2025/09/22 by Shuyue Li, Li, Shuyue, Qingmin Zhang +9
Physics and Astronomy · #FOS: Physical sciences #Ionosphere and magnetosphere dynamics #Solar and Space Plasma Dynamics #Solar and Stellar Astrophysics (astro-ph.SR)
paper · pdf · doi:10.48550/arxiv.2509.17309
openalex publication_date 2025/09/22 · openalex created_date 2025/10/16 · openalex updated_date 2026/07/28
In this paper, we report multiwavelength and multipoint observations of the prominence eruption originating from active region 11163, which generated an M3.5 class flare and a coronal mass ejection (CME) on 2011 February 24. The prominence lifts off and propagates nonradially in the southeast direction. Using the revised cone model, we carry out three-dimensional reconstructions of the icecream-like prominence. The latitudinal inclination angle decreases from ∼60\degr to ∼37\degr, indicating that the prominence tends to propagate more radially. The longitudinal inclination angle almost keeps constant (-6\degr). The highly inclined prominence eruption and the related CME drive an extreme ultraviolet (EUV) wave, which propagates southward at speeds of ∼381.60 km s-1 and ∼398.59 km s-1 observed in 193 Å and 304 Å, respectively. The M3.5 class flare presents quasi-periodic pulsations (QPPs) in soft X-ray, hard X-ray, EUV, and radio wavelengths with periods of 80-120 s. Cotemporary with the flare QPPs, a thin current sheet and multiple plasmoids are observed following the eruptive prominence. Combining with the appearance of drifting pulsation structure, the QPPs are most probably generated by quasi-periodic magnetic reconnection and particle accelerations as a result of plasmoids in the current sheet.