A. Y. Wagner, G. V. Bicknell, M. Umemura
We examine the detailed physics of the feedback mechanism by relativistic AGN jets interacting with a two-phase fractal interstellar medium (ISM). The (negative) feedback efficiency, as measured by the amount of cloud-dispersal generated by the jet-ISM interactions, is sensitive to the maximum size of clouds in the fractal cloud distribution; for a given filling factor and density, distributions of smaller clouds lead to higher outflow velocities. Feedback ceases to be efficient for Eddington ratios P_jet/L_edd <~ 10^-4, although systems with large cloud complexes >~ 50 pc require jets of Eddington ratio in excess of 10^-2 to disperse the clouds appreciably. Compared to the ISM density and maximum cloud size, the feedback efficiency depends weakly on volume filling factor. Based on measurements of the bubble expansion rates in our simulations we argue that sub-grid AGN prescriptions resulting in negative feedback in cosmological simulations without a multi-phase treatment of the ISM are good approximations if the volume filling factor of warm phase material is less than 0.1 and the cloud complexes are smaller than ~25 pc. We find that the acceleration of the dense embedded clouds is provided by the ram pressure (rather than the thermal pressure) of the high velocity flow through the porous channels of the warm phase, flow that has fully entrained the shocked hot-phase gas it has swept up, and is additionally mass-loaded by ablated cloud material. This mechanism, reminiscent of a two-stage feedback scenario proposed by Hopkins & Elvis (2010), transfers 10% to 40% of the jet energy to the cold and warm gas, accelerating it to several 100 to several 1000 km s^-1 within a few 10 to 100 Myr. Our predicted velocities match those observed in a range of high and low redshift radio galaxies hosting powerful radio jets.
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http://arxiv.org/abs/1205.0542
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