太陽風の流出とクロモスフィアの磁気ネットワーク

Hassler¹, Dammasch, Lemaire

¹Southwest Research Institute, 1050 Walnut Street, Boulder, CO 80302, USA. Max-Planck-Institut fur Aeronomie, D-37191 Katlenburg-Lindau, Germany. Institut d'Astrophysique Spatiale, Unite Mixte CNRS- Universite Paris XI, 91405 Orsay, France. Ins.

Science (New York, N.Y.)

|February 5, 1999

まとめ

太陽風は,クロモスフィアの磁気ネットワークと結びついた,冠状の穴の特定の領域から発生します. これらの発見は,太陽風の理解を向上させる.

科学分野:

ソーラー物理学ソーラー物理学
ヘリオフィジックスヘリオフィジックス
プラズマ物理学プラズマ物理学

背景:

冠状孔は,太陽の冠状に開いた磁場線の領域である.
太陽風の起源を理解することは,宇宙天候の予測に極めて重要です.
以前の観測では,冠状の底部での速度の詳細なマッピングが欠けていました.

研究の目的:

コロナの根底にある流出速度と磁気構造の関係を調査する.
太陽風の特定の源地域を特定するために.
冠状動力の理解を深めるために.

主な方法:

太陽と熱球天文台 (SOHO) の宇宙船を利用した.
770アングストームの共鳴線を使用してNe7+の速度マップを作成しました.
染色球磁気ネットワーク構造と相関する流出速度.

主要な成果:

冠状孔の流出速度は,染色球磁気ネットワークとの明確な関係を示しています.
太陽風は,磁気ネットワーク細胞の境界線と交差点に沿った局所的な領域から発生しているようです.
このネットワーク構造と関連した大きな流出速度シグネチャが観察されました.

結論:

太陽風は,冠状の底にある染色球磁気ネットワークに根付いている.
磁気ネットワークの境界に沿った局所化された領域は,太陽風の主要な源領域です.
これらの発見は,太陽風の起源のダイナミクスに関する新しい洞察を提供します.

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