Formation enthalpy of monovacancies in neutron-star matter

Analysis of the monovacancy formation enthalpy in the solid phase of neutron-star matter has shown that neither the continuous neutron superfluid nor changes in nuclear properties are of significance. Its calculation is a well-defined problem involving Coulomb and electron energies. The thermal equilibrium concentrations of monovacancies obtained are too small to give superfluid-neutron-vortex pinning of the strength required to explain the sequence of large glitches observed in the Vela pulsar, but the monovacancy-vortex interaction, if attractive, could contribute to the recovery of the spin-down rate observed after a glitch.