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Most of our understanding of the location and nature of the beamed emission comes from the pulse profiles, which are available over the whole electromagnetic spectrum. The radio profiles are the most detailed, with observations of polarisation, width and components.
The radio and high-energy profiles show that the emitting regions are concentrated in gaps in the magnetosphere located over the magnetic poles and near the velocity of light cylinder. The radio sources of most normal pulsars are distributed unevenly over the polar cap and are highly concentrated, broadband and variable. Their excitation may move laterally, causing drifting in sub-pulse timing. Other radio emitters are located close to the gamma-ray emitters in the outer magnetosphere. Almost all radio pulses are highly polarised; the sweep of position angle in the radio pulses is related to the magnetic field at the location of the emitters.
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