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Evolution of Spatial Complexity in Flare Ribbon Substructure and Its Relationship to Magnetic Reconnection Dynamics

  • Authors: Marcel F. Corchado Albelo, Maria D. Kazachenko, Ryan J. French, Vadim M. Uritsky, Emily Mason, Cole A. Tamburri, Rahul Yadav, Benjamin J. Lynch

Marcel F. Corchado Albelo et al 2026 The Astrophysical Journal 1000 .

  • Provider: AAS Journals

Caption: Figure 1.

Overview of the M6.5 flare in AR 12371 on 2015 June 22. (a) GOES 1–8 Å light curve; the IRIS-SJI analysis window is shaded yellow, and the IRIS-SG start time is marked by the vertical line. (b) AIA 193 Å image at 17:51 UT. (c) Corresponding HMI Bz magnetogram at 17:51 UT. (d) IRIS-SJI 1330 Å at 17:51 UT. Green and blue boxes show the SJI and SG FOVs, respectively. (e) Normalized time series of variables integrated over the respective FOVs: IRIS 1330 Å intensity (IUV; red), GOES 1–8 Å (ISXR; blue dashed) and its time derivative (dISXR/dt; blue solid), Fermi (IHXR) 15–25 keV (green dashed) and 50–100 keV (green solid), and ribbon-derived reconnection flux (Φ; black dashed) and rate (dΦ/dt; black solid).

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