Turbulence transport in the solar corona: Theory, modeling, and Parker Solar Probe

A primary goal of the Parker Solar Probe (PSP) Mission is to answer outstanding question how solar corona plasma heated high temperatures needed for acceleration wind. Various heating mechanisms have been suggested, but one that gaining increasing credence associated with dissipation low frequency magnetohyrodynamic (MHD) turbulence. However, MHD turbulence models come in several flavors: which outwardly propagating Alfvén waves experience reflection from large-scale flow and density gradients corona, resulting counterpropagating couple nonlinearly produce quasi-2D dissipates heats thereby driving The second approach eschews a dominant outward flux argues instead dominates lower coronal generated constantly upwelling magnetic carpet, experiencing as it advected through into wind, yielding exceed million degrees. We review two models, describe modeling has done, relate PSP observations basic predictions both models. Although measurements are made super-Alfvénic close region, thus providing glimpse likely properties Observations low-frequency by wind allow us place constraints on turbulently drive supersonic