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Updated: Jul 11, 2026

11:34
Scattering And Absorption of Light in Planetary Regoliths
Published on: July 1, 2019
まとめ
近赤外線スペクトルは,金星の夜側からの熱放出の違いを明らかにしています. 雲の頂上の下の水蒸気の変動は,特定の波長におけるコントラストの減少を説明する可能性がある.
科学分野:
- 惑星科学は惑星科学である.
- 大気科学 大気科学
- スペクトル顕微鏡検査です.
背景:
- 金星の夜側には,明るい (熱い) と暗い (冷たい) 斑点を含む熱放出の特徴があります.
- 大気の組成と動態を理解することは,金星の探査に不可欠です.
研究 の 目的:
- 金星の夜側の熱的特徴の近赤外線スペクトルを分析するために.
- 観測されたスペクトルコントラストの原因と大気組成への影響を調査する.
主な方法:
- 1200×1500のスペクトル解像度を持つ近赤外線スペクトル (2.2×2.5ミクロメートル) の取得
- 二酸化炭素 (CO2),一酸化炭素 (CO),水蒸気などのガスからの吸収帯の分析.
- 硫酸 (H2SO4) の雲を含む絶滅源の調査.
主要な成果:
- 明るいと暗い両方の特徴は,CO2,CO,水蒸気からの吸収帯を示した.
- 熱点と冷点の間の最大のスペクトルコントラストは,H2SO4雲とCO2帯に起因する2.21〜2.32マイクロメートルの間で発生しました.
- CO,雲,水蒸気吸収/散乱による波長>2.34マイクロメートルでのコントラスト減少 (5565%) が観察されました.
結論:
- 観測されたコントラストの減少は,金星の雲の頂上より下にある水蒸気濃度の潜在的な水平変動を示唆しています.
- スペクトル観測データは,金星の夜側における大気異質性の証拠を提供します.
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