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Successful phenomenological models of pulsar wind nebulae assume efficientdissipation of the Poynting flux of the magnetized electron-positron wind aswell as efficient acceleration of the pairs in the vicinity of the terminationshock, but how this is realized is not yet well understood. The present papersuggests that the corrugation of the termination shock, at the onset ofnon-linearity, may lead towards the desired phenomenology. Non-linearcorrugation of the termination shock would convert a fraction of order unity ofthe incoming ordered magnetic field into downstream turbulence, slowing downthe flow to sub-relativistic velocities. The dissipation of turbulence wouldfurther preheat the pair population on short length scales, close toequipartition with the magnetic field, thereby reducing the initial highmagnetization to values of order unity. Furthermore, it is speculated that theturbulence generated by the corrugation pattern may sustain a relativisticFermi process, accelerating particles close to the radiation reaction limit, asobserved in the Crab nebula. The required corrugation could be induced by thefast magnetosonic modes of downstream nebular turbulence; but it could also beproduced by upstream turbulence, either carried by the wind or seeded in theprecursor by the accelerated particles themselves.

A corrugated termination shock in pulsar wind nebulae?