Description
Planets form in discs of gas and dust around young stars. Within these discs, micron-sized dust particles need to clump together and grow 14 orders of magnitude to form planets. Collisions between dust particles can lead to growth or fragmentation, changing the dust size distribution. The state of the art in coupling dust coagulation to hydrodynamics are 2D simulations with ∼100 particle size bins. Many problems in planet formation, such as the streaming instability, are 3D in nature. Furthermore, they require extremely high resolution in size space. Coupling 3D hydrodynamics with coagulation requires going beyond the current state of the art. We will do this by harnessing the power of machine learning to obtain an efficient and accurate subgrid model for dust collisions. This will for the first time allow for a full treatment of the dust component, including coagulation, in simulations of the polydisperse streaming instability and pebble accretion.
| Talk category | data science (contact d.huppenkothen@uva.nl) |
|---|---|
| Preference for a talk or poster | Poster |
