MHD Simulations of Clusters of Galaxies Including Radiative Cooling

We carried out 2D and 3D magnetohydrodynamic simulations including radiative cooling and anisotropic thermal conduction of a magnetically turbulent intracluster medium. In 3D simulations, we found that magnetic pressure increases by a factor of 2 at 1.4 Gyr because magnetic fields accumulate in the center along with the plasma contracting by the cooling instability. In 2D simulations including thermal conduction, we found that a low temperature region exists along the loop-shaped magnetic field lines. Thus, the restriction of thermal conduction across magnetic field lines enables the coexistence of hot and cool plasmas in cluster cores.