1. Energy Partition in X-Class Flares With G. Holman, G. Share, A. Panasyuk, A. Ciaravella, Y.-K. Ko, J. Kohl ½ m v 2 (bulk or turbulent) B 2 /8π —> 3nkT non-thermal e -, p How much to each? Controlled by what parameters? Plasma β Length scale M A Magnetic topology E field

2. GOES – Thermal X-ray L TH, EM, T RHESSI – non-thermal Energy Deposition L NT, and area A V ~ A 3/2 with EM Gives n E TH = 3VnkT dE TH /dt rate of change of Thermal Energy by evaporation P cond = κT 7/2 A ½ v ~ 300 km/s, comparable to 10 6 K, while T > 10 7 K SUMER, X-ray crystal spectrometers Kinetic < Thermal energy

3. How much energy gets radiated from cooler gas? Slit spectrometer almost always misses impulsive kernel UVCS captures flare photons scattered from corona O VI photons from flare scatter Off coronal O VI ions: Measure L TR Ly photons from flare scatter off Coronal H I atoms: Measure L CH

4. O VI flash coincides with hard X-rays, precedes thermal X-rays Begins to fade before CME blows away corona 4:1 ratio implies scattered radiation Upflow Information

5. L CH ~ 10 L TR : Exceeds L TH for first few minutes Conduction to lower T does not dominate X-ray gas energetics P cond can’t be that high L NT balances dE/dt In X-class flare, non-thermal particles dominate energy dissipated in current sheet