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Understanding the Complex Morphology of a Coronal Mass Ejection: Multiview Analysis and Numerical Modeling

  • Authors: Cecilia Mac Cormack, Abril Sahade, Angelos Vourlidas, Phillip Hess, Robin Colaninno, Teresa Nieves-Chinchilla

Cecilia Mac Cormack et al 2025 The Astrophysical Journal 988 .

  • Provider: AAS Journals

Caption: Figure 4.

Snapshots of the evolution of the MFR obtained by CORHEL-CME from an arbitrary POV. The gray sphere (1 R) has Earth's meridian (green line), equator (teal line), and the STA meridian (pink line) plotted for reference. Panel (a): early rise of the MFR showing the northern leg's faster ascent. Panel (b): the southern leg started to reconnect with the open field lines of the west coronal hole (green lines). Panel (c): both legs of the MFR reached a similar height, where the northern leg started to reconnect with the east coronal hole after escaping the helmet streamer arcade. Panel (d): the MFR reaches a balance with the ambient field, evolving mostly self-similarly. The inner MFR (pink lines) remains attached to the solar surface at both ends. Panel (e): later snapshot of the evolution showing similar characteristics of the previous panels after more expansion (see the size of the sphere for reference).

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