The Spatial and Temporal Variations of Turbulence in a Solar Flare

Magnetohydrodynamic (MHD) plasma turbulence is believed to play a vital role in the production of energetic electrons during solar flares and non-thermal broadening spectral lines key sign this turbulence. Here, we determine how flare evolves time space using profiles Fe xxiv, xxiii xvi, observed by Hinode/EIS. Maps velocity are created for times covering X-ray rise, peak, decay. For first time, creation kinetic energy density maps reveal where available energization, suggesting that similar levels may be heat and/or accelerate large regions flare. We find distributed throughout entire flare; often greatest coronal loop tops, decaying at different rates locations. hotter ions (Fe xxiv xxiii), decreases as during/after peak shows clear spatial variation decreasing linearly from apex towards ribbon. cooler ion xvi), remains relativity constant flare, but steeply increases one region corresponding southern ribbon, peaking just prior hard X-rays before declining. The results suggest has more complex temporal structure than previously assumed, while newly introduced turbulent show availability identify important inhomogeneities macroscopic motions leading