Speaker
Description
I present general relativistic magnetohydrodynamic simulations of one potential r-process site associated with core collapse supernovae: the neutrino-driven wind. These outflows are launched from a hot proto-neutron star (PNS) remnant by neutrino-heating above their surfaces, within seconds after the collapse of a massive star. Previous work has shown that spherically symmetric winds from non-rotating PNSs fail to achieve the requisite conditions for a robust r-process. I explore for the first time the combined effects of rapid rotation and strong gravity of the PNS on the wind properties. I then explore the impact of a dynamically strong ordered magnetic field on the properties of non-rotating PNS winds. The wind in both cases is simulated in a controlled environment rather than as a part of a self-consistent global CCSNe simulation, to assess the viability of r-process nucleosynthesis as a function of PNS properties (neutrino energies/luminosities, rotation rate, magnetization). In future works I will combine the effects of rapid rotation and high magnetization in order to explain (according to the 'magnetar origin' model from Metzger et al. 2018) the observed fast, high-mass ejecta inferred from the 'blue KN' associated with GW170817.
