メリディナルプラズマの流れの変動によって引き起こされる異常な最小の太陽斑サイクル23です
Dibyendu Nandy1, Andrés Muñoz-Jaramillo, Petrus C H Martens
1Department of Physical Sciences, Indian Institute of Science Education and Research, Kolkata, Mohanpur 741252, West Bengal, India. dnandi@iiserkol.ac.in
Nature
|March 4, 2011
まとめ
太陽力ダイナモのシミュレーションにより,周期の初期により速い速度,後でより遅い速度を持つプラズマフローの特定のパターンが,弱い極場を持つ長期間の太陽最小値を説明することを明らかにしました. この発見は,太陽の活動とその地球への影響を予測するのに役立ちます.
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
- 天体物理学 天体物理学
背景:
- 太陽の斑点の活動は,最大値と最小値の周期的なサイクルを示します.
- 太陽斑のサイクル23に続く最小値は,極の弱い磁場と多数の太陽斑のない日によって特徴づけられ,異常に長かった.
研究 の 目的:
- 太陽の極域の再生を司るダイナモメカニズムを調査する.
- シミュレーションを用いて,太陽光斑のサイクル23後の長期太陽最小値の特性を説明する.
主な方法:
- 太陽の磁場の動力ダイナモシミュレーションを行いました.
- モデル化されたプラズマフロー,特にメリディオンフローは,太陽のサイクル全体を通して.
主要な成果:
- メリディアン流のパターンは,周期の前半に高速で,次半に遅いもので,太陽斑のサイクル23の観測された特徴を再現した.
- シミュレーションは,非常に深い太陽最小値と弱い極域の間の一般的な相関を示しています.
結論:
- シミュレートされたプラズマフローダイナミクスは,太陽光斑のサイクル23の後に観測された長期間の太陽最小値の妥当な説明を提供します.
- この研究では,太陽最小値の特徴は,極域の強度と関連しており,太陽放射線,太陽風,地球上の宇宙線流に影響を及ぼすことを示唆しています.
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