Overview
This project uses 2D and 3D numerical simulations of stellar interiors to study convection, internal waves, and their interplay in solar-like and massive stars. The primary tool is the MUSIC code, a fully compressible, time-implicit solver for the (magneto-)hydrodynamic equations.
Scientific goals
- Characterize the excitation and amplitude of internal gravity waves and acoustic modes by turbulent convection.
- Understand how rotation modifies wave propagation and mode amplitudes in stellar interiors.
- Connect simulation outputs directly to asteroseismic observables to validate stellar models.
- Contribute to the development and maintenance of the MUSIC code.
Related publications
- de Vries, N., Le Saux, A., Baraffe, I., Guillet, T., Townsend, R. H. D., Leclerc, A., and Morison, A. (2026). Revealing Mixed Modes in Compressible Hydrodynamical Simulations of Red Giant Stars, ApJ, 1005, 154
- Le Saux, A., Bessila, L. and Mathis, S. (2026). Impact of rotation on the amplitude of acoustic modes in solar-like stars: Insights from hydrodynamical simulations, MNRAS, 549, 1
- Le Saux, A., Leclerc, A., Laibe, G., Delplace, P. and Venaille, A. (2025). A Core-sensitive Mixed f/g-mode of the Sun Predicted by Wave Topology and Hydrodynamical Simulation , ApJL, 987, L12