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Pulsars are rapidly spinning highly magnetised neutron stars. Their spinperiod is observed to decrease with time. An early analytical model for thisprocess was the vacuum retarded dipole (VRD) by Deutsch (1955). This modelassumes an idealised star and it finds that the rotational energy is radiatedaway by the electromagnetic fields. This model has been superseded by morerealistic numerical simulations that account for the non-vacuum likesurroundings of the neutron star. However, the VRD still provides a reasonableapproximation and is a useful limiting case that can provide some qualitativeunderstanding. We provide detailed derivations of the spin down and relatedelectromagnetic field equations of the VRD solution. We also correcttypographical errors in the general field equations and boundary conditionsused by Deutsch (1955).

A Pedagogical Review of the Vacuum Retarded Dipole Model of Pulsar Spin Down