Abstract: Neutron stars are extreme astrophysical objects in which matter ranges from iron-like densities at the surface to several times nuclear saturation in the core. Their layered structure—outer crust, inner crust, and core—is governed by the nuclear matter equation of state (EoS), while superfluidity arising from neutron and proton pairing affects cooling, rotational stability, and sudden spin-up events (glitches). This thesis investigates the superfluid dynamics of the outer core, composed of a neutronic superfluid and a protonic superconductor in beta equilibrium with an electron gas, using a hydrodynamic model in which the two fluids are coupled through both dynamic entrainment and the Skyrme SLy4 effective N–N interaction. Analysis of the resulting equations of motion reveals dynamical instabilities, with results potentially linked to observable astrophysical phenomena. Also, the effects of single proton vortices on the neutron superfluid under realistic rotation and magnetic field conditions are examined.  

Tribunal:

President: Dr. José Antonio Pons Botella

Secretary: Dr. Maria Moreno Cardoner

Vocal: Dr. Jordi José Pont

Suplents:

Dr. Clara Dehman

Dr. Arnau Ríos Huguet

Directors: Dr. Francisco Javier Viñas Gausí and Dr. Mario Centelles Aixalà

Tutor: Dr. Joan Soto Riera