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Flare reconnection-driven magnetic field and Lorentz force variations at the Sun's surface View all abstracts by submitter

Krzysztof Barczynski   Submitted: 2019-04-23 09:57

During eruptive flares, vector magnetograms show increasing horizontal magnetic field and downward Lorentz force in the Sun's photosphere around the polarity-inversion line. Such behavior has often been associated with the implosion conjecture and interpreted as the result of either momentum conservation while the eruption moves upward, or of the contraction of flare loops. We characterize the physical origin of these observed behaviors by analyzing a generic 3D MHD simulation of an eruptive flare. Even though the simulation was undesigned to recover the magnetic field and Lorentz force properties, it is fully consistent with them, and it provides key additional informations to understand them. The area where the magnetic field increases gradually develops between current ribbons, which spread away from each other and are connected to the coronal region. This area is merely the footprint of the coronal post- flare loops, whose contraction increases their shear field component and the magnetic energy density in line with the ideal induction equation. For simulated data, we computed the Lorentz force density map by applying the method used in observations. We obtained increase of the downward component of the Lorentz force density around the PIL ?consistent with observations. However, this significantly differs from the Lorentz force density maps obtained directly from the 3D magnetic field and current. These results altogether question previous interpretations based on the implosion conjecture and momentum conservation with the CME, and rather imply that the observed increases in photospheric horizontal magnetic fields result from the reconnection-driven contraction of sheared flare-loops.

Authors: Krzysztof Barczynski, Guillaume Aulanier, Sophie Masson, Michael S. Wheatland
Projects: None

Publication Status: accepted for publication in ApJ (April 19, 2019)
Last Modified: 2019-04-24 14:28
Go to main E-Print page  Oscillations Accompanying a He I 10830 ? Negative Fare in a Solar Facula II. Response of the Transition Region and Corona  Why Does the Solar Corona Abnormally Rotate Faster Than the Photosphere?  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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