A Modified Pulsar Model Green Function Period Distribution

Extract

The downward accelerated e⁻ in the “unfavorable” zone, like that in the “favorable” one, will emit γ-photons, which in turn convert into e^± pairs in some places near the surface of stars. But what happens, which is different from that in the “favorable” zone, is that some γ-photons will travel through a long distance before their conversion. This makes it possible that some γ-photons arrive at the “diode” district in the “favorable” zone. The magnetic conversion of pairs is much easier to happen than that occured in the “favorable” zone, where the γ-photons are created by the primary e⁻ beam. The existence of dense e^± plasma near the surface of stars makes the E, vanish at places where such plasma is present.