A note on the ambipolar diffusion in superfluid neutron stars

Abstract

We address the problem of magnetic field dissipation in the neutron star cores, focusing on the role of neutron superfluidity. Contrary to the results in the literature, we show that in the finite-temperature superfluid matter composed of neutrons, protons, and electrons, magnetic field dissipates exclusively due to Ohmic losses and non-equilibrium beta-processes, and only an admixture of muons restores (to some extent) the role of particle relative motion for the field dissipation. The reason for this discrepancy is discussed.

6 pages, published in MNRAS

References in corpus (5)

• Temperature-dependent pulsations of superfluid neutron stars
• Magnetic Field Evolution in Neutron Stars: One-Dimensional Multi-Fluid Model
• The relevance of ambipolar diffusion for neutron star evolution
• Magnetic field evolution and equilibrium configurations in neutron star cores: the effect of ambipolar diffusion
• The freedom to choose neutron star magnetic field equilibria

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• Two-fluid simulations of the magnetic field evolution in neutron star cores in the weak-coupling regime
• On the weak magnetic field of millisecond pulsars: Does it decay before accretion?
• Magnetic-field evolution with large-scale velocity circulation in a neutron-star crust
• Evolution of magnetic deformation in neutron star crust
• Crucial role of neutron diffusion in the crust of accreting neutron stars
• Diffusion in superfluid Fermi mixtures: General formalism
• Magnetic coupling through flux branching of adjacent type-I and -II superconductors in a neutron star