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In Aristotelian Electrodynamics (AE), due to radiation over-damping, thevelocity rather than the acceleration of a charge is determined by the localelectromagnetic field. Treating electrons and positrons separately, AE seems togive a faithful description of the flow of charges in a pulsar magnetosphere.AE might allow to calculate the pulsar emission in full detail, at all energiesexcept the radio.  But AE is not a full theory -- the plasma production processes must be added.Here we show that the pulsar magnetosphere and the resulting emission aresensitive to the plasma production rate near the light cylinder. In strongpulsars (high production rate, due to photon-photon collisions), the number offield lines closing beyond the light cylinder decreases. This reduces both thepulsar efficiency (the ratio of the pulsed bolometric luminosity to thespin-down power) and the characteristic photon energy, in overall agreementwith the Fermi data.  For weak pulsars (low production rate), our numerical implementation of AEworks stably and seems to be ready to calculate the lightcurves and spectra.But for strong pulsars, the code (included) needs improvement or betterunderstanding.

Aristotelian Electrodynamics solves the Pulsar: Lower Efficiency of Strong Pulsars