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星の炭素の生産速度と,宇宙における炭素の豊富さ
H Oberhummer1, A Csótó, H Schlattl
1Institute of Nuclear Physics, Vienna University of Technology, Wiedner Hauptstrasse 8-10, A-1040 Vienna, Austria. ohu@kph.tuwien.ac.at
まとめ
宇宙 宇宙 宇宙 宇宙 宇宙 宇宙
科学分野:
- 核天体物理学は,核天体物理学である.
- 恒星の核合成である.
背景:
- 炭素は主に赤い巨星におけるトリプルアルファプロセスによって形成される.
- 正確な反応速度は,宇宙の元素の豊富さを理解するために非常に重要です.
研究 の 目的:
- 基本的な核力の変動に対する炭素生産の感受性を調査する.
- 恒星の炭素と酸素の安定性を決定するために.
主な方法:
- トリプルアルファ反応速度の顕微鏡12核モデルによる計算.
- 変化した反応速度を含む恒星の進化モデル.
- 強い力とクーロン力の変動に対する感度分析.
主要な成果:
- 強い力またはクーロンブ力が観測値からわずかに逸脱すると,炭素と酸素の生成が劇的に減少します (30〜1000倍).
- 狭い窓 (強い力では0.5%,クーロン力では4%) は,重要な炭素/酸素収量に不可欠です.
結論:
- 星の炭素生産は,基本的な核相互作用の正確な強さに非常に敏感です.
- 宇宙における炭素と酸素の観測された豊富さは,これらの力の微調整されたバランスを示唆しています.
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