Magnetohydrodynamics of neutron star interiors.
Abstract
Magnetohydrodynamic equations for the charged particles in the fluid interior of a neutron star are derived from the LandauBoltzmann kinetic equations. It is assumed that the protons are normal and the neutrons are superfluid. The dissipative processes associated with the weak interactions are shown to be negligible except in very hot neutron stars; we neglect them here. Among the topics discussed are: the influence of the neutronproton nuclear force (Fermi liquid corrections) on the magnetohydrodynamics; the effects of the magnetic field on the pressure, viscosity, and heat conductivity tensors; the plasma equation of state; and the form of the generalized Ohm's law.
 Publication:

The Astrophysical Journal
 Pub Date:
 February 1979
 DOI:
 10.1086/156808
 Bibcode:
 1979ApJ...227..995E
 Keywords:

 Hydrodynamic Equations;
 Magnetohydrodynamics;
 Neutron Stars;
 Plasma Dynamics;
 Stellar Interiors;
 Stellar Structure;
 Conductive Heat Transfer;
 Equations Of State;
 Fermi Liquids;
 NucleonNucleon Interactions;
 Ohms Law;
 Protons;
 Pulsars;
 Stellar Magnetic Fields;
 Superfluidity;
 Astrophysics;
 Magnetohydrodynamics:Neutron Stars;
 Neutron Stars:Interiors