アルヴェニク速度のピークと太陽に近い太陽風の回転フロー
J C Kasper1,2, S D Bale3,4,5, J W Belcher6
1Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA. jckasper@umich.edu.
Nature
|December 6, 2019
まとめ
超音速の太陽風の加速は アルフヴェン波によって引き起こされ 構造的な速度スパイクに編成されます これらのピークは 太陽風の重要な回転成分を明らかにし 恒星の角運動量損失の現在のモデルに 挑戦しています
科学分野:
- * ヘリオフィジックスとプラズマ物理学
- * 太陽物理学と恒星の進化
背景:
- * 太陽に近い超音速太陽風の加速は確認されていますが,未確認のエネルギー輸送プロセスによって駆動されています.
- * アルヴェニク波動は,重要なエネルギーを持つコロナと太陽風で観察される候補メカニズムです.
- * 過去の観測は,太陽から遠く,波幅を下回る太陽風の最小回転を示しました.
研究 の 目的:
- * 太陽風のプラズマ動態と太陽中心距離約35のエネルギー輸送を調査する.
- * 太陽風の加速と太陽からのエネルギー輸送に責任のあるプロセスを特定する.
- * 太陽風の流れの回転成分と,恒星の角運動量損失への影響を評価する.
主な方法:
- * ~35太陽半径の太陽中心距離で宇宙船を使用して太陽風プラズマのインシット観測.
- * アルフヴェン波,磁場線,プラズマ流速の分析
- * 観測された回転速度と古典的な予測と波幅の比較
主要な成果:
- * アルフヴェン波は,S型磁場曲線に関連した構造化された速度スパイク (最長数分) に組織されます.
- * 太陽風の流れ速度の重要な回転成分が検出され,ピークは35〜50 km/sでした.
- * 観測された回転フローは,数 km/sの古典的な予測を大幅に上回る.
結論:
- * 発見は,太陽風におけるコロナ循環とエネルギー輸送の既存のモデルに異議を唱える.
- * 重要な自転コンポーネントは,恒星における角運動量喪失のより複雑なメカニズムを示唆しています.
- * これらの過程を理解することは 恒星が時間の経過とともに 角運動力を失い 回転を低下させる仕組みを理解するために 極めて重要です
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