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As a fundamental magnetic structure in the solar corona, electric currentsheets (CSs) can form either prior to or during solar flare, and they areessential for magnetic energy dissipation in the solar corona by enablingmagnetic reconnection. However static reconstruction of CS is rare, possiblydue to limitation inherent in available coronal field extrapolation codes. Herewe present the reconstruction of a large-scale pre-flare CS in solar activeregion 11967 using an MHD-relaxation model constrained by SDO/HMI vectormagnetogram. The CS is found to be associated with a set of peculiar homologousflares that exhibit unique X-shaped ribbons and loops occurring in aquadrupolar magnetic configuration. This is evidenced by that the field linestraced from the CS to the photosphere form an X shape which nearly preciselyreproduces the shape of the observed flare ribbons, suggesting that the flareis a product of the dissipation of the CS through reconnection. The CS forms ina hyperbolic flux tube, which is an intersection of two quasi-separatrixlayers. The recurrence of the X-shaped flares might be attributed to therepetitive formation and dissipation of the CS, as driven by the photosphericfootpoint motions. These results demonstrate the power of data-constrained MHDmodel in reproducing CS in the corona as well as providing insight into themagnetic mechanism of solar flares.

Reconstruction of a Large-scale Pre-flare Coronal Current Sheet Associated with an Homologous X-shaped Flare