Fig. 1: Context observations of the 2022 September 25 flare.
From: Observation of super-Alfvénic slippage of reconnecting magnetic field lines on the Sun
a, The soft X-ray flux in the 1–8 Å channel of the GOES satellite. The grey shaded area indicates the time period under study. b–g, Depictions of the flare at the first (b−d) and second (e−g) instants marked by dashed lines in a, showing flare loops observed in AIA 131 Å (b and e), the ribbons in AIA 304 Å (c and f) and the western ribbon observed in IRIS SJI 1,330 Å (in reversed intensity) (d and g). c, Rectangles indicate the field of view in panels d and g. The contours in b indicate the photospheric magnetic field BLOS saturated to ±500 G, while yellow and magenta indicate positive and negative magnetic flux, respectively. The arrows in f and g delineate the artificial cuts across and along the ribbons, respectively, used to construct time–distance diagrams. The brightest emission is plotted in white color in b, c, e and f. Black color represents the highest intensities in d and g. SJI observations in d and g are also presented in Extended Data Fig. 5 and their animated version in Supplementary Video 3. FOV, field of view.
