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We study the growth of black holes (BHs) in galaxies using three-dimensionalsmoothed particle hydrodynamic simulations with new implementations of themomentum mechanical feedback, and restriction of accreted elements to thosethat are gravitationally bound to the BH. We also include the feedback from theX-ray radiation emitted by the BH, which heats the surrounding gas in the hostgalaxies, and adds radial momentum to the fluid. We perform simulations ofisolated galaxies and merging galaxies and test various feedback models withthe new treatment of the Bondi radius criterion. We find that overall the BHgrowth is similar to what has been obtained by earlier workers using theSpringel, Di Matteo, & Hernquist algorithms. However, the outflowing windvelocities and mechanical energy emitted by winds are considerably higher (v_w~ 1000-3000 km/s) compared to the standard thermal feedback model (v_w ~ 50-100km/s). While the thermal feedback model emits only 0.1 % of BH released energyin winds, the momentum feedback model emits more than 30 % of the total energyreleased by the BH in winds. In the momentum feedback model, the degree offluctuation in both radiant and wind output is considerably larger than in thestandard treatments. We check that the new model of the BH mass accretionagrees with analytic results for the standard Bondi problem.

Radiative and Momentum Based Mechanical AGN Feedback in a 3-Dimensional Galaxy Evolution Code