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Following the optical imaging of the exoplanet candidate Fomalhaut b (Fom b),we present a numerical model of how Fomalhaut's debris disk is gravitationallyshaped by an interior planet. The model is simple, adaptable to other debrisdisks, and can be extended to accommodate multiple planets. If Fom b is thedominant perturber of the belt, then to produce the observed disk morphology itmust have a mass < 3 Jupiter masses. If the belt and planet orbits areapsidally aligned, our model predicts a planet mass of 0.5 Jupiter masses. Theinner edge of the debris disk at 133 AU lies at the periphery of Fom b'schaotic zone, and the mean disk eccentricity of 0.11 is secularly forced by theplanet, supporting predictions made prior to the discovery of Fom b. However,previous mass constraints based on disk morphology rely on severaloversimplifications. We explain why our constraint is more reliable. It isbased on a global model of the disk that is not restricted to the planet'schaotic zone boundary. Moreover, we screen disk parent bodies for dynamicalstability over the system age of 100 Myr, and model them separately from theirdust grain progeny; the latter's orbits are strongly affected by radiationpressure and their lifetimes are limited to 0.1 Myr by destructive grain-graincollisions. The single planet model predicts that planet and disk orbits beapsidally aligned. Fom b's nominal space velocity does not bear this out, butthe astrometric uncertainties may be large. If the apsidal misalignment isreal, our upper mass limit of 3 Jupiter masses still holds. The belt containsat least 3 Earth masses of solids that are grinding down to dust. Such a largemass in solids is consistent with Fom b having formed in situ.

Fomalhaut's Debris Disk and Planet: Constraining the Mass of Fomalhaut b From Disk Morphology