Description
For many years now pebble accretion is recognized as perhaps the fastest growth mechanism in planet formation. Yet until now most studies have only considered a single pebble size (monodisperse) for calculating the growth rate of the planet. Pebble accretion works because specifically the pebble-sized solids are loosely coupled to the gaseous disk. The mechanics of these loosely coupled pebbles are largely dependent on their respective sizes, which is why a distribution of sizes (polydisperse) would be a much better representation of the reality of planet formation. This poster will showcase a multifluid approach to pebble accretion. Taking a fluid approach to pebble accretion has its drawbacks, but also comes with a lot of advantages. Most importantly we can now consider a non-static gaseous disk evolving simultaneously with the different solids, which is especially handy in the later stages of formation. At these stages the planet can grow sufficiently large to impact the gaseous disc, impacting the aerodynamics of the pebbles. Not only does this method showcase the accretion rate of a distribution of solid-sizes, we can also look at other mechanisms. For example disc-planet interactions like migration and the creation of Rossby-waves outside the planet.
| Talk category | NOVA Network 2 |
|---|---|
| Preference for a talk or poster | Poster |
