Student Posters Repository

Due to high computational costs, stellar evolution modeling is typically done in the 1D approximation where spherical symmetry is assumed. However, some hydrodynamical phenomena are intrinsically multidimensional, e.g. mixing of chemical elements due to convection. In common 1D evolution codes, these are parametrized as diffusion processes with certain diffusion coefficients. The exact value of these coefficients typically suffer from high uncertainties. To improve this, we conduct 2D and 3D hydro-simulations of shells inside a star by solving the compressible Euler-equations using a finite-Volume approach. From these simulations, we derive quantities like the amount of mixing or how far convective plumes penetrate into adjacent convectively stable regions. These results can help to improve the current treatment in 1D stellar evolution codes. Here, we show results for rotationally induced shear instabilities and convection in a He-burning shell obtained with our "Seven League Hydro (SLH)" code.