火星の大気中の強い水の同位体異常:現在のと古代の貯水池を調査する
G L Villanueva1, M J Mumma2, R E Novak3
1NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. Catholic University of America, Washington, DC 20064, USA. geronimo.villanueva@nasa.gov.
まとめ
火星は,大気中の水蒸気中の高デウテリウム/水素比によって証明された,かなりの量の水を失いました. 北極の氷は濃縮されているので,初期の火星は,地球全体に相当な水層を持っていたことを示唆しています.
科学分野:
- 惑星科学は惑星科学である.
- 天体生物学 アストロバイオロジー
- 地質化学 地質化学
背景:
- 火星の水の歴史を理解することは,その過去の居住性を評価するために不可欠です.
- デュテリウム/水素 (D/H) の比率は,惑星の天体の水失失の主要なトレーサとして機能する.
研究 の 目的:
- 火星全体で大気中の水 (H2O) とその減塩型 (HDO) をマッピングする.
- デウテリウム濃縮を定量化し,過去の水の豊富さや損失を推測する.
主な方法:
- 世界大気中のH2OとHDOの測定.
- 同位体異常とD/H比の分析.
主要な成果:
- 火星全体で強い同位体異常と著しいD/H濃縮が観測されました.
- 北極帽から昇華する水は,D/H比が地球のVSMOWの7倍を示しています.
- 北極の水の氷はデウテリウムで少なくとも8VSMOWに濃縮されています.
結論:
- 火星は,歴史上,かなりの水の損失を経験してきました.
- 初期の火星 (45億年前) は,少なくとも137メートルの深さの地球規模の水層を持っていた可能性が高い.
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