太陽の磁気流の輸送は,太陽の磁気流の輸送である

Y M Wang, A G Nash, N R Sheeley

Science (New York, N.Y.)

|August 18, 1989

まとめ

太陽の磁気流は,太陽の斑点帯から分散し,太陽の最小値に近い強力な極域を形成します. このプロセスは,コンベクションと循環によって駆動され,惑星間磁場と冠状孔の観測によってサポートされています.

科学分野:

太陽物理太陽物理学
マグネトヒドロダイナミクス
プラズマ物理学のプラズマ物理学

背景:

太陽の磁気流は,低緯度の太陽斑帯から発生する.
超粒子のコンベクションとメリディアン循環は,この流れを緯度を越えて分散させます.
太陽の11年周期が磁場分布に影響する.

研究の目的:

太陽光輸送プロセスが極の磁場をどのように形作るのかを調査する.
極域の"トップノート"構造の形成を理解するために.
シミュレートされた輸送を,太陽最小値に近い観測証拠と結びつけるため.

主な方法:

太陽磁気流体輸送の数値シミュレーションを用いて.
コンベクティブ運動とメリディアン循環の相互作用をモデル化.
シミュレーション結果を惑星間磁場と極性冠状孔のデータと比較する.

主要な成果:

シミュレーションでは,フクロス分散が強い極域に繋がっていることが示されています.
"トップノート"の極域構造は,モデルによって再現されています.
シミュレートされた拡散とフローレットは,観測された太陽磁場特性と一致しています.

結論:

太陽光輸送プロセスは,極の磁場を生成するために不可欠です.
このモデルは,太陽の最小値に近い強力な極域の観測証拠を裏付けている.
これらの輸送メカニズムを理解することは,太陽のサイクル予測の鍵です.

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