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Updated: Jul 9, 2026

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クロモスフィアのアネモネ・ジェットは,至る所に存在する再接続の証拠である
Kazunari Shibata1, Tahei Nakamura, Takuma Matsumoto
1Kwasan and Hida Observatories, Kyoto University, Yamashina, Kyoto 607-8471, Japan. shibata@kwasan.kyoto-u.ac.jp
まとめ
太陽の染色体圏の小さな磁気再接続イベントは,アネモネのジェットとして観察され,太陽の大気の加熱の長年のパズルを説明することができます. これらの至る所に存在する特徴は,広範囲に広がり,小規模な再接続が太陽の染色球とコロナを暖めるための鍵であることを示唆しています.
科学分野:
- ソーラー物理学 ソーラー物理学
- プラズマ物理学 プラズマ物理学
- 天体物理学 天体物理学
背景:
- 太陽の染色球とコロナの加熱は,太陽物理学の重要な未解決問題である.
- Hinodeの観測は,アクティブな地域,特に太陽の斑点の外部のクロモスフィアのアネモネジェットの一般的な発生を明らかにしました.
研究 の 目的:
- クロモスフィアのアネモネジェットの性質と影響を調査する.
- 太陽の染色球とコロナの加熱におけるこれらのジェットの潜在的な役割を調査する.
主な方法:
- 太陽の染色球に関するヒノデの観測の分析.
- クロモスフィアのアネモネジェットのサイズ,形,速度の特徴.
主要な成果:
- クロモスフィアのアネモネのジェットはどこにでもあり,通常は長さ2000~5000km,幅150~300kmで,速度10~20km/s.
- これらのジェットは,冠状のX線ジェットを映し出す,逆転したY形を示します.
- 観測された特徴は,磁気再接続がクロモスフィア内の小さな空間スケールで発生することを示唆しています.
結論:
- 小さなスケールでの磁気再接続は,太陽の染色体圏で一般的です.
- この広範囲にわたる小規模な再接続は,太陽の染色球とコロナを温めるための潜在的なメカニズムです.
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