  We present subarcsecond-resolution mid-infrared images of the debris disk
surrounding the 230 Myr- old A star Zeta Lep. Our data obtained with T-ReCS at
Gemini South show the source to be unresolved at 10.4 microns but clearly
extended at 18.3 microns. Quadratic subtraction of the PSF profile from that of
Zeta Lep implies a characteristic radius for the dust disk of 3 AU, which is
comparable in size to our solar system's asteroid belt. Simple models suggest
that the 18 micron flux is well approximated by two contiguous annuli of
mid-infrared-emitting dust from 2-4 and 4-8 AU with a 3:1 flux ratio for the
annuli, respectively. We consider two scenarios for the collisions that must be
resupplying the dust population: (1) continuous "steady state" grinding of
planetesimals, and (2) an isolated cataclysmic collision. We determine that
radiation pressure and subsequent collisions are the dominant determinants of
the disk morphology in either case, and that Poynting-Robertson drag is
comparatively insignificant.
