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We investigate the general interaction between an eccentric planet and acoplanar debris disc of the same mass, using analytical theory and n-bodysimulations. Such an interaction could result from a planet-planet scatteringor merging event. We show that when the planet mass is comparable to that ofthe disc, the former is often circularised with little change to its semimajoraxis. The secular effect of such a planet can cause debris to apsidallyanti-align with the planet's orbit (the opposite of what may be naivelyexpected), leading to the counter-intuitive result that a low-mass planet mayclear a larger region of debris than a higher-mass body would. The interactiongenerally results in a double-ringed debris disc, which is comparable to thoseobserved in HD 107146 and HD 92945. As an example we apply our results to HD107146, and show that the disc's morphology and surface brightness profile canbe well-reproduced if the disc is interacting with an eccentric planet ofcomparable mass (~10-100 Earth masses). This hypothetical planet had apre-interaction semimajor axis of 30 or 40 au (similar to its present-dayvalue) and an eccentricity of 0.4 or 0.5 (which would since have reduced to~0.1). Thus the planet (if it exists) presently resides near the inner edge ofthe disc, rather than between the two debris peaks as may otherwise beexpected. Finally we show that disc self-gravity can be important in this massregime and, whilst it would not affect these results significantly, it shouldbe considered when probing the interaction between a debris disc and a planet.

Double-ringed debris discs could be the work of eccentric planets: explaining the strange morphology of HD 107146