  This work presents a detailed analysis of the overall flow structure and
unique features of the inner region of the tilted disk simulations described in
Fragile et al. (2007). The primary new feature identified in the main disk body
is a latitude-dependent radial epicyclic motion driven by pressure gradients
attributable to the gravitomagnetic warping of the disk. The induced motion of
the gas is coherent over the scale of the entire disk and is fast enough that
it could be observable in features such as relativistic iron lines. The
eccentricity of the associated fluid element trajectories increases with
decreasing radius, leading to a crowding of orbit trajectories near their
apocenters. This results in a local density enhancement akin to a compression.
These compressions are sufficiently strong to produce a pair of weak shocks in
the vicinity of the black hole. These shocks are roughly aligned with the
line-of-nodes between the black-hole symmetry plane and disk midplane, with one
shock above the line-of-nodes on one side of the black hole and the other below
on the opposite side. These shocks enhance angular momentum transport and
energy dissipation near the hole, forcing some material to plunge toward the
black hole from well outside the innermost stable circular orbit. A new,
extended simulation, which was evolved for more than a full disk precession
period, allows us to confirm that these shocks and the previously identified
``plunging streams'' precess with the disk in such a way as to remain aligned
relative to the line-of-nodes, as expected based on our physical understanding
of these phenomena. Such a precessing structure would likely present a strong
quasi-periodic signal.
