Speaker
Description
Neutrons and protons in neutron-star cores are widely expected to exist in superfluid and superconducting states, respectively. These phases profoundly modify the magnetic evolution through the macroscopic manifestation of the interaction between quantized neutron vortices and proton flux tubes. In the simplest limit, neglecting rotation and entrainment, axisymmetric MHD equilibria have been derived for cores composed of superfluid neutrons, superconducting protons, and electrons ($snspe$-matter). In these equilibria, the charged fluid is in hydrostatic balance under the combined action of pressure, gravity, and magnetic buoyancy and tension forces, while the magnetic field satisfies a Grad–Shafranov-like equation. We have developed a numerical framework based on Dedalus to investigate the long-term evolution of $snspe$-matter in both axisymmetry and three dimensions. In this talk, we will present our first results and discuss their implications for neutron-star magnetic evolution and phenomenology.