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In the canonical picture of pulsars, radio emission arises from a narrow conecentered on the star's magnetic axis but many basic details remain unclear. Weuse high-quality polarization data taken with the Parkes radio telescope toconstrain the geometry and emission heights of pulsars showing interpulseemission, and include the possibility that emission heights in the main andinterpulse may be different. We show that emission heights are low in thecentre of the beam, typically less than 3\% of the light cylinder radius. Theemission beams are under-filled in longitude, with an average profile widthonly 60% of the maximal beam width and there is a strong preference for thevisible emission to be located on the trailing part of the beam. We showsubstantial evidence that the emission heights are larger at the beam edgesthan in the beam centre. There is some indication that a fan-like emission beamexplains the data better than conal structures. Finally, there is a strongcorrelation between handedness of circular polarization in the main andinterpulse profiles which implies that the hand of circular polarization isdetermined by the hemisphere of the visible emission.

On the beam properties of radio pulsars with interpulse emission