  We model the dynamics of dwarf early-type galaxies in the Virgo cluster when
subject to a variety of environmental processes. We focus on how these
processes imprint trends in dynamical state (rotational vs. pressure support as
measured by the $\lambda^*_{\rm Re/2}$ statistic) with projected distance from
the cluster center, and compare these results to observational estimates. We
find a large scatter in the gradient of $\lambda^*_{\rm Re/2}$ with projected
radius. A statistical analysis shows that models with no environmental effects
produce gradients as steep as those observed in none of the 100 cluster
realizations we consider, while in a model incorporating tidal stirring by the
cluster potential 34% of realizations produce gradients as steep as that
observed. Our results suggest that tidal stirring may be the cause of the
observed radial dependence of dwarf early-type dynamics in galaxy clusters.
