Abstract

High-energy non-thermal particles are produced during explosive energy-release phenomena in space and solar environments. Previous studies have established that magnetic reconnection can convert magnetic energy to not only power flows and heating but also to produce non-thermal energetic particles. However, significant signatures of high-energy particles are often found far away from the reconnection region (e.g., at the footpoints of flaring loops and in the inner regions of the terrestrial magnetosphere). Here we combine observations, simulations and theories to systematically study particle acceleration of flares and substorms with particular emphasis on the energetics. Specifically, we will focus on the following key unanswered questions:

• How energies are partitioned between thermal and non-thermal particles in the key regions of solar flares and the Earth’s magnetosphere?
• How energies are transported (in the forms of Poynting, enthalpy and bulk kinetic energy fluxes) to the obstructions (i.e., flaring loops and the chromosphere, the dipole magnetosphere and the ionosphere)?

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