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X-ray observations of clusters of galaxies reveal the presence of edges insurface brightness and temperature, known as "cold fronts". In relaxed clusterswith cool cores, these commonly observed edges have been interpreted asevidence for the "sloshing" of the core gas in the cluster's gravitationalpotential. Such sloshing may provide a source of heat to the cluster core bymixing hot gas from the cluster outskirts with the cool core gas. Usinghigh-resolution $N$-body/Eulerian hydrodynamics simulations, we model gassloshing in galaxy clusters initiated by mergers with subclusters. Thesimulations include merger scenarios with gas-filled and gasless subclusters.The effect of changing the viscosity of the intracluster medium is alsoexplored. We find that sloshing can facilitate heat inflow to the cluster core,provided that there is a strong enough disturbance. In adiabatic simulations,we find that sloshing can raise the entropy floor of the cluster core by nearlyan order of magnitude in the strongest cases. If the ICM is viscous, the mixingof gases with different entropies is decreased and consequently the heat fluxto the core is diminished. In simulations where radiative cooling is included,we find that though eventually a cooling flow develops, sloshing can preventthe significant buildup of cool gas in the core for times on the order of a Gyrfor small disturbances and a few Gyr for large ones. If repeated encounterswith merging subclusters sustain the sloshing of the central core gas as isobserved, this process can provide a relatively steady source of heat to thecore, which can help to prevent a significant cooling flow.

Stirring Up the Pot: Can Cooling Flows In Galaxy Clusters Be Quenched By Gas Sloshing?