A non-ideal MHD Gadget: Simulating massive galaxy clusters
  Magnetic fields in the intra-cluster medium of galaxy clusters have been
studied in the past years through different methods. In the next years the
up-coming generation of radio telescopes is going to provide new data that have
the potential of setting constraints on the properties of magnetic fields in
galaxy clusters. Here we present zoomed-in simulations for a set of massive
galaxy clusters (M_v > 10^15 M_sun/h). This is an ideal sample to study the
evolution of magnetic field during the process of structure formation in
detail. Turbulent motions of the gas within the ICM will manifest themselves in
a macroscopic magnetic resistivity eta_m, which has to be taken explicitly into
account, especially at scales below the resolution limit. We have adapted the
MHD GADGET code by Dolag & Stasyszyn (2009) to include the treatment of the
magnetic resistivity and for the first time we have included non-ideal MHD
equations to better follow the evolution of the magnetic field within galaxy
clusters. We investigate which value of the magnetic resistivity eta_m is
required to match the magnetic field profile derived from radio observations.
We find that a value of eta_m ~ 6 10^27 cm^2/s is necessary to recover the
shape of the magnetic field profile inferred from radio observations of the
Coma cluster. This value agrees well with the expected level of turbulent
motions within the ICM at our resolution limit. The magnetic field profiles can
be fitted by a beta-model like profile (Cavaliere & Fusco-Femiano 1976), with
small dispersion of the parameters. We find also that that the temperature,
density and entropy profiles of the clusters depend on the magnetic resistivity
constant, having flatter profiles in the inner regions when the magnetic
resistivity increases.
