A three-dimensional velocity of an erupting prominence prior to a coronal mass ejection. (27th February 2021)

• Record Type: Journal Article
• Authors: Gutierrez, Maria V; Otsuji, Kenichi; Asai, Ayumi; Terrazas, Raul; Ishitsuka, Mutsumi; Ishitsuka, Jose; Nakamura, Naoki; Yoshinaga, Yusuke; Morita, Satoshi; Ishii, Takako T; Ueno, Satoru; Kitai, Reizaburo; Shibata, Kazunari
• Is Part Of: Publications of the Astronomical Society of Japan. Volume 73:Number 2(2021)
• Page Start: 394
• Page End: 404
• Publication Date: 2021-02-27
• Subjects: Sun: chromosphere -- Sun: coronal mass ejections (CMEs) -- Sun: filaments, prominences -- Sun: flares; Astronomy -- Periodicals; 520.5
• DOI: 10.1093/pasj/psab006
• Languages: English
• ISSNs: 0004-6264

Abstract

Abstract: We present a detailed three-dimensional (3D) view of a prominence eruption, coronal loop expansion, and coronal mass ejections (CMEs) associated with an M4.4 flare that occurred on 2011 March 8 in the active region NOAA 11165. Full-disk Hα images of the flare and filament ejection were successfully obtained by the Flare Monitoring Telescope (FMT) following its relocation to Ica University, Peru. Multiwavelength observation around the Hα line enabled us to derive the 3D velocity field of the Hα prominence eruption. Features in extreme ultraviolet were also obtained by the Atmospheric Imager Assembly onboard the Solar Dynamic Observatory and the Extreme Ultraviolet Imager on board the Solar Terrestrial Relations Observatory - Ahead satellite. We found that, following collision of the erupted filament with the coronal magnetic field, some coronal loops began to expand, leading to the growth of a clear CME. We also discuss the succeeding activities of CME driven by multiple interactions between the expanding loops and the surrounding coronal magnetic field.