The formation of planetary systems from gas and dust in protoplanetary disks involves an extraordinary range of scales and requires an understanding of physical processes that are inherently hard to observe astronomically or model under laboratory conditions. The group uses magnetohydrodynamic, multi-fluid and radiation hydrodynamic simulations to tackle these problems, together with analytic methods and machine learning approaches. This group is interested in finding new ways to constrain planet formation from observations of protoplanetary disks, studies of the exoplanet population, and detailed characterization of both exoplanets and Solar System bodies.
Gas giant planets are expected to accrete most of their mass via a circumplanetary disk. If the planet is unmagnetized…
The Astrophysical JournalDespite over three hundred years of effort, no solutions exist for predicting when a general planetary configuration will become unstable.…
PNASThe core accretion model of giant planet formation has been challenged by the discovery of recycling flows between the planetary…
Monthly Notices of the Royal Astronomical Society
