SKA will enable spatially resolved radio studies of pulsar wind nebulae to probe particle acceleration and propagation in ultra-relativistic outflows.
Filamentary Diffusion of Cosmic Rays on Small Scales
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abstract
We investigate the diffusion of cosmic rays (CR) close to their sources. Propagating individual CRs in purely isotropic turbulent magnetic fields with maximal scale of spatial variations Lmax, we find that CRs diffuse anisotropically at distances r <~ Lmax from their sources. As a result, the CR densities around the sources are strongly irregular and show filamentary structures. We determine the transition time t* to standard diffusion as t* ~ 10^4 yr (Lmax/150 pc)^b (E/PeV)^(-g) (Brms/4 muG)^g, with b ~ 2 and g = 0.25-0.5 for a turbulent field with Kolmogorov power spectrum. We calculate the photon emission due to CR interactions with gas and the resulting irregular source images.
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Understanding Pulsar Wind Nebulae with the SKA
SKA will enable spatially resolved radio studies of pulsar wind nebulae to probe particle acceleration and propagation in ultra-relativistic outflows.