Evolution of the surface magnetic field of rotating proto-neutron stars

Understand

We study the evolution of the field on the surface of proto-neutron stars in the immediate aftermath of stellar core collapse by analyzing the results of self-consistent, axisymmetric simulations of the cores of rapidly rotating high-mass stars.

• To this end, we compare the field topology and the angular spectra of the poloidal and toroidal field components over a time of about one seconds for cores.
• Both components are characterized by a complex geometry with high power at intermediate angular scales.
• The structure is mostly the result of the accretion of magnetic flux embedded in the matter falling through the turbulent post-shock layer onto the PNS.