Pia Jakobus: Proto-Compact Star Convection and the Excitation Mechanism of the Core g-mode


Core-collapse supernovae (CCSNe), the explosion of massive stars, are among the several types of Gravitational Wave (GW) sources yet to be discovered by GW interferometers. In our general-relativistic neutrino hydrodynamics code CoCoNuT-FMT, we recently identified GWs of a core g-mode residing in the inner regions of the proto-compact star that is sensitive to the Equation of State at multiple times nuclear saturation density. The proto-compact star (PCS) convection zone plays the dominant role in the excitation mechanism of this mode. In this talk, I will present key properties of the PCS convection zone, and particularly focus on the question of why the core g-mode is absent in our 3D core-collapse supernova simulation whereas it is clearly visible in 2D. I will also discuss the validity of the mixing-length theory approximation within the PCS convection zone and briefly talk about a possible connection between passive scalars and the lepton-number emission self-sustained asymmetry.

The agenda of this meeting is empty