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Magnetohydrodynamic Simulations for Studying Solar Flare Trigger Mechanism  

Johan Muhamad   Submitted: 2017-06-22 19:51

In order to understand the flare trigger mechanism, we conduct three-dimensional magnetohydrodynamic simulations using a coronal magnetic field model derived from data observed by the Hinode satellite. Several types of magnetic bipoles are imposed into the photospheric boundary of the Non-linear Force-Free Field (NLFFF) model of Active Region NOAA 10930 on 2006 December 13 to investigate what kind of magnetic disturbance may trigger the flare. As a result, we confirm that certain small bipole fields, which emerge into the highly sheared global magnetic field of an active region, can effectively trigger a flare. These bipole fields can be classified into two groups based on their orientation relative to the polarity inversion line: the so called opposite polarity (OP) and reversed shear (RS) structures as suggested by Kusano et al. We also investigate the structure of the footpoints of reconnected field lines. By comparing the distribution of reconstructed field lines and the observed flare ribbons, the trigger structure of the flare can be inferred. Our simulation suggests that the data-constrained simulation, taking into account both the large-scale magnetic structure and small-scale magnetic disturbance (such as emerging fluxes) is a good way to discover a flare producing AR, which can be applied to space weather prediction.

Authors: Johan Muhamad, Kanya Kusano, Satoshi Inoue, Daikou Shiota
Projects: Hinode/SOT,Hinode/XRT

Publication Status: Published in ApJ
Last Modified: 2017-06-28 08:41
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Magnetohydrodynamic Simulations for Studying Solar Flare Trigger Mechanism

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