  Motivated by prior remote observations of a transition from striated solar
coronal structures to more isotropic ``flocculated'' fluctuations, we propose
that the dynamics of the inner solar wind just outside the Alfv\'en critical
zone, and in the vicinity of the first $\beta=1$ surface, is powered by the
relative velocities of adjacent coronal magnetic flux tubes. We suggest that
large amplitude flow contrasts are magnetically constrained at lower altitude
but shear-driven dynamics are triggered as such constraints are released above
the Alfv\'en critical zone, as suggested by global magnetohydrodynamic (MHD)
simulations that include self-consistent turbulence transport. We argue that
this dynamical evolution accounts for features observed by {\it Parker Solar
Probe} ({\it PSP}) near initial perihelia, including magnetic ``switchbacks'',
and large transverse velocities that are partially corotational and saturate
near the local Alfv\'en speed. Large-scale magnetic increments are more
longitudinal than latitudinal, a state unlikely to originate in or below the
lower corona. We attribute this to preferentially longitudinal velocity shear
from varying degrees of corotation. Supporting evidence includes comparison
with a high Mach number three-dimensional compressible MHD simulation of
nonlinear shear-driven turbulence, reproducing several observed diagnostics,
including characteristic distributions of fluctuations that are qualitatively
similar to {\it PSP} observations near the first perihelion. The concurrence of
evidence from remote sensing observations, {\it in situ} measurements, and both
global and local simulations supports the idea that the dynamics just above the
Alfv\'en critical zone boost low-frequency plasma turbulence to the level
routinely observed throughout the explored solar system.
