Speaker
Description
Core-collapse supernovae (CCSNe) are some of the brightest, most energetic events in the
universe. In order to model these phenomena accurately, we need to have a diverse range of physics such as neutrino transport and neutrino interactions, general-relativistic gravity, detailed equations of state (EoS) of dense matter, magnetohydrodynamic (MHD) and detailed progenitor models. When modelling these events, magnetic fields are usually only invoked along with rapid rotation to explain rare hypernova events. In this talk, I will present recent efforts to understand the role of magnetic fields in non-rotating and slowly rotating neutrino-driven CCSNe. I will describe our current understanding of how magnetic effects can aid the neutrino-driven mechanism and affect the formation of the compact object. Finally, I will present some open problems that need to be addressed.