Reconnection-driven Magnetohydrodynamic Turbulence in a Simulated Coronal-hole Jet

How a coronal-hole jet may work, in an appeal to magnetic reconnection as a driver of turbulence in its structure, using numerical MHD simulations. Jet structures appear all over the Sun at various times, including in association with active-region flares. A coronal-hole jet is explicitly one that appears in an apparently unipolar magnetic corona, and hence the structure is a pseudostreamer. A turbulent volume in the jet flow is assumed, seeming to set this apart from the descriptions of jets as mini-filament eruptions. The cartoon here shows an intricate interplay of Alfvénic (yellow) and compressible (blue) waves comprising the turbulent structure.

      This is a beautiful and novel cartoon, based on solid-looking simulations, but the Archivist retains some skepticism here. "Reconnection" and "turbulence" may or may not be correct descriptions of the microphysics, but as the authors point out we have Parker Solar Probe and Solar Orbiter observations to look forward to.