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鉱物学とヴェスタ全土におけるその多様性のスペクトロスコープによる特徴づけ
M C De Sanctis1, E Ammannito, M T Capria
1Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy. mariacristina.desanctis@iaps.inaf.it
Science (New York, N.Y.)
|May 15, 2012
まとめ
ヴェスタ・ヴェスタ ヴェスタ・ヴェスタ
科学分野:
- 惑星科学 惑星科学
- アステロイド鉱物学とは
- 宇宙地化学 宇宙地化学
背景:
- ヴェスタは,内部が異なる大きな小惑星です.
- その表面の構成は主にハワードライト・ユークリット・ダイオゲニット (HED) 隕石と関係しています.
- ヴェスタの鉱物学を理解することは,初期の太陽系プロセスについての洞察を提供します.
研究 の 目的:
- 小惑星ヴェスタの鉱物学を,ドーン宇宙船からのデータを用いて分析する.
- ヴェスタの表面構成における地域的および局所的な変動を調査する.
- ヴェスタの地質史とマグマの進化を理解する.
主な方法:
- Dawn宇宙船からの可視および赤外線スペクトロメーターデータの分析.
- ヴェスタの表面上の鉱物学的構成要素のスペクトロスコープによる識別.
- 既知の隕石組成とスペクトルデータの相関.
主要な成果:
- ベスタの鉱物学は,HED隕石と一致しています.
- 異なる鉱物学的領域が特定され,レアシルビア盆地におけるより高い二酸化成分と赤道地域におけるより高いユークリット成分を含む.
- クレーター壁や噴出物で観測された鉱物学的層構造の証拠.
結論:
- ヴェスタの地殻は,上部ユークリト層と,より深いダイオジニト層で構成されており,レアシルビアの影響で露出しています.
- スペクトルの変動性は,エウクリト基岩とピロキセンの累積物の複雑な地殻組成を示唆しています.
- ヴェスタは複雑なマグマの進化を示しており,その結果,地殻とマントルが分化しています.
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