Three-dimensional band-structure calculations in the weak-coupling limit show that quantum ion motion mitigates superfluid suppression in bcc and fcc lattices but leaves it strongly reduced in the intermediate inner crust, dramatically raising ion effective masses.
Title resolution pending
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
verdicts
UNVERDICTED 4representative citing papers
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.
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
-
Superfluid fraction in the crystalline crust of a neutron star: role of quantum zero-point motion of ions
Three-dimensional band-structure calculations in the weak-coupling limit show that quantum ion motion mitigates superfluid suppression in bcc and fcc lattices but leaves it strongly reduced in the intermediate inner crust, dramatically raising ion effective masses.
-
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.
-
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.
-
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.