We perform high-resolution ( 15-30 pc ) adaptive mesh simulations to study the impact of momentum-driven AGN feedback in cool-core clusters , focusing in this paper on the formation of cold clumps .
The feedback is jet-driven with an energy determined by the amount of cold gas within 500 pc of the SMBH .
When the intra-cluster medium ( ICM ) in the core of the cluster becomes marginally stable to radiative cooling , with the thermal instability to the free-fall timescale ratio t _ { TI } / t _ { ff } < 3 - 10 , cold clumps of gas start to form along the propagation direction of the AGN jets .
By tracing the particles in the simulations , we find that these cold clumps originate from low entropy ( but still hot ) gas that is accelerated by the jet to outward radial velocities of a few hundred km/s .
This gas is out of hydrostatic equilibrium and so can cool .
The clumps then grow larger as they decelerate and fall towards the center of the cluster , eventually being accreted onto the super-massive black hole .
The general morphology , spatial distribution and estimated H { \alpha } morphology of the clumps are in reasonable agreement with observations , although we do not fully replicate the filamentary morphology of the clumps seen in the observations , probably due to missing physics .