency does not change significantly. For
tidal disruption the disc destruction in clusters is fairly independent of the
actual distribution of the material in the disc. The all determining factor
remains the cluster density.
