EGU25-16745, updated on 15 Mar 2025
https://doi.org/10.5194/egusphere-egu25-16745
EGU General Assembly 2025
© Author(s) 2025. This work is distributed under
the Creative Commons Attribution 4.0 License.
The Role of Magnetic Skeleton in Solar Flare Filaments Activities
Juan Guo
Juan Guo
  • National Space Science Center, Chinese Academic of Science, Beijing, China (guojuan@nssc.ac.cn)

We report an M9.3 flare and filaments activities from NOAA Active Region 11261 that are strongly modulated by the 3D magnetic skeleton. Magnetic field extrapolation from the vector magnetic field suggests complex magnetic connectivity and the existence of a high coronal null point southeast of the active region. A small filament over the  inversed V-shaped polarity inversion line erupted and resulted in the M9.3 flare associated with a weak hot mass ejection, CME-like features, and the formation and activity of a relatively large filament. The ejection features and the eruption of the large filament were toward the southeast. Comparative analyses have disclosed the following new facts: (1) the trajectory of looptop hard X-ray emission provides solid evidence that the magnetic reconnection site propagated up toward the coronal null point as the flare and filaments erupted. (2) the EVU observations show coronal mass ejection-like eruption features in the ejection region of the magnetic skeleton. (3) the closed fan confined the west end of the large filament and the corresponding flare ribbons. We demonstrate a spatiotemporal relationship between the magnetic skeleton and the flare filament activity. We conclude that the magnetic skeleton can modulate and determine almost all the characteristics of the studied activity in the corresponding scale.

How to cite: Guo, J.: The Role of Magnetic Skeleton in Solar Flare Filaments Activities, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-16745, https://doi.org/10.5194/egusphere-egu25-16745, 2025.