Abstract:
Using the photospheric magnetic and coronal observations of Solar Dynamics Observatory, we studied the buildup and eruption of coronal nonpotential magnetic structure in emerging active region (AR) 12673. The velocity field derived from tracked vector-magnetograms indicates persistent shear and converging motions of flux regions about the polarity inversion line (PIL). A major helicity injection occurs during rapid flux emergence consistent with the very fast flux emergence phase. While this helicity flux builds up the sigmoid by September 4, the helicity injection by the continued shear and converging motions in the later evolution contributes to sigmoid sustenance and its core field twist as a manifestation of the flux rope that erupts after exceeding the critical value of the twist. Moreover, the total length of sheared PIL segments correlates with the non-neutralized current and maintains a higher value in both polarity regions as a signature of eruptive capability of the AR according to the flux rope models. The modeled magnetic field qualitatively reproduces the sigmoidal structure capturing major features like twisted core flux as flux rope and hook-shaped parts connecting at the middle of the PIL. Study of quasi-separatrix-layers reveals that the sheared arcade, enclosing the flux rope, is stressed to a critically stable state, and its coronal height becomes doubled from September 4 to 6. While demonstrating the fast injection of helicity per unit flux as the crucial factor for severe space-weather events, this study explains the formation of the flux rope and recurrent eruptive nature of the AR by the critically stable state of the sheared arcade early on September 6.
