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M. Ruszkowski (JILA, University of Colorado at Boulder), M.C. Begelman (JILA, APS, University of Colorado at Boulder)
It is now widely accepted that the temperatures of cooling flow cluster cores are maintained at a level of approximately 1 keV and that the mass deposition rates are lower than earlier ROSAT/Einstein estimates. We consider a model which incorporates the effects of simultaneous heating by both the central AGN "effervescent heating" and thermal conduction from the hot outer layers of clusters. Using ZEUS 1D hydrodynamical simulations, we demonstrate that there exists a family of solutions that does not suffer from the cooling catastrophe. In these cases, clusters relax to a stable final state, which is characterized by minimum temperatures of order 1 keV and density and temperature profiles consistent with observations. Moreover, the accretion rates are much reduced, thereby reducing the need for excessive mass deposition rates required by the standard cooling flow models. Although relatively small amount of conduction is required, we find that the energy input to the cluster is dominated by AGN. Using the FLASH code, we perform adaptive mesh refinement 2.5D simulations of the AGN heating to test the form of the effervescent heating function used in the ZEUS simulations.
The author(s) of this abstract have provided an email address for comments about the abstract: mr@quixote.colorado.edu
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.