Simultaneous Proton and Electron Energization during Macroscale Magnetic Reconnection

Abstract

The results of simulations of magnetic reconnection accompanied by electron and proton heating and energization in a macroscale system are presented. Both species form extended powerlaw distributions that extend nearly three decades in energy. The primary drive mechanism for the production of these nonthermal particles is Fermi reflection within evolving and coalescing magnetic flux ropes. While the powerlaw indices of the two species are comparable, the protons overall gain more energy than electrons and their power law extends to higher energy. The power laws roll into a hot thermal distribution at low energy with the transition energy occurring at lower energy for electrons compared with protons. A strong guide field diminishes the production of non-thermal particles by reducing the Fermi drive mechanism. In solar flares, proton power laws should extend down to 10's of keV, far below the energies that can be directly probed via gamma-ray emission. Thus, protons should carry much more of the released magnetic energy than expected from direct observations.

14 pages, 8 figures

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Cited by in corpus (6)

• Magnetic reconnection-driven energization of protons up to 400 keV at the near-Sun heliospheric current sheet
• Solar Flare Ion Temperatures
• Energy partitioning between thermal and non-thermal electrons and ions in magnetotail reconnection
• The Maximum Particle Energy Gain During Magnetic Reconnection
• Stereoscopic Observations of Solar X-ray Sources Explained by a Data-Constrained Magnetohydrodynamic Simulation
• Probing Proton versus Electron Heating and Energization during Magnetic Reconnection