Authors: Ivan Oparin (New Jersey Institute of Technology), Sabastian Fernandes (New Jersey Institute of Technology), Bin Chen (New Jersey Institute of Technology), Chengcai Shen (Center for Astrophysics | Harvard & Smithsonian), Xiaocan Li (Dartmouth College), Sijie Yu (New Jersey Institute of Technology), Fan Guo (Los Alamos National Laboratory)

The extended cusp-like structures in the above loop-top regions of solar flares, first discovered by Yohkoh in soft X-rays, have been considered as a key signature of magnetic reconnection. Recent multi-perspective observations done by SDO and STEREO have resolved their formation and temporal evolution and revealed an inherently three-dimensional geometry. The energy release process and subsequent heating still remain a matter of primarily physical interest. The full-scale three-dimensional magnetohydrodynamic and kinetic models of plasma and particle dynamics in solar flares can be a key to understanding how the plasma gets heated and transported in a solar flare. The results of numerical simulations can be directly compared with the observations in different wavelengths. In this work, we try to reveal the sites where magnetic energy is released by associating the observed features with the locations of the structures that can be responsible for the heating, such as shocks or highly turbulent plasma. We report the results of three-dimensional modeling of the synthetic thermal emission in ultraviolet and Soft X-ray ranges and make comparisons with multi-perspective observations of candle-flame-shaped solar flares.