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The termination shock of a pulsar wind is located roughly where the rampressure matches that of the surrounding medium. Downstream of the shock, MHDmodels of the diffuse nebular emission suggest the plasma is weakly magnetized.However, the transition from a Poynting-dominated MHD wind to aparticle-dominated flow is not well understood. We discuss a solution of this"sigma problem" in which a striped wind converts into a strong, superluminalelectromagnetic wave. This mode slows down as it propagates radially, and itsram pressure tends to a constant value at large radius, a property we use tomatch the solution to the surrounding nebula. The wave thus forms a pre-cursorto the termination shock, which occurs at the point where the wave dissipates.Possible damping and dissipation mechanisms are discussed qualitatively.

Superluminal Waves and the Structure of Pulsar Wind Termination Shocks