NATs are common in clusters of galaxies, and their distinctive structures reveal strong interactions with the cluster media driven by transsonic or supersonic relative motions. These interactions disrupt the AGN outflows and control the deposition of AGN energy, entropy, magnetic field and relativistic particles into the ICM. While this general picture is commonly understood, only relatively basic modeling has been carried out to date. We have begun a detailed simulation study exploring the fundamental interaction issues outlined above, based on high resolution 3D MHD calculations. The simulations incorporate passive relativistic electron populations followed with our Eulerian, Coarse-Grained finite Momentum Volume scheme. The electrons are subject to Fermi acceleration as well as adiabatic and nonadiabatic energy gains and losses, so realistic nonthermal emissions are computed that can be used to construct important diagnostic synthetic observations. We report on preliminary analysis of runs on a Microsoft 256-node (2048 cores) cluster running Windows HPC server 2008.