ユリセスの太陽風のプラズマ観測は,南緯度の高い地点で観測された
Science (New York, N.Y.)
|May 19, 1995
まとめ
ユリセス宇宙船のデータは,高速の太陽風の流れと,中緯度の相互作用領域を明らかにしています. 太陽のより高い緯度では,陽子の温度が上昇し,より広い電子線が広がり,複雑な太陽風構造を示した.
科学分野:
- 宇宙物理学 宇宙物理学
- プラズマ物理学 プラズマ物理学
- ヘリオフィジックス ヘリオフィジックス
背景:
- 太陽風は,太陽の上層大気から放出される電荷の粒子の連続した流れです.
- 高緯度における太陽風の振る舞いを理解することは,宇宙天候の予測に極めて重要です.
研究 の 目的:
- 太陽風のプラズマ観測をユリセス宇宙船から,太陽の南極の高緯度でまとめます.
- 未知の地域における太陽風の構造と性質を特徴づけること.
主な方法:
- ユリセス宇宙船によって収集されたインシトゥプラズマデータの分析.
- 高速流,相互作用領域,冠状質量放出など,太陽風の特徴を追跡する.
主要な成果:
- 繰り返し発生する高速流とコローテーション相互作用領域は,中緯度で支配的であった.
- 太陽風の速度は700〜800km/sに達し,極方向は -35°Cでした.
- 高緯度では,陽子の温度が上昇し,電子線が広がった.
- 圧縮,圧力バランス,アルフェニック構造は,高緯度の太陽風で観察されました.
結論:
- 高緯度の太陽風は,低緯度の太陽風と比較して独特な特性を発揮します.
- ヘリオマグネティックストリーマーベルトの傾きは,太陽風の衝撃の持続に影響します.
- ユリセスのデータは,太陽風の3次元構造に関する貴重な洞察を提供します.
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