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We present first results of three dimensional relativisticmagnetohydrodynamical simulations of Pulsar Wind Nebulae. They show that thekink instability and magnetic dissipation inside these nebulae may be the keyprocesses allowing to reconcile their observations with the theory of pulsarwinds. In particular, the size of the termination shock, obtained in thesimulations, agrees very well with the observations even for Poynting-dominatedpulsar winds. Due to magnetic dissipation the total pressure in the simulatednebulae is particle-dominated and more or less uniform. While in the main bodyof the simulated nebulae the magnetic field becomes rather randomized, close tothe termination shock, it is dominated by the regular toroidal field freshlyinjected by the pulsar wind. This field is responsible for driving polaroutflows and may explain the high polarization observed in pulsar wind nebulae.

Solution to the Sigma-Problem of Pulsar Wind Nebulae