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Recent observations suggest that rotation may be dynamically significant in the cores of some cooling flow clusters (e.g. Hydra-A). We have therefore begun to investigate the effect of rotation on the properties of cooling flows. This was performed by first computing a spherically symmetric cooling flow in the gravitational potential of an elliptical galaxy and King model cluster distribution. The 1D solution was perturbed by applying a rotation and its evolution followed using an axisymmetric hydrodynamical code. The effects of different rotation profiles and rotation strengths have been studied, and will be presented.
