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Numerical simulations of active galactic nuclei (AGN) feedback in cool-coregalaxy clusters have successfully avoided classical cooling flows, but oftenproduce too much cold gas. We perform adaptive mesh simulations that includemomentum-driven AGN feedback, self-gravity, star formation and stellarfeedback, focusing on the interplay between cooling, AGN heating and starformation in an isolated cool-core cluster. Cold clumps triggered by AGN jetsand turbulence form filamentary structures tens of kpc long. This cold gasfeeds both star formation and the supermassive black hole (SMBH), triggering anAGN outburst that increases the entropy of the ICM and reduces its coolingrate. Within 1-2 Gyr, star formation completely consumes the cold gas, leadingto a brief shutoff of the AGN. The ICM quickly cools and redevelops multiphasegas, followed by another cycle of star formation/AGN outburst. Within 6.5 Gyr,we observe three such cycles. There is good agreement between our simulatedcluster and the observations of cool-core clusters. ICM cooling is dynamicallybalanced by AGN heating, and a cool-core appearance is preserved. The minimumcooling time to free-fall time ratio typically varies between a few and$\gtrsim 20$. The star formation rate (SFR) covers a wide range, from 0 to afew hundred $\rm M_{\odot}\, yr^{-1}$, with an average of $\sim 40 \,\rmM_{\odot}\, yr^{-1}$. The instantaneous SMBH accretion rate shows largevariations on short timescales, but the average value correlates well with theSFR. Simulations without stellar feedback or self-gravity produce qualitativelysimilar results, but a lower SMBH feedback efficiency (0.1% compared to 1%)results in too many stars.

Cooling, AGN Feedback and Star Formation in Simulated Cool-Core Galaxy Clusters