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In many ways, the HR 8799 planetary system strongly resembles our own. Itfeatures four giant planets and two debris belts, analogues to the Asteroid andEdgeworth-Kuiper belts. Here, we present the results of dynamical simulationsof HR 8799's inner debris belt, to study its structure and collisionalenvironment.  Our results suggest that HR 8799's inner belt is highly structured, with gapsbetween regions of dynamical stability. The belt is likely constrained betweensharp inner and outer edges, located at ~6 and ~8 au, respectively. Its inneredge coincides with a broad gap cleared by the 4:1 mean-motion resonance withHR 8799e.  Within the belt, planetesimals are undergoing a process of collisionalattrition like that observed in the Asteroid belt. However, whilst the meancollision velocity in the Asteroid belt exceeds 5 km/s, the majority ofcollisions within HR 8799's inner belt occur with velocities of order 1.2 km/s,or less. Despite this, they remain sufficiently energetic to be destructive -giving a source for the warm dust detected in the system.  Interior to the inner belt, test particles remain dynamically unstirred,aside from narrow bands excited by distant high-order resonances with HR 8799e.This lack of stirring is consistent with earlier thermal modelling of HR 8799'sinfrared excess, which predicted little dust inside 6 au. The inner system issufficiently stable and unstirred that the formation of telluric planets isfeasible, although such planets would doubtless be subject to a punitive impactregime, given the intense collisional grinding required in the inner belt togenerate the observed infrared excess.

Modelling the Inner Debris Disc of HR 8799