  We perform 3D stratified shearing-box MHD simulations on the gas dynamics of
protoplanetary disks threaded by net vertical magnetic field Bz. All three
non-ideal MHD effects, Ohmic resistivity, the Hall effect and ambipolar
diffusion are included in a self-consistent manner based on equilibrium
chemistry. We focus on regions toward outer disk radii, from 5-60AU, where
Ohmic resistivity tends to become negligible, ambipolar diffusion dominates
over an extended region across disk height, and the Hall effect largely
controls the dynamics near the disk midplane. We find that around R=5AU, the
system launches a laminar/weakly turbulent magnetocentrifugal wind when the net
vertical field Bz is not too weak, as expected. Moreover, the wind is able to
achieve and maintain a configuration with reflection symmetry at disk midplane.
The case with anti-aligned field polarity (Omega. Bz<0) is more susceptible to
the MRI when Bz drops, leading to an outflow oscillating in radial directions
and very inefficient angular momentum transport. At the outer disk around and
beyond R=30AU, the system shows vigorous MRI turbulence in the surface layer
due to far-UV ionization, which efficiently drives disk accretion. The Hall
effect affects the stability of the midplane region to the MRI, leading to
strong/weak Maxwell stress for aligned/anti-aligned field polarities.
Nevertheless, the midplane region is only very weakly turbulent. Overall, the
basic picture is analogous to the conventional layered accretion scenario
applied to the outer disk. In addition, we find that the vertical magnetic flux
is strongly concentrated into thin, azimuthally extended shells in most of our
simulations beyond 15AU. This is a generic phenomenon unrelated to the Hall
effect, and leads to enhanced zonal flow. Observational and theoretical
implications, as well as future prospects are briefly discussed.
