Mr Antonio Graziano Pili
Physical and observational properties of neutron stars (NSs) are deeply influenced by the morphology of their magnetic field. Therefore an accurate description of both the interior and exterior stellar magnetic field is necessary to improve our understanding of NS phenomenology. I will present a comprehensive numerical study of GR equilibria of magnetised NSs, taking into account different magnetic field geometries (including twisted magnetospheres) and the combined role of rotation, showing how the two determine the overall deformation of the star. I will also address the gauge freedom in choosing different prescriptions for the surface charge and current, their physical implications, and how they modify the exterior electromagnetic properties.