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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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).
Coherent structures that self-consistently emerge in strong MHD turbulence serve as the dominant sites for localized electric-field intensification and repeated particle acceleration across cosmic plasmas.
citing papers explorer
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Turbulent AGN coronae as the origin of diffuse neutrinos up to PeV energies
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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Can magnetic reconnection power neutrino emission from AGN coronae?
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.
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Distributions of particles accelerated by strong Alfv\'enic turbulence
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).
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Strong MHD Turbulence and Coherent Structures as Drivers of Cosmic Particle Acceleration
Coherent structures that self-consistently emerge in strong MHD turbulence serve as the dominant sites for localized electric-field intensification and repeated particle acceleration across cosmic plasmas.
- Transport of electrons in tangled magnetic fields