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Abstract

This thesis presents multidimensional simulations of magnetohydrodynamic phenomena occurring in the interior of stars. Understanding these phenomena is essential for improving current theories of stellar evolution. The highly subsonic flow regimes found in the regions deep inside stars pose severe challenges to conventional methods of computational magnetohydrodynamics (MHD). Therefore, the first part of this thesis focuses on the development of a suitable numerical solver optimized for magnetized, low-Mach-number stellar flows. The proposed MHD solver is implemented in the Seven-League Hydro (SLH) code and then used to perform unprecedented simulations of turbulent dynamo action in an oxygen-burning shell of a massive star. It is demonstrated that strong, dynamically generated magnetic fields have a significant impact on the evolution of the convective shell and potentially influence the explosion mechanism of core-collapse supernovae. The new MHD capabilities of SLH pave the way for the next generation of stellar models and will aid in the study of various stellar MHD processes in flow regimes that were previously inaccessible.