Thermal Conduction and Cooling of Young Neutrons Stars. Evolution of Pulsar Magnetic Fields.
Abstract
Thermal conductivity of matter in different regions of a neutron star is calculated. In the crust the electron conductivity is limited by electronphonon collisions and is calculated in the WiedermannFranz approximation by using the standard solution of the coupled electronphonon Boltzmann equation in the relaxation time approximation. In the core with normal nucleons, the electron and neutron conductivities are calculated in the theory of Fermi liquids. Stability and evolution of dipole and strong toroidal internal magnetic fields are considered. The problem of stability of the dipole magnetic field of a newly born pulsar is presented terms of a two dimensional model solution of the nonlinear equations of magnetohydrodynamics. A variational principle to test the linear stability of the solution is formulated.
 Publication:

Ph.D. Thesis
 Pub Date:
 May 1979
 Bibcode:
 1979PhDT.........6R
 Keywords:

 Physics: Astronomy and Astrophysics;
 Neutron Stars;
 Pulsars;
 Stellar Evolution;
 Stellar Magnetic Fields;
 Magnetohydrodynamics;
 Mathematical Models;
 Stellar Models;
 Stellar Temperature;
 Thermal Conductivity;
 Two Dimensional Models;
 Astrophysics