BSk31 calculations find Z=40 equilibrium throughout the inner crust density range with clusters impermeable to neutron superfluid, producing EOS similar to BSk24 but altered pairing fields.
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Role of neutron pairing with density-gradient dependence in the semi-microscopic treatment of the inner crust of neutron stars
BSk31 calculations find Z=40 equilibrium throughout the inner crust density range with clusters impermeable to neutron superfluid, producing EOS similar to BSk24 but altered pairing fields.