Numerical transport modeling of the Cygnus Bubble finds that spatially dependent Bohm diffusion and strong suppression of the diffusion coefficient over at least 150 pc are required to match the observed gamma-ray spectrum and morphology, implying extreme assumptions for steady hadronic acceleration
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SKA will enable spatially resolved radio studies of pulsar wind nebulae to probe particle acceleration and propagation in ultra-relativistic outflows.
citing papers explorer
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Suppressed diffusion and gamma-ray emission from the Cygnus Bubble
Numerical transport modeling of the Cygnus Bubble finds that spatially dependent Bohm diffusion and strong suppression of the diffusion coefficient over at least 150 pc are required to match the observed gamma-ray spectrum and morphology, implying extreme assumptions for steady hadronic acceleration
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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.
- Anisotropic Diffusion in Pulsar Halos: Interpreting the asymmetric morphology of Geminga and Monogem halos measured by HAWC