Sympathetic Solar Eruption on 2024 February 9

• Published in: Research in astronomy and astrophysics Vol. 25; no. 1; pp. 15006 - 191
• Main Authors: Li, Shu-Yue, Zhang, Qing-Min, Ying, Bei-Li, Feng, Li, Su, Ying-Na, Lin, Mu-Sheng, Zhang, Yan-Jie
• Format: Journal Article
• Language: English
• Published: National Astromonical Observatories, CAS and IOP Publishing 01.01.2025; School of Science,Nanjing University of Posts and Telecommunications,Nanjing 210023,China; School of Astronomy and Space Science,University of Science and Technology of China,Hefei 230026,China; Key Laboratory of Dark Matter and Space Astronomy,Purple Mountain Observatory,Nanjing 2i0023,China%Key Laboratory of Dark Matter and Space Astronomy,Purple Mountain Observatory,Nanjing 2i0023,China%Key Laboratory of Dark Matter and Space Astronomy,Purple Mountain Observatory,Nanjing 2i0023,China
• Subjects: Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun: flares; Sun:filaments,prominences; Sun:flares; Sun:coronal mass ejections(CMEs)
• ISSN: 1674-4527; 2397-6209
• DOI: 10.1088/1674-4527/ad9a33

In this paper, we perform a follow-up investigation of the solar eruption originating from active region 13575 on 2024 February 9. The primary eruption of a hot channel generates an X3.4 class flare, a full-halo coronal mass ejection (CME), and an extreme-ultraviolet (EUV) wave. Interaction between the wave and a quiescent prominence (QP) leads to a large-amplitude, transverse oscillation of QP. After the transverse oscillation, QP loses equilibrium and rises up. The ascending motion of the prominence is coherently detected and tracked up to  ∼1.68 R ⊙ by the Solar UltraViolet Imager onboard the GOES-16 spacecraft and up to  ∼2.2 R ⊙ by the Solar Corona Imager (SCI_UV) of the Ly α Solar Telescope onboard the ASO-S spacecraft. The velocity increases linearly from 12.3 to 68.5 km s −1 at 18:30 UT. The sympathetic eruption of QP drives the second CME with a typical three-part structure. The bright core comes from the eruptive prominence, which could be further observed up to  ∼3.3 R ⊙ by the Large Angle Spectroscopic Coronagraph onboard the Solar and Heliospheric Observatory mission. The leading edge of the second CME accelerates continuously from  ∼120 to  ∼277 km s −1 . The EUV wave plays an important role in linking the primary eruption with the sympathetic eruption.