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Updated: Feb 7, 2026
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GPI Anchoring of Proteins in the ER Membrane
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月の潮回転形と,極地移動の証拠
Ian Garrick-Bethell1, Viranga Perera2, Francis Nimmo3
11] Department of Earth and Planetary Sciences, University of California, Santa Cruz, 1156 High Street, Santa Cruz, California 95064, USA [2] School of Space Research, Kyung Hee University, 1 Seocheon-dong, Giheung-gu, Yongin-si, Gyeonggi-do 446-701, Korea.
Nature
|August 1, 2014
まとめ
月の形状は,初期の潮の加熱と,後に凍った潮の膨らみによって説明されます. この過程により,月の極軸は時間とともに大きく変化した.
科学分野:
- 月面地質学と地球物理学
- 惑星科学は惑星科学である.
- ジオダイナミクスは地力学です.
背景:
- 月の大規模地形の起源は,その地質学,軌道進化,方向性を理解するために重要です.
- 以前の仮説には,後期増殖,衝撃,潮効果,およびコンベクションが含まれるが,大きな盆地では分析が複雑になる.
研究 の 目的:
- 月の大規模な地形と重力の球体ハーモニクスを主要な盆地の外で推定するために.
- 月の形状と地質学的歴史に関する仮説を検証する.
主な方法:
- 月の地形と重力の球体ハーモニクスの分析,大きな衝撃盆地を除く.
- 潮加熱と潮回転膨張効果のモデリング.
主要な成果:
- 度2の地形は,地殻形成中の初期の潮加熱と主に一致しています.
- 度2の地形図の二次成分は, ~32の地球半径で凍結した潮回転の膨らみと一致する.
- 内部密度のコントラストは,月の極軸を36 ± 4°で方向転換させた.
結論:
- 月の形状は,初期の潮の加熱と,後に凍った潮の膨らみによる組み合わせによって最もよく説明されます.
- これらのプロセスは,月の地質を結びつけ,月の形状,重力,極地移動の歴史に関する疑問を解決します.
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