0_5432 The solar corona shows inexplicably high temperatures, up to million degrees, when compared with the cold lower photosphere. The conversion of magnetic energy into thermal one through the magnetic reconnection has been chased for the last decades as the mechanism to explain this phenomenon. The reason why such mechanism remains elusive is because reconnection events are singularly too small and fast to be detected (nanoflares), whereas their collective action is sufficient to sustain the million degrees corona against thermal conduction and radiative losses.
Coronal loops are confined arch-like magnetic structures in active regions of the solar corona where the plasma is confined to flow along the magnetic field because of the extremely low plasma beta. 
We perform magnetohydrodynamics (MHD) simulations of magnetic reconnection events in coronal loops where small energies are converted into thermal and kinetic energy. We especially focus on the dynamic counter part of nanoflares, i.e. the nanojets resulting from the magnetic tension that is generated together with the magnetic energy release as a byproduct of the magnetic reconnection. Nanojets, although not frequent, have been observed as short lived motion of plasma in the transverse direction with respect to the guiding field of the coronal loops.
We analyse the relationship between the nanoflare and the nanojet, explaining how the latter, when observed, could give away the occurrence of the former.
Such results are especially interesting in light of the newly approved MUSE mission of NASA, a new high cadence high resolution EUV spectrometer to be launched in 2027.
Our 3D MHD simulations are key to bridge the gap between idealised magnetic reconnection models and future MUSE observations.