X-ray and radio observations of galaxy clusters have revealed a wealth of
structures in association with extragalactic radio sources. Structures in
the form of large-scale cavities and weak shocks provide a reliable gauge
of the energy output of extragalactic radio jets launched by AGNs.
Furthermore, they place interesting constraints on the nature of AGN
outflows, especially on large scales. We will present 3-D MHD simulations
of jets/lobes in the ICM and compare them with ~70 X-ray cavities as well
as individual jet/lobe sources. In addition, we will present cosmological
MHD simulations of galaxy cluster formation with AGN jets/lobes feedback
and its implications for the origin and energetics of the cluster-wide
magnetic fields. We demonstrate that the ICM turbulence is excited and
sustained by the frequent mergers during the cluster formation. We
quantify the available turbulent kinetic energy and nonlinear cascade
rates. This turbulence excites a small-scale dynamo process that
transports and amplifies the fields originated from the radio jet/lobe
system. This process could be the primary process of populating the whole
cluster with magnetic fields. We describe the properties of magnetic
fields, including their strength, spatial distribution, power spectra and
saturation mechanism. These simulations can be compared with observations
made by VLA, LOFAR, and E-VLA.
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