月面での太陽風記録:惑星の窒素からのプレソラー解読
K Hashizume1, M Chaussidon, B Marty
1Centre de Recherches Pétrographiques et Géochimiques-CNRS, BP 20, 54501 Vandoeuvre-lès-Nancy Cedex, France. kohash@ess.sci.osaka-u.ac.jp
まとめ
太陽風の窒素は月面の規則石に15Nを欠けているが,非太陽系の成分は15Nを濃縮している. これは,星間窒素化合物が惑星の窒素に寄与したことを示唆している.
科学分野:
- 宇宙化学 (コスモケミストリー)
- 惑星科学 惑星科学
- イソトープ地球化学 イソトープ地球化学
背景:
- 惑星の体内の窒素同位体は,原太陽系のガスから変化を示しています.
- 窒素の起源を理解することは,惑星の形成と進化の鍵です.
研究 の 目的:
- 月面のレゴリットにおける窒素の同位体組成を調べるために.
- 惑星の物質における窒素の起源を決定する.
主な方法:
- 月面のレゴリット粒子のイオンマイクロプローブ分析.
- 異なるレゴリット成分における窒素と水素同位体の分析.
主要な成果:
- 太陽風の窒素は,月面のレゴリットに15Nで,地球の大気と比較して少なくとも24%減少しています.
- デウテリウム豊富な水素に関連した非太陽性窒素成分は,15N濃縮を示しています.
- 地球上の惑星や隕石は,原太陽系のガスと比較して15Nの体系的な濃縮を示しています.
結論:
- 単純な星雲や惑星の分割は,観測された15N濃度を説明することはできません.
- 星間起源の可能性がある15N豊富な化合物は,惑星の窒素に寄与したに違いない.
- これらの星間化合物は,15Nが欠乏した原太陽星雲とバランスをとっていないかもしれません.
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