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During solar flares, a large fraction of the released magnetic energy iscarried by energetic electrons that transfer and deposit energy in the Sun'satmosphere. Electron transport is often approximated by a cold thick-targetmodel (CTTM), assuming that electron energy is much larger than the temperatureof the ambient plasma, and electron energy evolution is modeled as a systematicloss. Using kinetic modeling of electrons, we re-evaluate the transport anddeposition of flare energy. Using a full collisional warm-target model (WTM),we account for electron thermalization and for the properties of the ambientcoronal plasma such as its number density, temperature and spatial extent. Weshow that the deposition of non-thermal electron energy in the lower atmosphereis highly dependent on the properties of the flaring coronal plasma. Ingeneral, thermalization and a reduced WTM energy loss rate leads to an increaseof non-thermal energy transferred to the chromosphere, and the deposition ofnon-thermal energy at greater depths. The simulations show that energy isdeposited in the lower atmosphere initially by high energy non-thermalelectrons, and later by lower energy non-thermal electrons that partially orfully thermalize in the corona, over timescales of seconds, unaccounted for inprevious studies. This delayed heating may act as a diagnostic of both theinjected non-thermal electron distribution and the coronal plasma, vital forconstraining flare energetics.

The Role of Energy Diffusion in the Deposition of Energetic Electron Energy in Solar and Stellar Flares