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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 3.

Evolution of FRBLE complexity and reconnection proxies. (a)–(c) Example frames (same as Figures 2(a5), (b5), and (c5)) showing ﹩{ \mathcal D }﹩ along the FRBLE at 17:52, 17:58, and 18:16 UT. Contours show HMI Bz levels: +500/+1000 G (red), −500/ − 1000 G (blue), and 0 G (white). (d) and (e) Distributions ﹩{w}_{{ \mathcal D }}﹩ for the positive and negative polarity ribbons. Solid lines show the mean ﹩\bar{{ \mathcal D }}﹩, dotted lines show the 95th percentile, and black dashed lines show the box-counting dimension ﹩{{ \mathcal D }}_{{{\rm{BC}}}}﹩. (f) and (g) Time series reconnection dynamics proxies in positive and negative magnetic polarity FRBLEs, respectively. The solid and dashed colored lines (red and blue) represent the 1330 Å intensity emitted from the FRBLE and full SJI FOV, respectively, while the black dashed line shows the cumulative reconnection rate derived from FRBLE observations. Vertical gray lines mark the times in (a)–(c).

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