It is now widely accepted that heating processes play a fundamental role in galaxy clusters , struggling in an intricate but fascinating ‘ dance ’ with its antagonist , radiative cooling .
Last generation observations , especially X-ray , are giving us tiny hints about the notes of this endless ballet .
Cavities , shocks , turbulence and wide absorption-lines indicate the central active nucleus is injecting huge amount of energy in the intracluster medium .
However , which is the real dominant engine of self-regulated heating ? One of the model we propose are massive subrelativistic outflows , probably generated by a wind disc or just the result of the entrainment on kpc scale by the fast radio jet .
Using a modified version of AMR code FLASH 3.2 , we explored several feedback mechanisms which self-regulate the mechanical power .
Two are the best schemes that answer our primary question , id est quenching cooling flow and at the same time preserving a cool core appearance for a long term evolution ( 7 Gyr ) : one more explosive ( with efficiencies \sim 5 \times 10 ^ { -3 } -10 ^ { -2 } ) , triggered by central cooled gas , and the other gentler , ignited by hot gas Bondi accretion ( with \epsilon = 0.1 ) .
These three-dimensional simulations show that the total energy injected is not the key aspect , but the results strongly depend on how energy is given to the ICM .
We follow the dynamics of best models ( temperature , density , SB maps and profiles ) and produce many observable predictions : buoyant bubbles , ripples , turbulence , iron abundance maps and hydrostatic equilibrium deviation .
We present a deep discussion of merits and flaws of all our models , with a critical eye towards observational concordance .