Except for a brief period after their birth, neutron stars are expected to contain various superfluid and
superconducting phases [363, 116
, 29
, 367
]. In this section, after a brief discussion of superconductivity
and its possible occurrence in neutron star crusts, we will review our current theoretical understanding of
the static and dynamic properties of neutron superfluid in the inner crust of neutron stars. For a general
introduction and a recent overview on superfluidity and superconductivity, see, for instance, the book by
Annett [22].
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