Electron-neutron scattering and transport properties of neutron stars

Abstract

We show that electrons can couple to the neutron excitations in neutron stars and find that this can limit their contribution to the transport properties of dense matter, especially the shear viscosity. The coupling between electrons and neutrons is induced by protons in the core, and by ions in the crust. We calculate the effective electron-neutron interaction for the kinematics of relevance to the scattering of degenerate electrons at high density. We use this interaction to calculate the electron thermal conductivity, electrical conductivity, and shear viscosity in the neutron star inner crust, and in the core where we consider both normal and superfluid phases of neutron-rich matter. In some cases, particularly when protons are superconducting and neutrons are in their normal phase, we find that electron-neutron scattering can be more important than the other scattering mechanisms considered previously.

arXiv comment18 pages, 8 figures

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• Transport coefficients of leptons in superconducting neutron star cores
• Tensor Fermi liquid parameters in nuclear matter from chiral effective field theory
• The Photon in Dense Nuclear Matter I: Random Phase Approximation
• Compressional modes in two-superfluid neutron stars with leptonic buoyancy
• Supplement to the theory of electron neutron scattering