Length Scales and Turbulent Properties of Magnetic Fields in Simulated
  Galaxy Clusters
  Additional physics beyond standard hydrodynamics is needed to fully model the
intracluster medium (ICM); however, as we move to more sophisticated models, it
is important to consider the role of magnetic fields and the way the fluid
approximation breaks down. This paper represents a first step towards
developing a self-consistent model of the ICM by characterizing the statistical
properties of magnetic fields in cosmological simulations of galaxy clusters.
We find that plasma conditions are largely homogeneous across a range of
cluster masses and relaxation states. We also find that the magnetic field
length scales are resolution dependent and not based on any particular physical
process. Energy transfer mechanisms and scales are also identified, and imply
the existence of small scale dynamo action. The scales of the small scale
dynamo are resolution limited and driven by numerical resistivity and
viscosity.
