Composition of planets with an N-body-Monte-Carlo approach

With exoplanet spectroscopy and mass/radius relations we are obtaining more and more insight into the composition of extrasolar planets. Current data suggests a large diversity. A big question is: is this diversity due to different initial conditions of the circumstellar protoplanetary disks in which these planets are formed? Or is it because of the intrinsically chaotic nature of the formation of multi-planet systems? The goal of this project is to develop a new hybrid N-body-Monte-Carlo code that will be able to address questions such as these, and can follow the path that different constituents (such as silicates, metals and various ice species) follow from the initial dust phase to the final rocky and gaseous planets. The code will be very modular, so that it can be easily adaptable to different tasks. And we intend to make it publicly available, first within the SPP 1992 and later completely.