MHD and forward modeling of reconnection-driven coronal heating by Nanojets during MHD avalanches

In the solar corona, heating might stem from numerous, localized and impulsive episodes of magnetic energy release, referred to as “nanoflares”. During avalanche-like processes, misaligned magnetic field lines can rupture and reconnect, thus generating a nanoflare storm. Small-angle field line reconnection are known to produce the acceleration of collimated outflow jets, named “nanojets”. Detection and analysis of such reconnection nanojets becomes then important, because they are a signature of the reconnection. We performed full 3D magnetohydrodynamic (MHD) simulations of interacting and twisted coronal flux tubes strands. In our model the magnetized atmosphere is stratified from the high-beta chromosphere to the corona through the narrow transition region. Photospheric rotation motions stress the flux tubes until they become unstable and determine an avalanche of reconnection episodes with the formation, fragmentation, and dissipation of current sheets akin to a nanoflare storm. In this work we address the nanojets which form from these reconnection episodes, at Parker energies (about 10^24 ergs) and at speeds even above 1000 km/s, and we study their detectability, in particular considering EUV observations with the Atmospheric Image Assembly (AIA) on-board Solar Dynamics Observatory and the forthcoming MUltislit Solar Explorer (MUSE).