This thesis investigates the modeling of stellar magnetism in radiative layers driven by the Tayler-Spruit dynamo instability. The study was conducted using the Xshells code, building on results from a reference study performed with the PARODY code. An initial phase was dedicated to becoming familiar with Xshells and installing it on a high-performance computing (HPC) cluster. The first objective was to reproduce the results of the reference paper, which focuses on the radiative zone of stars. The subsequent objective was to modify the boundary conditions and introduce a volumetric forcing in order to investigate how the system saturates under more realistic conditions.