Credit: ESO/L. Calçada Credit: ESO/L. Calçada Data informed computational fluid dynamics for planet formation
About the project
Numerical fluid simulations are central to understanding the physics of protoplanetary disks, the cradle of planets. One of the major obstacles in planet formation models is the understanding of the dynamics of these disks surrounding young stars. The challenge is to consistently account for the multiple size scales involved in planet formation, which requires extremely high spatial resolutions. The solution lies, on the one hand, in increasing computational power through the use of exascale machines, and on the other hand, in reducing computational costs through innovative optimization methods. This project aims to reduce the numerical footprint of fluid simulations by using artificial intelligence tools to model the smallest scales, with the specific feature of taking into account the particular physics of this rotating, sheared turbulent flow (Keplerian rotation).
Meheut, H.; Gerosa, F. A. & Bec, J.
A unique solution to overcome the barriers to planetesimal formation at low dust-to-gas ratio
arXiv e-prints, 2025, arXiv:2508.20070
