Speaker
Description
The most energetic core-collapse supernovae are thought to arise from rapidly rotating, magnetised progenitors. However, the three-dimensional pre-collapse structure of their angular momentum and magnetic fields remains poorly constrained, limiting the realism of magnetorotational core-collapse simulations.
In this talk, I will present two novel progenitor models for magneto-rotational core-collapse supernovae. We evolved two stellar models through their final minutes pre-collapse in full 3D MHD, including both the core and outer layers, allowing us to characterise the stable 3D magnetic field topology and strength throughout the star. We identify strong amplification of the magnetic field in convective regions, alongside a tendency for small-scale fields to develop there. As a result, regions that are magnetically disconnected in the original one-dimensional stellar-evolution description become magnetically linked in the multidimensional models.
We also identify behaviour in the 3D models that diverges from 1D prescriptions, notably in angular momentum transport and convective flows. With this in mind I will further discuss how our models can be used to feed back into 1D modelling to yield more physically consistent pre-supernova models.