Goldstone modes in the neutron star core

Abstract

We formulate a theory of Goldstone bosons and their interactions in the superfluid and superconducting phase of dense nucleonic matter at densities of relevance to the neutron star core. For typical neutron star temperatures in the range T = 10^6 to 10^9 K, the Goldstone mode associated with rotational symmetry, called angulons, couple weakly to each other and to electrons. Consequently, these modes have anomalously large mean free paths and can contribute to both diffusive and ballistic transport of heat and momentum. In contrast, the two Goldstone bosons associated with density oscillations of the neutron and electron + proton fluids, called superfluid phonons, mix and couple strongly to electrons. They have shorter mean free paths, and their contribution to transport is negligible. Long-wavelength superfluid phonons and angulons can play a role in neutron star seismology, and lead to interesting phenomenology as angulons couple to magnetic fields and have anisotropic dispersion relations.

4 pages, 1 figure

References in corpus (8)

• General coordinate invariance and conformal invariance in nonrelativistic physics: Unitary Fermi gas
• Superfluid Heat Conduction and the Cooling of Magnetized Neutron Stars
• Electron-muon heat conduction in neutron star cores via the exchange of transverse plasmons
• Superfluid dynamics in neutron star crusts
• A low energy theory for superfluid and solid matter and its application to the neutron star crust
• The low lying modes of triplet-condensed neutron matter and their effective theory
• Shear viscosity due to phonons in superfluid neutron stars
• Elementary excitations in homogeneous superfluid neutron star matter: Role of the proton component

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• Symmetry Realization via a Dynamical Inverse Higgs Mechanism
• Massive and massless modes of the triplet phase of neutron matter
• Microscopic description of axisymmetric vortices in ${}^3{P}_2$ superfluids
• Domain walls in neutron ${}^3{P}_2$ superfluids in neutron stars
• Thermal conductivity due to phonons in the core of superfluid neutron stars
• Quark matter contribution to the heat capacity of magnetized neutron stars
• Critical endpoint and universality class of neutron ${}^3{P}_2$ superfluids in neutron stars
• Dispersion and decay of collective modes in neutron star cores
• Two-component superfluid hydrodynamics of neutron star cores
• Coexistence phase of ${}^1{S}_0$ and ${}^3{P}_2$ superfluids in neutron stars
• Topological defects at the boundary of neutron ${}^3{P}_2$ superfluids in neutron stars
• Spin-polarized phases of ${}^3{P}_2$ superfluids in neutron stars
• Electron-neutron scattering and transport properties of neutron stars
• Core structures of vortices in Ginzburg-Landau theory for neutron ${}^3{P}_2$ superfluids
• Proximity effects of vortices in neutron ${}^3{P}_2$ superfluids in neutron stars: Vortex core transitions and covalent bonding of vortex molecules
• Superfluid liquid crystals: pasta phases in neutron star crusts
• Transport properties of superfluid phonons in neutron stars
• Strongly interacting matter in extreme magnetic fields
• Symmetry classification of uniform states in spin-2 Bose-Einstein condensates and neutron ${}^3{P}_2$ superfluids
• Emergent chirality and superfluidity of parity-doubled baryons in neutron stars