ABSTRACT
The standard model of a radio pulsar is pictured schematically in Fig. 1. A neutron star of radius R 106 cm has a magnetic field with polar field strength typically 1012G, frozen into the solid crust which rotates with angular velocity α ≡ 2π/P1. The rotation period P1 inferred from the recurring radio emission is typically close to 1s, but can be smaller, e.g., ≈ 1/30 s for the pulsar in the Crab Nebula. There is also the class of “millisecond pulsars,” thought to have fields closer to 108 G.
