Description
One of the grand challenge of planet formation consist of performing 3D simulations of young dusty stellar systems that include grain growth and fragmentation self-consistently. Up to now, this task was considered as almost computationally inaccessible, due to the prohibitive computational cost associated to algorithms solving for the coagulation equation. I will show how connecting mathematical, physical, numerical and computational aspects of the coagulation equation led to the design of a novel scheme capable of addressing this challenge (Lombart and Laibe 2020).
