細粒子のコンドリート型フィロシリケートの nebular 起源である

Fred J Ciesla¹, Dante S Lauretta, Barbara A Cohen

¹Department of Planetary Sciences, Lunar and Planetary Laboratory, University of Arizona, 1629 East University Boulevard, Tucson, AZ 85721, USA. fciesla@lpl.arizona.edu

Science (New York, N.Y.)

|January 25, 2003

まとめ

CMコンドライトのフィロシリケートは,太陽星雲の衝撃波によって急速に形成された可能性があり,ゆっくりとしたガス-固体反応ではありません. これは,同時にコンドルルとリム形成を説明する.

科学分野:

惑星科学は惑星科学である.
宇宙化学 (コスモケミストリー)
ミネラロジーは,鉱物学です.

背景:

水分化された鉱物,特にフィロシリケートは,CMコンドライトのコンドルールの周りの増殖リムに含まれています.
以前のモデルでは,初期の太陽星雲における標準的なガス-固体反応によってこれらのフィロシリケートの形成が疑問視されていた.

研究の目的:

コンドルル・リムにおけるフィロシリケートの急速な形成のための新しいモデルを提案する.
コンドルルの同時形成と,その細粒子の増殖縁の形成を説明するために.

主な方法:

太陽の星雲の凍った領域でコンドルを形成する衝撃波によって生み出される条件を調査する.
衝撃を受けた星雲環境の中で鉱物水分化と冷却の時間スケールを分析する.

主要な成果:

凍った星雲の領域における衝撃波は,鉱物の急速な水分化に有利な条件を作り出すことができます.
フィロシリケート形成の計算された時間スケールは,水素化の安定から水氷の凝縮までの冷却期間と一致しています.

結論:

コンドルルを形成する衝撃波は,CMコンドライトの縁の急速な水分化とフィロシリケートの形成のための有効なメカニズムを提供します.
この衝撃波のシナリオは,コンドルーラとその増積輪の共同形成について一貫した説明を提供します.

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