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Pulsar Wind Nebulae (PWNe) constitute an ideal astrophysical environment totest our current understanding of relativistic plasma processes. It is wellknown that magnetic fields play a crucial role in their dynamics and emissionproperties. At present, one of the main issues concerns the level of magneticturbulence present in these systems, which in the absence of space resolvedX-ray polarization measures cannot be directly constrained. In this work weinvestigate, for the first time using simulated synchrotron maps, the effect ofa small scale fluctuating component of the magnetic field on the emissionproperties in X-ray. We illustrate how to include the effects of a turbulentcomponent in standard emission models for PWNe, and which consequences areexpected in terms of net emissivity and depolarization, showing that the X-raysurface brightness maps can provide already some rough constraints. We thenapply our analysis to the Crab and Vela nebulae and, by comparing our modelwith Chandra and Vela data, we found that the typical energies in the turbulentcomponent of the magnetic field are about 1.5 to 3 times the one in the orderedfield.

Modeling the effect of small-scale magnetic turbulence on the X-ray properties of Pulsar Wind Nebulae