Abstract

Galaxy clusters form at the densest knots in the cosmic web and can contain thousands of individual galaxies. The space between the galaxies contains a very hot and dilute plasma, known as the intracluster medium, which can be observed with X-ray telescopes. Galaxy clusters continuously grow via accretion and mergers, which excite motions and turbulence in the intracluster medium. In this talk, I will first describe how analytic solutions for linear hydromagnetic waves can be used for testing cosmological magnetohydrodynamic (MHD) codes. I will then present PICO -Clusters, a new suite of cosmological zoom-in simulations of 25 massive (M_200,c > 10^14.9 M_sun) galaxy clusters. These simulations use the moving mesh code Arepo, the IllustrisTNG galaxy formation model and start with a weak seed magnetic field initialised at z=127, which is then evolved using comoving ideal magnetohydrodynamics. I will discuss the driving of turbulence and amplification of magnetic fields in the intracluster medium and the cluster mass dependence of the resulting amplitudes. Finally, I will present the current status of performing cosmological cluster simulations using Braginskii viscosity to model a weakly collisional intracluster medium.