Theoretical models of the spectra and flow dynamics of plerions are reviewed. The models constrain pulsar wind properties, e.g. the ratio sigma of Poynting flux to kinetic energy flux, when combined with high-resolution images of the wind-plerion interface. It is shown that a pulsar wind is oscillatory; it propagates as a subluminal, relativistic plasma wave, with sigma >~ 1, in the inner wind zone r ~< 108 rc (rc is the light-cylinder distance) and as a superluminal wave, with sigma >> 1, in the outer wind zone r >~ 108 rc. The inner-outer transition is triggered by a magnetoparametric instability; it may account for the optical and X-ray `inner knots' of the Crab and PSR B1509-58.
Neutron Stars in Supernova Remnants
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