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In many ways, the HR8799 system resembles our Solar system more closely thanany other discovered to date - albeit on a larger, younger, and more dramaticscale - featuring four giant planets and two debris belts. The first belt liesbeyond the orbit of the outer planet, and mirrors our Solar system'sEdgeworth-Kuiper belt. The second belt lies interior to the orbit of the innerplanet, HR8799e, and is analogous to our Asteroid Belt. With such a similararchitecture, the system is a valuable laboratory for examining exoplanetdynamics, and the interaction between debris disks and planets.  In recent years, HR8799's outer disk has been relatively well characterised,primarily using the Herschel Space Observatory. In contrast, the inner disk,too close to HR8799 to be spatially resolved by Herschel, remains poorlyunderstood. This leaves significant questions over both the location of theplanetesimals responsible for producing the observed dust, and the physicalproperties of those grains.  We have performed extensive simulations of HR8799's inner, unresolved debrisbelt, using UNSW Australia's supercomputing facility, Katana. Here, we presentthe results of integrations following the evolution of a belt of dynamicallyhot debris interior to the orbit of HR8799e, for a period of 60 Myr, using aninitial population of 500,000 massless test particles. These simulations haveenable the characterisation of the extent and structure of the inner belt,revealing that its outer edge must lie interior to the 3:1 mean-motionresonance with HR8799, at approximately 7.5au, and highlighting the presence offine structure analogous to the Solar system's Kirkwood gaps. In the future,out results will allow us to calculate a first estimate of the small-bodyimpact rate and water delivery prospects for any potential terrestrialplanet(s) that might lurk, undetected, in the inner system.

Towards a dynamics-based estimate of the extent of HR 8799's unresolved warm debris belt