Abstract
The behavior of the unbound neutrons in the inner crust of neutron stars is linked to various neutron-star characteristics such as glitches in the repetition rate of pulsars. This paper presents a novel calculation of low-density superfluid neutron matter using techniques and interactions previously applied to the study of finite nuclei. The starting point is a two-body interaction softened using renormalization-group techniques. The resulting interaction is used in a Hartree-Fock-Bogoliubov calculation that includes pairing. This provides a good starting point for the many-body perturbation expansion, and for including more sophisticated nuclear interactions in future work.
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