Magnetized neutron stars with superconducting cores: Effect of entrainment

Abstract

We construct equilibrium configurations of magnetized, two-fluid neutron stars using an iterative numerical method. Working in Newtonian framework we assume that the neutron star has two regions: the core, which is modelled as a two-component fluid consisting of type-II superconducting protons and superfluid neutrons, and the crust, a region composed of normal matter. Taking a new step towards more complete equilibrium models, we include the effect of entrainment, which implies that a magnetic force acts on neutrons, too. We consider purely poloidal field cases and present improvements to an earlier numerical scheme for solving equilibrium equations, by introducing new convergence criteria. We find that entrainment results in qualitative differences in the structure of field lines along the magnetic axis.

10 pages, 4 figures, 2 tables

References in corpus (4)

• Neutron conduction in the inner crust of a neutron star in the framework of the band theory of solids
• The contrasting magnetic fields of superconducting pulsars and magnetars
• Two-fluid models of superfluid neutron star cores
• The inside-out view on neutron star magnetospheres

Cited by in corpus (7)

• Evidence for an abundant old population of Galactic ultra long period magnetars and implications for fast radio bursts
• On the magnetic field evolution timescale in superconducting neutron star cores
• Coherent magneto-elastic oscillations in superfluid magnetars
• The freedom to choose neutron star magnetic field equilibria
• The impact of superconductivity and the Hall effect in models of magnetized neutron stars
• Application of superconducting-superfluid magnetohydrodynamics to nuclear "pasta" in neutron stars
• Methods for relativistic self-gravitating fluids: From binary neutron stars to black hole-disks and magnetized rotating neutron stars