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The neutron superfluid permeating the inner crust of mature neutron stars isexpected to play a key role in various astrophysical phenomena like pulsarglitches. Despite the absence of viscous drag, the neutron superfluid can stillbe coupled to the solid crust due to non-dissipative entrainment effects.Entrainment challenges the interpretation of pulsar glitches and suggests thata revision of the interpretation of other observed neutron-star phenomena mightbe necessary.

How "free" are free neutrons in neutron-star crusts and what does it imply for pulsar glitches ?