Gravitational wave signature of proto-neutron star convection: I. MHD numerical simulations

Understand

Gravitational waves provide a unique and powerful opportunity to constrain the dynamics in the interior of proto-neutron stars during core collapse supernovae.

• Convective motions play an important role in generating neutron stars magnetic fields, which could explain magnetar formation in the presence of fast rotation.
• We compute the gravitational wave emission from proto-neutron star convection and its associated dynamo, by post-processing three-dimensional MHD simulations of a model restricted to the convective zone in the anelastic approximation.
• We consider two different proto-neutron star structures representative of early times (with a convective layer) and late times (when the star is almost entirely convective).