Superfluid Heat Conduction and the Cooling of Magnetized Neutron Stars

Abstract

We report on a new mechanism for heat conduction in the neutron star crust. We find that collective modes of superfluid neutron matter, called superfluid phonons (sPhs), can influence heat conduction in magnetized neutron stars. They can dominate the heat conduction transverse to magnetic field when the magnetic field $B \gsim 10^{13}$ G. At density $\rho \simeq 10^{12}-10^{14}$ g/cm${}^3$ the conductivity due to sPhs is significantly larger than that due to lattice phonons and is comparable to electron conductivity when temperature $\simeq 10^8$ K. This new mode of heat conduction can limit the surface anisotropy in highly magnetized neutron stars. Cooling curves of magnetized neutron stars with and without superfluid heat conduction could show observationally discernible differences.

4 pages, 3 figures

References in corpus (7)

• General coordinate invariance and conformal invariance in nonrelativistic physics: Unitary Fermi gas
• The Magnificent Seven: Magnetic fields and surface temperature distributions
• Dense Matter in Compact Stars: Theoretical Developments and Observational Constraints
• Strongly paired fermions: Cold atoms and neutron matter
• 2D Cooling of Magnetized Neutron Stars
• Electron thermal conductivity owing to collisions between degenerate electrons
• Thermal conductivity of ions in a neutron star envelope

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