Pulsar near fields.
Abstract
Maxwell's equations and the equation of motion E = v x B are used to derive an equation which when solved will give the fields B, E, J and the charge density rho around a pulsar. The equation derived includes the effect of moderate currents along the Blines, 'moderate' being defined as small enough not to change the equation of motion or disrupt the deviation. To handle the time problem which arises in the oblique rotator model, Fourier analysis and complex variables are used. This allows the derivation to be made entirely in the inertial frame, thus eliminating the need for a transform from the rotating frame of the star. The equation derived is used to calculate the near fields around a neutron star for the case of a dipole magnetic field on the surface of the star and zero current along the Blines.
 Publication:

The Astrophysical Journal
 Pub Date:
 October 1974
 DOI:
 10.1086/153151
 Bibcode:
 1974ApJ...193..225P
 Keywords:

 Equations Of Motion;
 Maxwell Equation;
 Neutron Stars;
 Pulsars;
 Stellar Magnetic Fields;
 Stellar Rotation;
 Charge Distribution;
 Laplace Equation;
 Magnetic Dipoles;
 Magnetospheres;
 Stellar Atmospheres;
 Astrophysics