  We present a new method of analysis for determining the surface geometry of
five protoplanetary disks observed with near-infrared imaging polarimetry using
Subaru-HiCIAO. Using as inputs the observed distribution of polarized intensity
(PI), disk inclination, assumed properties for dust scattering, and other
reasonable approximations, we calculate a differential equation to derive the
surface geometry. This equation is numerically integrated along the distance
from the star at a given position angle. We show that, using these
approximations, the local maxima in the PI distribution of spiral arms (SAO
206462, MWC 758) and rings (2MASS J16042165-2130284, PDS 70) are associated
with local concave-up structures on the disk surface. We also show that the
observed presence of an inner gap in scattered light still allows the
possibility of a disk surface that is parallel to the light path from the star,
or a disk that is shadowed by structures in the inner radii. Our analysis for
rings does not show the presence of a vertical inner wall as often assumed in
studies of disks with an inner gap. Finally, we summarize the implications of
spiral and ring structures as potential signatures of ongoing planet formation.
