  Using simple geometrical arguments, we paint an overview of the variety of
resonant structures a single planet with moderate eccentricity (e < ~0.6) can
create in a dynamically cold, optically thin dust disk. This overview may serve
as a key for interpreting images of perturbed debris disks and inferring the
dynamical properties of the planets responsible for the perturbations. We
compare the resonant geometries found in the solar system dust cloud with
observations of dust clouds around Vega and other stars and we discuss a new
model for the asymmetries in the Epsilon Eridani cloud.
