Numerical simulations of rotating cooling flow clusters

We present the results of 2D numerical simulations of spherically symmetric, steady-state cooling flows with varying mass-dropout strengths undergoing a rotational perturbation. Rotation serves to break the spherical symmetry of the cooling flow and initiates the formation of disk-like structure extending out to similar to 10 kpc. For low mass-dropout strength simulations we find evidence for cooling instabilities formed by Kelvin-Helmholtz instabilities within the disk-like structure. The higher mass-dropout strength simulations do not form cooling instabilities within the disk-like structure due to the decreased degree of cooling within this environment. Morphological comparisons of the disk-like structures are made with observations of the X-ray emitting gas of A4059. The influence of imposing axi-symmetry on the simulation evolution is briefly discussed.