A sample of 27 Galactic pulsar wind nebulae shows a diffusion coefficient about two orders of magnitude below the Galactic average, implying large low-diffusion bubbles around these pulsars.
The theory of pulsar wind nebulae
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abstract
I review the current status of our theoretical understanding of Pulsar Winds and associated nebulae (PWNe). In recent years, axisymmetric models of pulsar winds with a latitude dependent energy flux have proved very successful at explaining the morphology of PWNe as seen in the X-rays. This success has prompted developments aimed at using multi-wavelength observations of these nebulae as a diagnostics of the hidden physics of the pulsar wind and of the mechanism(s) through which particles are accelerated in these sources. I will discuss these most recent developments in terms of the information that we infer from detailed comparison of simulated non-thermal emission with current observations.
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Evidences of low-diffusion bubbles around Galactic pulsars
A sample of 27 Galactic pulsar wind nebulae shows a diffusion coefficient about two orders of magnitude below the Galactic average, implying large low-diffusion bubbles around these pulsars.