Formation of giant planets from large planetesimals

Recent numerical simulations show that large, Ceres sized planetesimals might form very rapidly in protoplanetary disks. In this work we want to explore the consequences of these findings on the formation of (extrasolar) giant planets.

Jupiter Mass and accretion rate in classical in-situ formation scenario. Once without and once with artificially switched off planetesimal accretion rate at 1.5 Myr evolution, decreasing core luminosity and therefore increasing gas accretion.

Precise task

An core accretion formation model is adapted to study the case of such massive planetesimals as building blocks for (giant) planets and the consequences are compared with the population of known extrasolar planets. A possible extension of the project would be to explicitly follow the trajectories of the massive planetesimals in the nebula under the influence of solar gravity, gravity from the protoplanet and nebular gas, using them as super-particles to calculate directly the growth rate of the protoplanet.