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

Detection of Small Kuiper Belt Objects by Stellar Occultations