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Structures observed in debris disks may be caused by gravitationalinteraction with planetary or stellar companions. These perturbed disks areoften thought to indicate the presence of planets and offer insights into theproperties of both the disk and the perturbing planets. Gaps in debris disksmay indicate a planet physically present within the gap, but such gaps can alsooccur away from the planet's orbit at mean-motion resonances (MMRs), and thisis the focus of our interest here. We extend our study of planet-diskinteraction through MMRs, presented in an earlier paper, to systems in whichthe perturbing planet has moderate orbital eccentricity, a common occurrence inexoplanetary systems. In particular, a new result is that the 3:1 MMR becomesdistinct at higher eccentricity, while its effects are absent for circularplanetary orbits. We also only consider gravitational interaction with aplanetary body of at least 1 Jupiter mass. Our earlier work shows that even a 1Earth mass planet can theoretically open an MMR gap; however, given the narrowgap that can be opened by a low-mass planet, its observability would bequestionable. We find that the widths, locations, and shapes of two prominentstructures, the 2:1 and 3:1 MMRs, could be used to determine the mass,semimajor axis, and eccentricity of the planetary perturber and present analgorithm for doing so. These MMR structures can be used to narrow the positionand even determine the planetary properties (such as mass) of any inferred butas-yet-unseen planets within a debris disk. We also briefly discuss theimplications of eccentric disks on brightness asymmetries and their dependenceon the wavelengths with which these disks are observed.

astrophysical journal/the astrophysical journal

Detection and Characterization of Extrasolar Planets through Mean-Motion  Resonances. II. The Effect of the Planet's Orbital Eccentricity on Debris  Disk Structures