Abstract
The pulse γ‐ray spectrum from geminga has been obtained from COS‐B observation. We fit the pulsed spectrum by both the outergap and polar gap models and conclude that only the outergap model can explain the observed spectrum. We suggest that the pulsed γ‐rays from Geminga are emitted by the primary e± which are accelerated in the outer magnetospheric gap. If the observed X‐rays from Geminga result from the stellar heating by these primary electrons/positrons, we argue that this is a common phenomenon for all pulsars with an outergap. Its power is Lz=1.3×1031 P−2 B12 erg s−1.
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