太陽風の起源は,冠状のフンネルにある
Chuan-Yi Tu1, Cheng Zhou, Eckart Marsch
1Department of Geophysics, Peking University, Beijing 100871, China. cytu@public3.bta.net.cn
まとめ
太陽風は,太陽の冠状孔から発生し,磁気フンネル内の光球より5〜20メガメートルの高さから流出を開始します. この発見は,太陽風の現象を明確にしています.
科学分野:
- * 太陽物理学 太陽物理学
- * プラズマ物理学
- * 天体物理学
背景:
- * 太陽の冠状孔の中の太陽風の正確な起源は,太陽物理学の長年のパズルです.
- *太陽風の発生源を理解することは,宇宙天候の予測と冠動力学の理解に不可欠です.
研究 の 目的:
- * 太陽の冠から太陽風の流出を開始する特定の高度とメカニズムを特定する.
- * イオン行動と磁場構造を相関させ,太陽風の出発点を決定する.
主な方法:
- *様々なイオン (Ne7+,C3+) からのスペクトル線のドップラー速度と放射の相関図.
- * 光球磁気図から無力磁場を異なる高さへ引き算する.
- *磁気ファネルとの関係でイオン放出高度と流出速度を分析する.
主要な成果:
- *太陽風の流出は,磁気フンネルの中で光球より5〜20メガメートルの高さで始まります.
- *Ne7+イオンは約20メガメートルを放射し,流出速度は約10km/sである.
- *C3+イオンは主に5メガメートルの範囲を放射し,平均フロー速度は有意ではない.
結論:
- *太陽風は,太陽のコロナにある磁気ファネル内の特定の高度から発生します.
- * 観測されたイオン行動は,太陽風がこれらの構造の中で外向きの旅を開始するモデルをサポートします.
- *これらの発見に基づいて,太陽風の起源に関する新しいモデルが提案されています.
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