The Formation of Cluster Cooling Cores within a Complex Supercluster Environment

Details The Formation of Cluster Cooling Cores within a Complex Supercluster Environment The Formation of Cluster Cooling Cores within a Complex Supercluster Environment

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...198.9202m&link_type=abstract

American Astronomical Society, 198th AAS Meeting, #92.02; Bulletin of the American Astronomical Society, Vol. 33, p.1178

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We present preliminary results from the simulation of cluster formation that include the effects of radiative cooling by the gas for a Λ CDM cosmological model. In adiabatic simulations of structure formation, a network of filaments is observed which conveys material into the clusters. This phenomena of highly non-spherical accretion is also observed when radiative cooling is present. In addition, the accreted substructures often possess dense cores that may donate pre-cooled gas to the primary cooling core or disrupt the signature of the dominant cooling core. The simulations indicate a cluster history that differs greatly from the view of an isolated, spherically symmetric cooling flow and paints a new picture for the formation of cooling cores in rich clusters as the result of accretion of cool groups from supercluster filaments. We will examine the implications of the interaction of the central cooling core with its environment for the interpretation of recent X-Ray observations. An adaptive mesh Eulerian code was used in the simulations. The highest level of refinement employed corresponds to 15 h-1 kpc within a computational volume of 2563 h-3 Mpc3. The computations presented were performed on the SGI Origin 2000 cluster at NCSA.

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