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We examine the detailed physics of the feedback mechanism by relativistic AGNjets interacting with a two-phase fractal interstellar medium in the kpc-scalecore of galaxies using 29 3D grid-based hydrodynamical simulations. Thefeedback efficiency, as measured by the amount of cloud-dispersal generated bythe jet-ISM interactions, is sensitive to the maximum size of clouds in thefractal cloud distribution but not to their volume filling factor. Feedbackceases to be efficient for Eddington ratios P_jet/L_edd<10^-4, although systemswith large cloud complexes ~50 pc require jets of Eddington ratio in excess of10^-2 to disperse the clouds appreciably. Based on measurements of the bubbleexpansion rates in our simulations we argue that sub-grid AGN prescriptionsresulting in negative feedback in cosmological simulations without amulti-phase treatment of the ISM are good approximations if the volume fillingfactor of warm phase material is less than 0.1 and the cloud complexes aresmaller than ~25 pc. We find that the acceleration of the dense embedded cloudsis provided by the ram pressure of the high velocity flow through the porouschannels of the warm phase, flow that has fully entrained the shocked hot-phasegas it has swept up, and is additionally mass-loaded by ablated cloud material.This mechanism transfers 10% to 40% of the jet energy to the cold and warm gas,accelerating it within 10 to 100 Myr to velocities that match those observed ina range of high and low redshift radio galaxies hosting powerful radio jets.

Driving Outflows with Relativistic Jets and the Dependence of AGN Feedback Efficiency on ISM Inhomogeneity