Full 3D End-to-End Simulation of a Supernova
The goal of this proposal is to simulate the death of massive star end-to-end in 3D numerical simulations in order to determine the nucleosynthesis of that star. The simulation is subdivided in three distinct phases that each use their specialized simulation code. The simulation will start about 10 minutes before the iron core of the star collapses toward formation of a neutron star. This sets the initial structure, the spectrum of the velocity field and of the density perturbations that are key to model the instabilities in the subsequent phases in a consistent and realistic fashion. Second, the researchers will follow the collapse of the core and the early evolution of the proto-neutron star for three seconds (longer than any multi-group simulation before) to obtain converged explosion energies, outflows, and trajectories and sufficient information about the neutrino signal that triggers nucleosynthesis in the outer layers of the exploding star. Finally, they will simulate the explosion as it proceeds through the outer layers of the star, including the hydrodynamic instabilities and to decide which parts of the outer layers of the star fall onto the neutron star and what is ejected. The specific target of this study is a low-mass supernova with a comparatively low explosion energy that the researchers believe may have triggered the formation of the solar system.
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