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Updated: Jun 24, 2026

06:14
Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface
Published on: July 30, 2020
アルフヴェン波は,太陽の下層大気圏にある
David B Jess1, Mihalis Mathioudakis, Robert Erdélyi
1Astrophysics Research Centre, School of Mathematics and Physics, Queen's University, Belfast, BT7 1NN, Northern Ireland, UK. d.jess@qub.ac.uk
まとめ
科学者たちは,太陽の大気中のアルフヴェン波を検出し,明るい点から発生しました. これらのトルション振動は,太陽のコロナを温めるためのメカニズムを提供し,太陽物理学の長年の謎である.
科学分野:
- 太陽物理 太陽物理学
- プラズマ天体物理学とは
- 星の大気の動態 星の大気の動態
背景:
- 太陽の大気中のエネルギー流と加熱を駆動するメカニズムは,未だに十分に理解されていない.
- 振動現象の調査は,エネルギー輸送プロセスに関する洞察を提供します.
研究 の 目的:
- 太陽の大気中の振動現象を検知し,特徴づけること.
- エネルギー伝送と冠状熱の原因となる波形を特定する.
主な方法:
- 巨大な太陽の明るい点群に関連した振動現象の波紋分析.
- 振動振幅,周期,ドップラー速度を測定する.
- 波の様子を排除するために,強度の振動と横断の位移の分析.
主要な成果:
- 126秒から700秒までの周期と2.6 km/sの振幅を持つ振動の検出.
- 振動は染色球のドップラーシフト (平均23 km/sのブルーシフト) と結合している.
- グローバル誘導を示す,+/-22度の回転と180度の相移転を持つトルションアルフヴェン波の識別.
結論:
- 検出されたトルションアルフヴェン波は,太陽の大気中の重要なエネルギー輸送メカニズムです.
- これらの波からのエネルギーの流れは,太陽の冠状熱を説明するのに十分である.
- この発見は,冠状熱の長年の問題に対する潜在的な解決策を提供します.
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