Case B: Moderately rotating magnetized NS

GRMHD evolution in full 3D

This case corresponds to the one with the strongest toroidal magnetic field.

The following figures show the rest-mass density and magnetic field at four different instances, in side and top view. Green lines signify the poloidal + toroidal magnetic field, while white lines signify the poloidal magnetic field. After $\sim 10t_A$ the star exhibits turbulent motion on its surface, together with large density oscillations close to the surface and at $\pm 45^\circ$ from the equatorial plane. By that time the toroidal geometry of the magnetic field is lost and the kink instability is fully developed. In our simulations our stars preserve their general (hydrostatic) axisymmetry and we did not observe any significant nonaxisymmetric mode growth that can lead to appreciable gravitational wave emission.

As in case A the initial uniform rotation is replaced in the core of the neutron star with differential rotation that at times becomes counterrotating. After approximately $\sim 23 t_A$ the star becomes again uniformly rotating but with a smaller than the initial angular velocity.