Forced precession of neutron stars
Abstract
The dynamics of a neutron star subject to an external torque is analyzed by considering it as a twocomponent body. The solid crust and the interior plasma coupled to it by a magnetic field constitute one component, with the interior neutron superfluid being the other component. A viscous stress and an inertial stress acting between the crust and the interior are expressed in equations of motion solved by a perturbation method in the limit that the spin rate changes during the precession period; the viscous stress causes a secular evolution of the spin angular momentum and precession amplitude even if relativistic effects dominate the precession rate. The strength of the inertial couple is critical in determining the decay rate of forced precessional motion; the behavior of a forceprecessed superfluid can be found by laboratory experiments that are proposed.
 Publication:

The Astrophysical Journal
 Pub Date:
 November 1980
 DOI:
 10.1086/158464
 Bibcode:
 1980ApJ...242..306D
 Keywords:

 Neutron Stars;
 Precession;
 Stellar Motions;
 Superfluidity;
 Equations Of Motion;
 Spin Dynamics;
 Stellar Models;
 Stellar Rotation;
 Stellar Structure;
 Stress Analysis;
 Torque;
 Astrophysics