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

摘要: NGC1275, the central galaxy in Perseus cluster, is host of gigantic hot bipolar bubbles inflated by AGN jets observed radio as A. It presents a spectacular $H{\alpha}$-emitting nebulosity surrounding with loops and filaments gas extending to over 50 kpc. The origin still unknown, but probably correlates mechanism responsible for giant buoyant bubbles. We present 2.5 3-dimensional MHD simulations region cluster which turbulent energy, possibly triggered star formation supernovae (SNe) explosions introduced. reveal that turbulence injected massive stars could be nearly isotropic distribution drag magnetic fields upward indicated recent observations. Weak shell-like shock fronts propagating into ICM velocities 100-500 km/s are found, also resembling outflow momentum slows infall intracluster medium, thus limiting further starburst activity NGC1275. As subsonic most simulated volume, kinetic energy not efficiently converted heat additional heating required suppress cooling flow at core cluster. Simulations combining can reproduce temperature radial profile around While main source, crucial isotropize distribution.