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Circumstellar disks have long been regarded as windows into planetarysystems. The advent of high sensitivity, high resolution imaging in thesubmillimetre where both the solid and gas components of disks can be detectedopens up new possibilities for understanding the dynamical histories of thesesystems and therefore, a better ability to place our own solar system, whichhosts a highly evolved debris disk, in context. Comparisons of dust masses fromprotoplanetary and debris disks have revealed a stark downturn in mass inmillimetre-sized grains around a stellar age of 10 Myr, ostensibly in the"transition disk" phase, suggesting a period of rapid accretion of such grainsonto planetesimals. This rapid formation phase is in keeping with radionucleidestudies of Kuiper Belt Objects in the solar system. Importantly, this suggeststhat any thermal gradients in the gas of disks of this era will be "frozen in"to the planetesimals as they rapidly accrete from the solids and ices in theirvicinity. Measurements of radial gradients in thermal tracers such as DHO, DCNand other tracers can therefore provide insight into the nascent solar system'sabudances. In studies of dynamical evolution of the solar system, it is tacitlyassumed that such abundances can reveal the location of formation for bodiesnow found in the asteroid belt and Kuiper belt. Similarly, evidence of gasdetected from collisional evolution in young debris disks could potentiallyreveal how rapidly objects have dynamically evolved in those systems, most ofwhich will be significantly younger than the solar system.

Insights into planet formation from debris disks: I. The solar system as an archetype for planetesimal evolution