Case A: Rapidly rotating magnetized NS

GRMHD evolution in full 3D

This case is the most stable of all our models.

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 purely poloidal magnetic field. After approximately $\sim 9 t_A$ although the star preserves broadly its shape, the magnetic field instabilities start to develop. In addition the initial uniform rotation is replaced in the core of the neutron star with differential rotation that at times becomes counterrotating.