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F. C. Michel (Rice University)
Pulsars are generally expected to accelerate plasma "winds" to relativistic energies. However, tracking such acceleration and the interactions between the plasma and the accelerating fields are beyond the usual perturbation based wave-plasma dispersion relations. We present here a new approximate approach which will permit tracking plasma from rest to relativistic energies. This approach automatically includes self-consistently radiation reaction. It is most suitable for numerical calculations, is exact in an obvious limit, and seems robust in a coarse gridding. We will here discuss the approximation and illustrate some standard plasma results.
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