Structure in the ε Eridani Dusty Disk Caused by Mean Motion Resonances with a 0.3 Eccentricity Planet at Periastron

The morphology of the epsilon Eridani dust ring is reproduced by a numerical simulation of dust particles captured into the 5: 3 and 3: 2 exterior mean-motion resonances with a 0. 3 eccentricity 10^-4 solar mass planet at periastron at a semi-major axis of 40 AU. The morphology will differ when the planet is at aphelion, in about 140 years. Moderate eccentricity planets in outer extra-solar systems will cause observable variations in the morphology of associated dusty rings.