Speaker
Description
Our understanding of nucleosynthesis and stellar evolution is limited by many uncertainties coming from the complex multi-dimensional processes in stellar interiors, such as the interplay between convection, nuclear burning, and magnetic fields. 3D hydrodynamic models allow for a more realistic treatment of stellar interiors, including explicit nuclear reaction networks and other multi-D processes, paving the way towards multi-D simulations of entire burning phases.
In this talk, I will present results from 3D simulations of advanced burning phases in massive stars, focusing on the time evolution of their chemical composition and the coupling between nuclear burning, convection, and magnetic fields. I will highlight the key differences with 1D models and discuss the implications of these findings for nucleosynthesis and the improvement of stellar evolution models.