  The origin of narrow line region (NLR) outflows remains unknown. In this
paper, we explore the scenario in which these outflows are circumnuclear clouds
driven by energetic accretion disk winds. We choose the well-studied nearby
Seyfert galaxy NGC 4151 as an example. By performing 3D hydrodynamical
simulations, we are able to reproduce the radial distributions of velocity,
mass outflow rate and kinetic luminosity of NLR outflows in the inner 100 pc
deduced from spatial resolved spectroscopic observations. The demanded kinetic
luminosity of disk winds is about two orders of magnitude higher than that
inferred from the NLR outflows, but is close to the ultrafast outflows (UFO)
detected in X-ray spectrum and a few times lower than the bolometric luminosity
of the Seyfert. Our simulations imply that the scenario is viable for NGC 4151.
The existence of the underlying disk winds can be confirmed by their impacts on
higher density ISM, e.g., shock excitation signs, and the pressure in NLR.
