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Fig. B.1


For each γ-ray emission model, the pulsar γ-ray (shaded surface) and radio (blue contours) emission patterns (phase plots) as a function of magnetic obliquity α, are shown. Each phase-plot panel gives the pulsar light curve as a function of the observer line-of-sight ζ for each α value stepped every 10° in the interval 0°<α< 90°. The γ-ray and radio phase plots have been obtained for a magnetic field strength of 108 Tesla and spin period of 30 ms for the PC and radio cases, and gap widths of 0.04 and 0.01 for the SG and OG/OPC cases, respectively.

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