Self-consistent band calculation of slab phase in neutron-star crust

Abstract

Fully self-consistent band calculation has been performed for slab phase in neutron-star inner crust, using the BCPM energy density functional. Optimized slab structure is calculated at given baryon density either with the fixed proton ratio or with the beta-equilibrium condition. Numerical results indicate the band gap of in order of keV to tens of keV, and the mobility of dripped neutrons are enhanced by the Bragg scattering, which leads to the macroscopic effective mass, ${\bar{m}}_z^{\ast }/m_n=0.65\sim 0.75$ near the bottom of the inner crust in neutron stars. We also compare the results of the band calculation with those of the Thomas-Fermi approximation. The Thomas-Fermi approximation becomes invalid at low density with high proton ratio.

arXiv comment15 pages, 14 figures

References in corpus (18)

• Pulsar Constraints on Neutron Star Structure and Equation of State
• Pulsar glitches: The crust is not enough
• Neutron conduction in the inner crust of a neutron star in the framework of the band theory of solids
• Disordered nuclear pasta, magnetic field decay, and crust cooling in neutron stars
• Crustal Entrainment and Pulsar Glitches
• A highly resistive layer within the crust of X-ray pulsars limits their spin periods
• Unified equation of state for neutron stars on a microscopic basis
• Band structure effects for dripped neutrons in neutron star crust
• Accurate nuclear masses from a three parameter Kohn-Sham DFT approach (BCPM)
• Thermodynamic properties of nuclear "pasta" in neutron star crusts
• Superfluid Density of Neutrons in the Inner Crust of Neutron Stars: New Life for Pulsar Glitch Models
• On the validity of the Wigner-Seitz approximation in neutron star crust
• Entrainment coefficient and effective mass for conduction neutrons in neutron star crust: simple microscopic models
• Nuclear "pasta" structures in low-density nuclear matter and neutron star crust
• Entrainment coefficient and effective mass for conduction neutrons in neutron star crust: II Macroscopic treatment
• Role of the boundary conditions in the Wigner-Seitz approximation applied to the neutron star inner crust
• On the superfluid properties of the inner crust of neutron stars
• A new statistical method for the structure of the inner crust of neutron stars

Cited by in corpus (18)

• Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. II. Pasta phases in semi-classical approximation
• Time-dependent extension of the self-consistent band theory for neutron star matter: Anti-entrainment effects in the slab phase
• Coordinate-space solver for finite-temperature Hartree-Fock-Bogoliubov calculation using the shifted Krylov method
• Superfluid extension of the self-consistent time-dependent band theory for neutron star matter: Anti-entrainment versus superfluid effects in the slab phase
• Effects of pairing gap and band gap on superfluid density in the inner crust of neutron stars
• Entrainment effects in neutron-proton mixtures within the nuclear-energy density functional theory. II. Finite temperatures and arbitrary currents
• The proto-neutron star inner crust in the liquid phase
• Superfluid fraction in the slab phase of the inner crust of neutron stars
• Superfluid density in linear response theory : pulsar glitches from the inner crust of neutron stars
• Superfluid fraction in the crystalline crust of a neutron star: role of BCS pairing
• Superfluid fraction in the rod phase of the inner crust of neutron stars
• Superfluid density in disordered pasta phases in neutron star crusts
• Emergence of the geometric contribution to the superfluid density in the inner crust of neutron stars
• Dynamical scheme for computing the mass parameter of a system in a medium
• Superfluid fraction in the crystalline crust of a neutron star: role of quantum zero-point motion of ions
• Nuclear structure and reaction with quantum shape fluctuation
• Phase transitions in the inner crust of neutron stars within the superfluid band theory: Competition between ${}^1{\text{S}}_0$ pairing and spin polarization under finite temperature and magnetic field
• Fermi Operator Expansion for the Hartree-Fock-Bogoliubov Theory