  We study outflows driven by Active Galactic Nuclei (AGNs) using high-
resolution simulations of idealized z=2 isolated disk galaxies. Episodic
accretion events lead to outflows with velocities >1000 km/s and mass outflow
rates up to the star formation rate (several tens of Msun/yr). Outflowing winds
escape perpendicular to the disk with wide opening angles, and are typically
asymmetric (i.e. unipolar) because dense gas above or below the AGN in the
resolved disk inhibits outflow. Owing to rapid variability in the accretion
rates, outflowing gas may be detectable even when the AGN is effectively "off."
The highest velocity outflows are sometimes, but not always, concentrated
within 2-3 kpc of the galactic center during the peak accretion. With our
purely thermal AGN feedback model -- standard in previous literature -- the
outflowing material is mostly hot (10^6 K) and diffuse (nH<10^(-2) cm-3), but
includes a cold component entrained in the hot wind. Despite the powerful
bursts and high outflow rates, AGN feedback has little effect on the dense gas
in the galaxy disk. Thus AGN-driven outflows in our simulations do not cause
rapid quenching of star-formation, although they may remove significant amounts
of gas of long (>Gyr) timescales.
