Simulating the Cooling Flow of Cool-Core Clusters

Details Simulating the Cooling Flow of Cool-Core Clusters Simulating the Cooling Flow of Cool-Core Clusters

Aug 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011scgg.conf...30l&link_type=abstract

"Structure in Clusters and Groups of Galaxies in the Chandra Era, 2011 Chandra Science Workshop held July 12-14, 2011. Edited by

Physics

Scientific paper

In an attempt to better understand the cooling flow problem of galaxy clusters, we simulate the onset of the cooling instability of the hot gas in the center of cool-core clusters using Enzo, an adaptive mesh refinement (AMR) code. The 3D simulation setup is such that the initial gas density profile matches the observations of Perseus Cluster with an NFW dark matter potential. We find that the cooling instability happens globally, causing the temperature to drop and the density to increase within r ˜ a few tens of pc. The amount of cold gas remains in good agreement with observations when the gas inflow is strong enough to potentially trigger feedback that stifles the cooling flow.

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