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  Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection

Cheng, X., Xing, C., Aulanier, G., Solanki, S. K., Peter, H., & Ding, M. D. (2023). Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection. The Astrophysical Journal, 954, L47. doi:10.3847/2041-8213/acf3e4.

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アイテムのパーマリンク: https://hdl.handle.net/21.11116/0000-000E-79B8-B 版のパーマリンク: https://hdl.handle.net/21.11116/0000-000E-79B9-A
資料種別: 学術論文

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URL:
https://ui.adsabs.harvard.edu/abs/2023ApJ...954L..47C (全文テキスト(全般))
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 作成者:
Cheng, X.1, 著者           
Xing, C., 著者
Aulanier, G., 著者
Solanki, S. K.1, 著者           
Peter, H.1, 著者           
Ding, M. D., 著者
所属:
1Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832289              

内容説明

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キーワード: Solar coronal mass ejections; Solar magnetic reconnection; Solar flares; Magnetohydrodynamics; 310; 1504; 1496; 1964; Astrophysics - Solar and Stellar Astrophysics; Physics - Space Physics
 要旨: Coronal mass ejections are explosive plasma phenomena prevalently occurring on the Sun and probably on other magnetically active stars. However, how their pre-eruptive configuration evolves toward the main explosion remains elusive. Here, based on comprehensive observations of a long-duration precursor in an event on 2012 March 13, we determine that the heating and slow rise of the pre-eruptive hot magnetic flux rope (MFR) are achieved through a precursor reconnection located above cusp-shaped high-temperature precursor loops. It is observed that the hot MFR threads are built up continually, with their middle initially showing an "M" shape and then being separated from the cusp of precursor loops, causing the slow rise of the entire MFR. The slow rise, in combination with the thermal-dominated hard X-ray source concentrated at the top of the precursor loops, shows that the precursor reconnection is much weaker than the flare reconnection of the main eruption. We also perform a 3D magnetohydrodynamics simulation that reproduces the early evolution of the MFR transiting from the slow to fast rise. It is revealed that the magnetic tension force pertinent to "M"-shaped threads drives the slow rise, which, however, evolves into a magnetic pressure gradient-dominated regime responsible for the rapid acceleration eruption.

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 日付: 2023
 出版の状態: 出版
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 識別子(DOI, ISBNなど): DOI: 10.3847/2041-8213/acf3e4
ISSN: 0004-637X
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出版物 1

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出版物名: The Astrophysical Journal
種別: 学術雑誌
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出版社, 出版地: -
ページ: - 巻号: 954 通巻号: - 開始・終了ページ: L47 識別子(ISBN, ISSN, DOIなど): -