Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprj11007m&link_type=abstract
American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As
Astronomy and Astrophysics
Astrophysics
Scientific paper
New state of the art large-scale structure simulations have suggested a novel scenario for the formation of cooling cores in rich clusters. We find that cores of cool gas, material that would be identified as a classical cooling flow based upon its X-Ray luminosity excess and temperature profile, are built from the accretion of discrete, stable subclusters. Any ``cooling flow'' present is overwhelmed by the velocity field within the cluster. Thus, the inclusion of consistent initial cosmological conditions for the cluster within its surrounding environment is crucial when attempting to address the evolution of cooling cores in rich galaxy clusters. This new model for the hierarchical assembly of cooling cores naturally explains the high frequency of these cores in rich galaxy clusters despite the fact that a majority of rich clusters also show evidence of substructure which is believed to arise from recent merger activity. Also, complex filamentary structures of cool gas in our simulations appear similar to those seen in recent Chandra observations. Our simulations were computed with a coupled N-body, Eulerian AMR hydrodynamics cosmology code that properly treats the effects of radiative cooling by the gas. We employ seven levels of refinement to attain a peak resolution of 15.6 h-1 kpc within a volume 256 h-1 Mpc on a side and assume a standard ΛCDM cosmology.
Bryan Greg
Burns Jack
Loken Chris
Motl Patrick
Norman Michael
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