  Planets embedded within debris disks gravitationally perturb nearby dust and
can create clumpy, azimuthally asymmetric circumstellar ring structures that
rotate in lock with the planet. The Earth creates one such structure in the
solar zodiacal dust cloud. In an edge-on system, the dust "clumps" periodically
pass in front of the star as the planet orbits, occulting and
forward-scattering starlight. In this paper, we predict the shape and magnitude
of the corresponding transit signal. To do so, we model the dust distributions
of collisional, steady-state exozodiacal clouds perturbed by planetary
companions. We examine disks with dusty ring structures formed by the planet's
resonant trapping of in-spiraling dust for a range of planet masses and
semi-major axes, dust properties, and disk masses. We synthesize edge-on images
of these models and calculate the transit signatures of the resonant ring
structures. The transit light curves created by dusty resonant ring structures
typically exhibit two broad transit minima that lead and trail the planetary
transit. We find that Jupiter-mass planets embedded within disks hundreds of
times denser than our zodiacal cloud can create resonant ring structures with
transit depths up to $\sim10^{-4}$, possibly detectable with \emph{Kepler}.
Resonant rings produced by planets more or less massive than Jupiter produce
smaller transit depths. Observations of these transit signals may provide upper
limits on the degree of asymmetry in exozodiacal clouds.
