Using simple geometrical arguments , we paint an overview of the variety of resonant structures a single planet with moderate eccentricity ( e \lesssim 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 , \epsilon Eridani and Fomalhaut .