Dust coagulation and processing in an evolving disk

The aggregation, fragmentation and thermal processing of dust in protoplanetary disks is believed to be the first step on the long road from dust to planets. Models of this process in the literature have so far been applied mostly to the early solar system, and were mostly limited to a static 'minimum mass solar nebula' model of the protoplanetary disk. We present the initial results of a campaign to extend such a modeling to evolving protoplanetary disks, to improve the realism and detail of coagulation/fragmentation models compared to models in the literature so far and to link these models to observations