When Clusters Collide: A Numerical Hydro/N-Body Simulation of Merging Galaxy Clusters

We present initial results from a three-dimensional numerical simulation of two merging clusters of galaxies. This is the first such simulation employing a hybrid Hydro/N-body code where the hydrodynamics is solved by an Eulerian, finite-difference method. The hybrid code allows for the self-consistent evolution of the intracluster medium (ICM), represented by the fluid equations of hydrodynamics, within a gravitational potential defined by the cluster dark matter as represented by the N-body particle distribution. Initial results reveal a broadening and elongation of the X-ray emission with respect to the initial cluster, a complex temperature and density structure resulting from multiple shocks, and sustained high-velocity gas motions within the ICM accompanied by significant postmerger heating within the core of the dominant cluster. These results provide a possible mechanism for the disruption of cooling flows and the bending of wide-angle tailed radio sources (WATs). We present synthetic X-ray images at various epochs which can be compared directly with new ROSAT data.