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Turbulence plays a key role for forming the complex geometry of thelarge-scale current sheet (CS) and fast energy release in a solar eruption. Inthis paper, we present full 3D high-resolution simulations for the process of amoderate Coronal Mass Ejection (CME) and the thermodynamical evolution of thehighly confined CS. Copious elongated blobs are generated due to tearing andplasmoid instabilities giving rise to a higher reconnection rate and undergothe splitting, merging and kinking processes in a more complex way in 3D. Adetailed thermodynamical analysis shows that the CS is mainly heated byadiabatic and numerical viscous terms, and thermal conduction is the dominantfactor that balances the energy inside the CS. Accordingly, the temperature ofthe CS reaches to a maximum of about 20 MK and the range of temperatures isrelatively narrow. From the face-on view in the synthetic Atmospheric ImagingAssembly 131 $\mathring{A}$, the downflowing structures with similar morphologyto supra-arcade downflows are mainly located between the post-flare loops andloop-top, while moving blobs can extend spikes higher above the loop-top. Thedownward-moving plasmoids can keep the twisted magnetic field configurationuntil the annihilation at the flare loop-top, indicating that plasmoidreconnection dominates in the lower CS. Meanwhile, the upward-moving ones turninto turbulent structures before arriving at the bottom of the CME, implyingthat turbulent reconnection dominates in the upper CS. The spatialdistributions of the turbulent energy and anisotropy are addressed, which showa significant variation in the spectra with height.

Three-dimensional simulation of thermodynamics on confined turbulence in a large-scale CME-flare current sheet