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A Pedagogical Review of the Vacuum Retarded Dipole Model of Pulsar Spin Down
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Pulsars are rapidly spinning highly magnetised neutron stars. Their spin period is observed to decrease with time. An early analytical model for this process was the vacuum retarded dipole (VRD) by Deutsch (1955). This model assumes an idealised star and it finds that the rotational energy is radiated away by the electromagnetic fields. This model has been superseded by more realistic numerical simulations that account for the non-vacuum like surroundings of the neutron star. However, the VRD still provides a reasonable approximation and is a useful limiting case that can provide some qualitative understanding. We provide detailed derivations of the spin down and related electromagnetic field equations of the VRD solution. We also correct typographical errors in the general field equations and boundary conditions used by Deutsch (1955).
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Measuring the electric dipole moment of the neutron using neutron star spin-down
The thesis derives a conditional 90% limit |d_n| < 4.42e-25 e cm from the spin-down budget of PSR J0437-4715 via an effective magnetic-quadrupole channel, the first astrophysical bound of this kind.
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