Neutron Star Matter Superfluidity: from BCS to QMC

The equation of state and pairing gap of neutron matter at low densities are important to the structure and cooling of neutron stars, and potentially to the surface properties of neutron-rich nuclei. Over the last few decades, several many-body schemes have been devised in an attempt to calculate the pairing gap for this system. In this talk, I will show that using only the S=L=0 component of a realistic nucleon-nucleon interaction is sufficient up to significant densities. I will present Bardeen-Cooper-Schrieffer (BCS) calculations as well as Quantum Monte Carlo (QMC) results for the equation of state and pairing gap for neutron matter.