Speaker
Description
Pebble accretion is widely considered a key, and probably necessary, ingredient for rapid planet formation. However, most studies still rely on simplified gas prescriptions or assume a single particle size. In this work, we revisit pebble accretion using a multifluid hydrodynamical model that evolves the gas and multiple pebble species self-consistently. This allows us to move beyond static background discs and directly study how the planet’s perturbation of the gas affects the accretion of solids.
In this talk, I will show how a polydisperse pebble distribution reshapes not only the total accretion onto the planet, but also the structure of the surrounding disc. What happens once the planet approaches pebble isolation mass? How does the disc respond as the planet grows beyond it? By following the coupled evolution of gas and multiple dust species, we gain new insight into how planet growth and disc restructuring proceed together.
| Talk category | NOVA Network 2 |
|---|---|
| PhD relevance | 3rd |
