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The star Fomalhaut hosts a narrow, eccentric debris disc, plus a highlyeccentric companion Fomalhaut b. It is often argued that Fomalhaut b cannothave significant mass, otherwise it would quickly perturb the disc. We showthat material in internal mean-motion resonances with a massive, coplanarFomalhaut b would actually be long-term stable, and occupy orbits similar tothe observed debris. Furthermore, millimetre dust released in collisionsbetween resonant bodies could reproduce the width, shape and orientation of theobserved disc. We first re-examine the possible orbits of Fomalhaut b, assumingthat it moves under gravity alone. If Fomalhaut b orbits close to the discmidplane then its orbit crosses the disc, and the two are apsidally aligned.This alignment may hint at an ongoing dynamical interaction. Using theobservationally allowed orbits, we then model the interaction between a massiveFomalhaut b and debris. Whilst most debris is unstable in such an extremeconfiguration, we identify several resonant populations that remain stable forthe stellar lifetime, despite crossing the orbit of Fomalhaut b. This debrisoccupies low-eccentricity orbits similar to the observed debris ring. Theseresonant bodies would have a clumpy distribution, but dust released incollisions between them would form a narrow, relatively smooth ring similar toobservations. We show that if Fomalhaut b has a mass between those of Earth andJupiter then, far from removing the observed debris, it could actually besculpting it through resonant interactions.

Fomalhaut b could be massive and sculpting the narrow, eccentric debris disc, if in mean-motion resonance with it