  We perform simulations to study the effects of active galactic nuclei (AGNs)
radiation and wind feedback on the properties of slowly rotating accretion flow
at parsec scale. We find that when only radiative feedback is considered,
outflows can be produced by the radiation pressure due to Thomson scattering.
The mass flux of outflow is comparable to that of inflow. Although strong
outflow is present, the luminosity of AGN can be easily super-Eddington. When
wind feedback is also taken into account, the mass flux of outflow does not
change much. Consequently, the luminosity of the central AGN can still be
super-Eddington. However, observations show that the luminosity of most AGNs is
sub-Eddington. Some other mechanisms are needed to reduce the AGNs luminosity.
Although the mass outflow rate does not change much by wind feedback, other
properties of outflow (density, temperature, velocity and kinetic power) can be
significantly changed by wind feedback. In the presence of wind feedback, the
density of outflow becomes significantly lower, temperature of outflow becomes
significantly higher, velocity of outflow is increased by one order of
magnitude, the kinetic power of outflow is increased by a factor of $40-100$.
