  Outflows play a pivotal role in star formation as one of its most visible
markers and a means of transporting mass, momentum, and angular momentum from
the infalling gas into the surrounding molecular cloud. Their wide reach (at
least thousands of au) is a contrast to typical disk sizes ($\sim 10-100$ au).
We employ high-resolution three-dimensional nested-grid nonideal
magnetohydrodynamic (MHD) simulations to study outflow properties in the Class
0 phase. We find that no disk wind is driven from the extended centrifugal disk
that has weak magnetic coupling. The low-velocity winds emerge instead from the
infalling magnetic pseudodisk. Much of the disk actually experiences an infall
of matter rather than outflowing gas. Some of the pseudodisk wind (PD-wind)
moves inward to regions above the disk and either falls onto the disk or
proceeds upward. The upward flow gives the impression of a disk wind above a
certain height even if the gas is originally emerging from the pseudodisk. The
PD-wind has the strongest flow coming from a disk interaction zone that lies
just outside the disk and is an interface between the inwardly advected
magnetic field of the pseudodisk and the outwardly diffusing magnetic field of
the disk. The low-velocity wind exhibits the features of a flow driven by the
magnetic pressure gradient force in some regions and those of a
magnetocentrifugal wind in other regions. We interpret the structure and
dynamics of the outflow zone in terms of the basic physics of gravity, angular
momentum, magnetic fields, and nonideal MHD.
