In multispecies relativistic turbulence, energization occurs at reconnection current sheets driven by the divergence of the relativistic pressure tensor, with electrons accelerated more efficiently than positrons due to species imbalance.
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5 Pith papers cite this work. Polarity classification is still indexing.
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3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.
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.
Reconnection in transrelativistic AGN coronae can energize protons to tens of PeV, producing a neutrino spectrum consistent with NGC 1068 observations without tuning the proton spectral slope.
Curvature acceleration in strong Alfvénic turbulence saturates due to diminishing energy exchange efficiency, producing particle distributions f(p) ∝ p^{-3} (non-relativistic) and f(γ) ∝ γ^{-3} (ultrarelativistic).
citing papers explorer
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Clumps in a Cocoon: Geometry and Mixing Set the Universal X-ray to H$\alpha$ Surface Brightness Ratio
3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.