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Updated: May 5, 2026
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Measuring the Densities of Aqueous Glasses at Cryogenic Temperatures
Published on: June 28, 2017
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初期の火星の水溶液の凍結に対する安定性
Alberto G Fairén1, Alfonso F Davila, Luis Gago-Duport
1Space Science and Astrobiology Division, NASA Ames Research Center, Moffett Field, California 94035, USA. alberto.g.fairen@nasa.gov
Nature
|May 22, 2009
まとめ
火星の塩水流体は,非常に低い温度でも液体として残ることができ,火星の水活動を説明する可能性がある. これにより,寒い惑星で水分化ミネラルが広範囲に存在するというパラドックスが解消される.
科学分野:
- 惑星科学は惑星科学である.
- 地質化学 地質化学
背景:
- 火星の特徴は,過去に液体の水があったことを示唆しますが,その表面は現在あまりにも冷たいです.
- 火星の地球平均気温は,純粋な水 (273 K) の凍結点以下です.
- 既存の気候モデルは,表面温度が液体の水にとって十分温かいことを説明するのに苦労しています.
研究 の 目的:
- 火星上の液体の水の維持における溶解液体の役割を調査する.
- 玄武岩気象から派生した火星の液体の凍結と蒸発をモデル化するために.
主な方法:
- バサルトの気象と着陸場所のデータに基づいて,火星の液体の組成をシミュレートした.
- これらの流体の凍結と蒸発プロセスをモデル化しました.
- 結果的に得られる鉱物組成を分析した.
主要な成果:
- 玄武岩から派生した溶液を含む火星の液体は,273K以下の温度でも液体として残ります.
- モデル化された鉱物組成は,火星の表面で観測されたものと一致しています.
- これは,塩素の火星の液体の凍結に対する安定性を示しています.
結論:
- 火星の水に溶けた塩は凍結点を低下させ,液体の水の存在を可能にします.
- これは,初期の火星の気候パラドックスへの解決策を提供します.
- 火星の景色全体に水分化および蒸発性鉱物の存在を説明します.
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