A population of AGN coronae with magnetization parameters spanning up to σ ~ 10 can reproduce the entire observed diffuse neutrino flux from TeV to PeV energies.
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MMS data shows perpendicular electrons dominate j·E dissipation in magnetotail magnetic structures during turbulent reconnection, with bidirectional energy transfer and quantified mechanisms including parallel E, Fermi, betatron, and polarization effects.
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.
This review summarizes the basic principles of electron transport in inhomogeneous and tangled magnetic fields through gyro-centre trajectories, kinetic instabilities, trapping, and diffusion processes.
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