Derives exact expressions for pressure and chemical potentials in the neutron star inner crust within Hartree-Fock and extended Thomas-Fermi frameworks, applicable to catalyzed and accreted matter, with examples using BSk24.
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Three-dimensional band-structure calculations in the BCS approximation within HFB theory find that only 8% of free neutrons participate in superflow at baryon density 0.03 fm^{-3}, independent of the pairing gap.
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.
citing papers explorer
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Pressure and chemical potentials in the inner crust of a cold neutron star within Hartree-Fock and extended Thomas-Fermi methods
Derives exact expressions for pressure and chemical potentials in the neutron star inner crust within Hartree-Fock and extended Thomas-Fermi frameworks, applicable to catalyzed and accreted matter, with examples using BSk24.
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Superfluid fraction in the crystalline crust of a neutron star: role of BCS pairing
Three-dimensional band-structure calculations in the BCS approximation within HFB theory find that only 8% of free neutrons participate in superflow at baryon density 0.03 fm^{-3}, independent of the pairing gap.
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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.