Turbulent electron-ion coronae around accreting black holes self-regulate into a two-temperature state that generates nonthermal ions and X-ray spectra consistent with observations including an MeV tail.
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Pair production via radiative magnetic reconnection near spinning black holes supplies non-uniform plasma to jets at levels sufficient to explain M87 radio emission.
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.
citing papers explorer
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High-energy Emission from Turbulent Electron-ion Coronae of Accreting Black Holes
Turbulent electron-ion coronae around accreting black holes self-regulate into a two-temperature state that generates nonthermal ions and X-ray spectra consistent with observations including an MeV tail.
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Non-uniform particle injection into black hole jets by radiative magnetic reconnection
Pair production via radiative magnetic reconnection near spinning black holes supplies non-uniform plasma to jets at levels sufficient to explain M87 radio emission.
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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.