Image Details

Choose export citation format:

Understanding the Complex Morphology of a Coronal Mass Ejection. II. How Pre-eruptive Conditions Shape Coronal Mass Ejection Evolution

  • Authors: Abril Sahade, Cecilia Mac Cormack, Angelos Vourlidas, Teresa Nieves-Chinchilla, Cooper Downs, Clementina Sasso, Judith T. Karpen

Abril Sahade et al 2026 The Astrophysical Journal 1003 .

  • Provider: AAS Journals

Caption: Figure 1.

Pre-eruptive configuration and early eruption of the October event. (a) HMI magnetogram of AR 13873. The red dashed line marks the PIL. The magenta (orange) dot indicates the northern (southern) footpoint. (b) pre-eruption filament observed in AIA 304 at 05:16 UT (white arrow). Footpoints are marked as in panel (a). (c) First activation at 06:03 UT, with flare ribbon signatures. The southern extension of the ribbons is indicated by the white arrow. d) Eruptive filament at 06:16 UT, highlighted by the white arrow. (e) Early eruption at 06:25 UT observed by SUVI, shown as a composite of the 304 and 171 Å channels to show the core of the eruption and the ambient corona. (f) Post-eruptive arcade observed in AIA 171 at 07:54 UT. The white arrow indicates the location of the dimming associated with the northern footpoint. An animated version of this figure shows the evolution of the eruption in AIA 304, SUVI 304, SUVI 131, and SUVI 171 images from 05:00 to 09:00 UT. The real-time duration of the animation is 14 s.

(An animation of this figure is available in the online article.)

(An animation of this figure is available.)

The video/animation of this figure is available in the online journal.

Other Images in This Article
Copyright and Terms & Conditions

Additional terms of reuse