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The magnetic fields of neutron stars

 

 
  Typically Gauss for normal pulsars
  Consistent with flux conservation during stellar collapse
  Typically Gauss for millisecond pulsars
  Gravity dominates stellar structure
  B field dominates exterior

  Stellar surface is so small that observed emission is dominated by the magnetic field.
  The electromagnetic wave generated by the misaligned rotating dipole causes loss of rotational energy and accounts for the observed slowdown
  Only field lines inside light cylinder are closed
  Particles are constrained move along field lines