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We present 2D hydrodynamical simulations for the evolution of early-typegalaxies containing central massive black holes (MBHs), starting at age 2 Gyr.The code contains accurate and physically consistent radiative and mechanicalAGN wind feedback, with parsec-scale central resolution. Mass input comes fromstellar evolution; energy input includes Type Ia and II supernova and stellarheating; star-formation is included. Realistic, axisymmetric dynamical modelsfor the galaxies are built solving the Jeans' equations. The lowest mass models(Mstar = 8 10^{10}Msun) develop global outflows sustained by SNIa's heating,ending with a significantly lower amount of hot gas and new stars. In moremassive models, nuclear outbursts last to the present epoch, with large andfrequent fluctuations in nuclear emission and from the gas (Lx). Each burstlast ~ 10^{7.5} yr, during which (for r < 2-3 kpc) cold, inflowing, and hot,outflowing gas phases coexist. The Lx-T relation for the gas matches that oflocal galaxies. AGN activity causes positive feedback for star formation.Roughly half of the total mass loss is recycled into new stars (DeltaMstar),just ~ 3% of it is accreted on the MBH, the remainder being ejected from thegalaxy. The ratio between the mass of gas expelled to that in to new stars, theload factor, is ~0.6. Rounder galaxies shapes lead to larger final MBH masses,DeltaMstar, and Lx. Almost all the time is spent at very low nuclearluminosities, yet one quarter of the total energy is emitted at an Eddingtonratio > 0.1. The duty-cycle of AGN activity approximates 4% (Abridged).

The Effect of the AGN Feedback on the Interstellar Medium of Early-Type Galaxies: 2D Hydrodynamical Simulations of the Low-Rotation Case