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Global Energetics of Solar Flares. IX. Refined Magnetic Modeling View all abstracts by submitter

Markus J. Aschwanden   Submitted: 2019-09-18 13:37

A more accurate analyticalsolution of the vertical-current approximation nonlinear force-freefield (VCA3-NLFFF) model is presented that includes besides theradial (Br) and the azimuthal(Bϕ ) magnetic field components, apoloidal component (Bθ ≠ 0) also. This new analytical solution is of second-order accuracy in the divergence-freeness condition, and of third-order accuracy in the force-freeness condition. We re-analyze the sample of 173 GOES M- and X-class flares observed with the Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO). The new code reproduces helically twisted loops with a low winding number below the kink instability consistently, avoiding unstable, highly-twisted structures of the Gold-Hoyle flux rope type. The magnetic energies agree within EVCA3 / EW = 0.99±0.21 with the Wiegelmann (W-NLFFF) code. The time evolution of the magnetic field reveals multiple, intermittent energy build-up and releases in most flares, contradicting both the Rosner-Vaiana model (with gradual energy storage in the corona) and the principle of time scale separation (τflare ≪ τstorage) postulated in self-organized criticality models. The mean dissipated flare energy is found to amount to 7%±3% of the potential energy, or 60%±26% of the free energy, a result that can be used for predicting flare magnitudes based on the potential field of active regions.

Authors: Markus J. Aschwanden
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Publication Status: ApJ (Sept 23, 2019; in press)
Last Modified: 2019-09-23 13:47
Go to main E-Print page  Non-Stationary Fast-Driven Self-Organized Criticality in Solar Flares  The Solar Orbiter SPICE instrument - An extreme UV imaging spectrometer  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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