Multifluid simulations of embedded planets

Planets form in discs of gas and dust around young stars. While the gas component has by far the most mass and is therefore dynamically more important, it is the dust component that is easier to observe. Ideally one would like to identify planets from their signature in the dust, but this is not straightforward since the dust interacts with the gas through a drag force. What is needed are simulations of embedded planets that take into account both gas and dust, so that we can make the link between the structures in the dust that are observed and the planet that is causing these structures. In this project the student will perform multifluid calculations of embedded planets and link these to recent observations.