Heating the Intracluster Medium: Magnetohydrodynamic (MHD) Simulations of Shock/Bubble Rotational Heating

Type Conference Paper
Names Samuel H. Friedman, S. Heinz
Proceedings Title Bulletin of the American Astronomical Society
Conference Name American Astronomical Society, AAS Meeting #215, #436.18
Volume 42
Pages 387
Date January 1, 2010
Short Title Heating the Intracluster Medium
URL http://adsabs.harvard.edu/abs/2010AAS...21543618F
Library Catalog NASA ADS
Abstract Recent observations of galaxy clusters show that temperatures of the intracluster medium (ICM) lie in the range of 10-100 million K. We would expect this gas to cool via radiative cooling; however, we do not observe this cooling. One way of keeping the ICM hot involves the coupling of jets emanating from supermassive black holes at the centers of galaxies within the cluster with the ICM. The energies involved in the bubbles that these jets inflate in the ICM can provide sufficient energy to heat the gas. However, we do not know how the jet energy becomes thermalized; we present a mechanism that will thermalize the jet energy. The jets have a duty cycle which can cause a shock wave to run across a previously inflated underdense bubble in the ICM. The resulting instability (Richtmyer-Meshkov) causes energy from the shock/jet to transform into rotational kinetic energy, which can then thermalize through turbulence and viscosity. We present the results of shock/bubble interactions with 2D and 3D hydrodynamic and magnetohydrodynamic (MHD) simulations.
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