  Knowledge of the Kuiper Belt is currently limited to those objects that can
be detected directly. Objects with diameters less than $\sim$10km reflect too
little light to be detected. These smaller bodies could contain most of the
mass in the Kuiper Belt while the abundance of these bodies may constrain the
distribution of mass. The overall size distribution of bodies within the Kuiper
Belt can also be inferred from the relative abundances of sub-km and larger
bodies. Stellar occultations are already used to study dark objects in the
Solar System, such as asteroids or planetary rings. Occultation by a KBO of a
size comparable to, or larger than, that of the Fresnel Scale will result in
Fresnel diffraction. Detection of diffraction effects requires fast
multiple-star photometry, which will be conducted in July 2007 using the
Orthogonal Parallel Transfer Imaging Camera (OPTIC) mounted on the University
of Hawaii 2.2m telescope on Mauna Kea. This paper details how knowledge of the
mass and structure of the outer Solar System may be obtained through the
detection of serendipitous stellar occultations.
