Magnetic Energy Dissipation during the 2014 March 29 Solar Flares

Abstract

We calculated the time evolution of the free magnetic energy during the 2014-Mar-29 flare (SOL2014-03-29T17:48), the first X-class flare detected by IRIS. The free energy was calculated from the difference between the nonpotential field, constrained by the geometry of observed loop structures, and the potential field. We use AIA/SDO and IRIS images to delineate the geometry of coronal loops in EUV wavelengths, as well as to trace magnetic field directions in UV wavelengths in the chromosphere and transition region. We find an identical evolution of the free energy for both the coronal and chromospheric tracers, as well as agreement between AIA and IRIS results, with a peak free energy of $E_{free}(t_{peak})\approx (45\pm 2)\times 10^{30}$ erg, which decreases by an amount of $\Delta E_{free}\approx (29\pm 3)\times 10^{30}$ erg during the flare decay phase. The consistency of free energies measured from different EUV and UV wavelengths for the first time here, demonstrates that vertical electric currents (manifested in form of helically twisted loops) can be detected and measured from both chromospheric and coronal tracers.

ApJ Letters (accepted 2015-Apr-10; in press)

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• Observations and Modelling of the Pre-Flare Period of the 29 March 2014 X1 Flare
• Quasi-periodic pulsations in a solar flare with an unusual phase shift
• Helical Twisting Number and Braiding Linkage Number of Solar Coronal Loops
• Energy origination and triggering mechanism of a series of homologous confined flares