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Heating from active galactic nuclei (AGN) is thought to stabilize cool-coreclusters, limiting star formation and cooling flows. We employ radiativemagneto-hydrodynamic (MHD) simulations to model light AGN jet feedback withdifferent accretion modes (Bondi-Hoyle-Lyttleton and cold accretion) in anidealised Perseus-like cluster. Independent of the probed accretion model,accretion efficiency, jet density and resolution, the cluster self-regulateswith central entropies and cooling times consistent with observed cool-coreclusters in this non-cosmological setting. We find that increased jetefficiencies lead to more intermittent jet powers and enhanced star formationrates. Our fiducial low-density jets can easily be deflected by orbiting coldgaseous filaments, which redistributes angular momentum and leads to moreextended cold gas distributions and isotropic bubble distributions. Incomparison to our fiducial low momentum-density jets, high momentum-densityjets heat less efficiently and enable the formation of a persistent cold-gasdisc perpendicular to the jets that is centrally confined. Cavity luminositiesmeasured from our simulations generally reflect the cooling luminosities of theintracluster medium (ICM) and correspond to averaged jet powers that arerelatively insensitive to short periods of low-luminosity jet injection. Coldgas structures in our MHD simulations with low momentum-density jets generallyshow a variety of morphologies ranging from discy to very extended filamentarystructures. In particular, magnetic fields are crucial to inhibit the formationof unrealistically massive cold gas discs by redistributing angular momentumbetween the hot and cold phases and by fostering the formation of elongatedcold filaments that are supported by magnetic pressure.

Self-regulated AGN feedback of light jets in cool-core galaxy clusters