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NGC1275, the central galaxy in the Perseus cluster, is the host of gigantichot bipolar bubbles inflated by AGN jets observed in the radio as Perseus A. Itpresents a spectacular $H{\alpha}$-emitting nebulosity surrounding NGC1275,with loops and filaments of gas extending to over 50 kpc. The origin of thefilaments is still unknown, but probably correlates with the mechanismresponsible for the giant buoyant bubbles. We present 2.5 and 3-dimensional MHDsimulations of the central region of the cluster in which turbulent energy,possibly triggered by star formation and supernovae (SNe) explosions isintroduced. The simulations reveal that the turbulence injected by massivestars could be responsible for the nearly isotropic distribution of filamentsand loops that drag magnetic fields upward as indicated by recent observations.Weak shell-like shock fronts propagating into the ICM with velocities of100-500 km/s are found, also resembling the observations. The isotropic outflowmomentum of the turbulence slows the infall of the intracluster medium, thuslimiting further starburst activity in NGC1275. As the turbulence is subsonicover most of the simulated volume, the turbulent kinetic energy is notefficiently converted into heat and additional heating is required to suppressthe cooling flow at the core of the cluster. Simulations combining the MHDturbulence with the AGN outflow can reproduce the temperature radial profileobserved around NGC1275. While the AGN mechanism is the main heating source,the supernovae are crucial to isotropize the energy distribution.

Turbulence and the formation of filaments, loops and shock fronts in NGC 1275 in the Perseus Galaxy Cluster