Gapless superfluidity in neutron stars: Normal-fluid fraction

Abstract

Our previous investigation within the time-dependent nuclear energy-density functional theory showed that the nuclear superfluids contained inside cold neutron stars could become gapless under certain circumstances. The absence of a gap in the energy spectrum of quasiparticle excitations leads to a specific heat that is comparable to that in the normal phase in sharp contrast with the exponential suppression in the BCS phase of type ${}^1{S}_0$ pairing. Here, we further study gapless superfluidity within the same microscopic framework focusing on hydrodynamic properties. In particular, we calculate the mass fraction transported by the normal fluid of quasiparticle excitations, and we find that it can be finite even at zero temperature. We derive an approximate analytical formula for arbitrary neutron-proton superfluid mixtures. We also present numerical results for neutron stars. Our study suggests that the dynamics of neutron stars may be much more complicated than previously thought. The realization of gapless superfluidity in neutron stars and its implications are discussed.

28 pages, 8 figures

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Cited by in corpus (6)

• Gapless neutron superfluidity can explain the late time cooling of transiently accreting neutron stars
• Superfluid fraction in the crystalline crust of a neutron star: role of BCS pairing
• Time-dependent nuclear energy-density functional theory toolkit for neutron star crust: Dynamics of a nucleus in a neutron superfluid
• Gapless neutron superfluidity in the crust of the accreting neutron stars KS 1731-260 and MXB 1659-29
• Superfluid fraction in the crystalline crust of a neutron star: role of quantum zero-point motion of ions
• Thermodynamic stability of superflows in General Relativity and Newtonian gravity