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Session 52 - Simulations of Clusters of Galaxies.
Display session, Tuesday, January 16
North Banquet Hall, Convention Center
X-ray and optical observations suggest that rotation may be dynamically significant in the cores of some cooling flow clusters. Evidence for the presence of disk-like structure has been found in recent ROSAT HRI X-ray images of A4059. Optical observations of Hydra A provide evidence for solid-body rotation within the inner 3-4 kpc of the cluster D galaxy. Motivated by these observations, we have performed 2D simulations of rotating cooling flows utilizing the hydrodynamical code ZEUS-3D. We first computed a spherically symmetric (1D) cooling flow in the gravitational potential of an elliptical galaxy and King model cluster distribution. A series of cooling flows with different mass dropout strengths were created to test the effects of rotation on the spherically symmetric solutions. The 1D solutions were perturbed by applying a rotation and their evolution followed assuming equatorial and rotation axis symmetry on the ZEUS-3D grid. The impact which rotation has on the different cooling flows is examined through deviations in X-ray morphology as well as other observables. This research was funded by NSF Grant AST93-17596.
