Speaker
Description
Unlike X-ray pulsars, the isolated radio pulsars have a rather ‘quiet’ surface activity where the key forces are the strong surface gravity and the surface magnetic fields. The strong surface magnetic field leads to pair production and subsequent generation of the electron positron plasma and finally the radio beam and other emissions. The observed pulse patterns of the radio pulsars thus depend on the emission mechanism taking place at the polar caps that are highly guided by these surface magnetic field. The surface magnetic field on the other hand depends on the transport properties of a rapidly varying matter of the neutron star crust. We study the decay of the magnetic field of a neutron star assuming the magnetic field of the star is mostly located in the outer crust. We further study the effect of radial oscillation on the surface magnetic field and their relevance to observational features.
