Improving low-mass star models using 3D hydrodynamic simulations and asteroseismology

Stars are multi-dimensional (MultiD) objects involving complex phenomena (convection, rotation, magnetic fields, binary interactions). Although 3D hydrodynamic simulations cannot follow the entire evolution of stars, they can finally guide and constrain next-generation 1D stellar evolution models (convective boundaries can be resolved with resolutions >= 1024^3). This is crucially needed because the predictive power of current 1D models is crippled by uncertain 1D prescriptions of 3D phenomena, in particular for convective boundary mixing (CBM). Simultaneously, Asteroseismology can constrain CBM from the observational side. The goal of this PhD is to develop and implement new prescriptions for CBM in 1D stellar evolution models and test their predictions using asteroseismic observations.