Magnetohydrodynamics of neutron star interiors

Abstract

Magnetohydrodynamic equations for the charged particles in the fluidinterior of a neutron star are derived from the Landau-Boltzmannkinetic equations. It is assumed that the protons are normal andthe neutrons are superfluid. The dissipative processes associatedwith the weak interactions are shown to be negligible except in veryhot neutron stars; we neglect them here. Among the topics discussedare: the influence of the neutron-proton nuclear force (Fermi liquidcorrections) on the magnetohydrodynamics; the effects of the magneticfield on the pressure, viscosity, and heat conductivity tensors;the plasma equation of state; and the form of the generalized Ohm'slaw.