MHD-PIC simulations find that the non-thermal particle spectral index alpha steepens as alpha proportional to beta to the power 0.5 in the relativistic regime, due to inertial mass density acting as an energy sink that reduces Alfven velocity.
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Turbulence-driven magnetic reconnection in the corona of NGC 1068 accelerates protons to ~10^14 eV, producing neutrinos via pp interactions that match IceCube data while gamma rays are attenuated by pair production.
Simulations of turbulent reconnection in relativistic jets show energy-independent acceleration time in the Fermi regime matching theory up to a Larmor radius threshold set by current sheet thickness, then energy-dependent drift regime.
citing papers explorer
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The $\beta$-Dependence of Particle Spectra in Relativistic Turbulent Reconnection
MHD-PIC simulations find that the non-thermal particle spectral index alpha steepens as alpha proportional to beta to the power 0.5 in the relativistic regime, due to inertial mass density acting as an energy sink that reduces Alfven velocity.
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A Turbulence-Driven Magnetic Reconnection Model for the High-Energy Neutrino Emission from NGC 1068
Turbulence-driven magnetic reconnection in the corona of NGC 1068 accelerates protons to ~10^14 eV, producing neutrinos via pp interactions that match IceCube data while gamma rays are attenuated by pair production.
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Particle Acceleration Time due to Turbulent-Induced Magnetic Reconnection
Simulations of turbulent reconnection in relativistic jets show energy-independent acceleration time in the Fermi regime matching theory up to a Larmor radius threshold set by current sheet thickness, then energy-dependent drift regime.