Speaker
Description
Solar observations provide a wealth of data at high resolution in all layers of the solar atmosphere, obtained from ground-based and space-born observatories. A multi-layer analysis of a C-class flare observed on 1 July 2012 is presented using high-resolution Swedish 1-m Solar Telescope (SST) observations, SDO/HMI SHARP data, SDO/AIA imaging, and potential field extrapolations. The chromospheric structure, flare ribbon positions, fine-scale polarity inversion line (PIL), photospheric velocity flows and the components of the rate-of-strain tensor are strongly co-spatial. This indicates that the flare occurred within a well-defined area of photospheric deformation. The extrapolated magnetic field lines are rooted across the PIL, with opposite footpoints embedded in distinct flow streams and different local strain environments, consistent with differential stressing. The field lines are spatially consistent with the chromospheric and ultraviolet flare ribbons observed in SST Hα and AIA 1700 Å, linking the photospheric deformation to the overlying flare geometry. The combined observations strongly suggest that localised strain and shear flow around the PIL contribute to the magnetic field evolution before and after the flare. This event therefore provides a compelling example of how fine-scale photospheric deformation can organise flare-relevant magnetic connectivity from the photosphere into the chromosphere and lower corona.
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