Explosive phenomena such as supernova remnant shocks and solar flares have demonstrated evidence for the production of relativistic particles. Interest has therefore been renewed in collisionless shock waves and magnetic reconnection as a means to achieve such energies. Although ions can be energized during such phenomena, the relativistic energy of the electrons remains a puzzle for theory. We present supercomputer simulations showing that efficient electron energization can occur during turbulent magnetic reconnection arising from a strong collisionless shock. Upstream electrons undergo first-order Fermi acceleration by colliding with reconnection jets and magnetic islands, giving rise to a nonthermal relativistic population downstream. These results shed new light on magnetic reconnection as an agent of energy dissipation and particle acceleration in strong shock waves.
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Article Synopsis
- The study examines how energy moves within plasma turbulence, focusing on its effects on heating in space and astrophysical environments.
- It suggests that magnetic reconnection plays a key role in energy transfer, facilitating both downward transfer to smaller scales and upward transfer to larger scales.
- Utilizing advanced simulations, the research provides solid evidence that magnetic reconnection initiates this complex dual energy transfer process.
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