3D Nuclear-Hydrodynamics Models of the Interiors of Stars Using the Magnus Supercomputer

Dr Simon Campbell1

1School of Physics and Astronomy at Monash University

Whilst 1D stellar models have been very successful in reproducing many features of stars, some of their success is based on parameterisation and calibration, as opposed to good physical models or understanding.

This is especially true for phases in which the structure is dominated by turbulent convection. In an attempt to improve this situation we are making large-scale 3D simulations of stellar interior convection zones, with a view to understand the key physics that is needed to improve 1D models (which are still required). In this talk I will discuss the simulation of two different stars, performed on the Pawsey supercomputer Magnus. I will also present movie animations of the simulations, some of which were produced using the Zeus visualisation cluster at Pawsey.


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