HLRB Project h0072
Simulating Supernova Shock Propagation Through Stellar Envelopes In 3D
Max-Planck-Institut fuer Astrophysik
Proposing Institution
Max-Planck-Institut fuer Astrophysik
Project Manager
PD Dr. Ewald Müller
Karl-Schwarzschildstr. 1
85741 Garching
Abstract
Longterm simulations of Core Collapse Supernovae (SNe) ranging from seconds to hours after core bounce are of interest in astrophysics, since they connect the modeling of the explosion mechanism with observables. They are able to predict the spatial distribution of the heavy elements, which are produced during the star's life and in the supernova explosion itself, and which can be observed in the supernova remnant. This holds in particular for the distribution of radioactive Ni-56, which powers the supernova light curve.The most sophisticated simulations of that type so far (Kifonidis et. al, 2003, 2006) where carried out under the assumption of axial symmetry. However, one may expect significant differences between these 2D simulations and full 3D models, since all flow features in 2D axisymmetric simulations are of toroidal character. The suppression of the third spatial dimension most certainly influences the growth of flow instabilities and the amount of compositional mixing, e.g. of Ni-56, in the ejecta as found in 2D simulations.Goal of the project is to simulate the propagation of the supernova shock wave through the stellar envelope in three spatial dimensions, and to investigate the amount of mixing of chemical elements due to Rayleigh-Taylor and Richtmyer-Meshkov instabilities triggered by the passage of the shock wave.
