Turbulent structures in discs

Protoplanetary discs are the birthplace of planetary systems that form around nascent stars. These discs are now observed with an exquisite resolution that allows us to probe the kinematics of the gas during planet formation.

From a theoretical standpoint, however, it is not yet clear which process may drive turbulence in those objects, nor what would be the observable signature of these mechanisms since most of our knowledge comes from either local box models and/or 2D axisymmetric simulations.

This project addresses this question with global full 3D simulations performed with the exascale-ready code IDEFIX, and able to capture all of the scales involved in turbulence driving.