Скачать или смотреть Angular momentum transport in massive stars during late burning - Dr. Lucy McNeill (Monash)

Rotation plays a decisive role in supernova explosions and their remnants. In particular, theories to explain the observed neutron star spin and magnetic field populations rely sensitively on the fine details of angular momentum transport during stellar evolution.In this talk we present results from two 3D hydrodynamics simulations of massive stars during oxygen burning (~10 minutes before core-collapse), in order to address some of these uncertainties. In the rapidly rotating supernova progenitor, we find that similar to the Sun, convective shells rotate around 30 percent faster at the equator, i.e. slower at larger cylindrical radius R. This is in contradiction with previous 2D simulations, assumptions made in 1D stellar evolution codes and widely used analytic theory. If angular momentum is pushed out of a convective core before supernova, it may be more difficult to form e.g. millisecond magnetars, which require rapid core rotation.In the initially non-rotating progenitor, we explore the idea of stochastic angular momentum transport where internal gravity waves are excited by vigorous convection, leading to a net spin up in the neutron star progenitor core. We find that this mechanism is orders of magnitude less efficient at spinning up the stellar core than previous 1D studies, and that it is unlikely to reproduce the observed neutron star birth spin population.