ライマンアルファ放射線によるイオンの共振強化二光子イオン化は,ガス状の星雲の中で行われます
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1Institute of Physics, Lund University, Lund S-221 00, Sweden.
Science (New York, N.Y.)
|February 7, 2001
まとめ
星雲の明るい放射スペクトル線は,共振強化二光子イオン化 (RETPI) によって説明される可能性があります. このメカニズムは,強烈なHライマンアルファ放射線によって駆動され,光学的に厚い星雲の中でイオンを効率的に形成します.
科学分野:
- 天体物理学 天体物理学
- 原子・分子物理学 原子・分子物理学
- ネブラー物理学 ネブラー物理学
背景:
- 明るい星の近くにある星雲は,高興奮温度を示す放射スペクトル線を示している.
- これらの高興奮イオンの形成の正確なメカニズムは,天体物理学における長年の謎でした.
研究 の 目的:
- 星雲のための新しいイオン形成機構を提案し,調査する.
- 星雲環境で観測される明るい放射スペクトル線の起源を説明するために.
主な方法:
- 共振強化二フォトンイオン化 (RETPI) によるイオン形成の理論モデリング.
- 光学的に厚い星雲に閉じ込められたHライマンアルファ放射線の分析.
- 稀化したガス媒体のイオン化と再結合率の計算.
主要な成果:
- 強烈で閉じ込められたHライマンアルファ放射線によるRETPIは,観測されたスペクトル線を生成するための有効なメカニズムです.
- 提案されているイオン化プロセスは,稀な nebular 条件で十分に迅速です.
- フォトイオンは,強化されたHe iおよびHe ii放射線によって触媒化されたRETPIをさらに受けることができます.
結論:
- 共振強化の2光子イオン化は,星雲の高興奮スペクトル線の説得力のある説明を提供します.
- 十分なヘリウムの存在は,二次RETPIを通じてイオン形成プロセスを強化します.
- このメカニズムは,星雲の化学と物理学の新しい理解を提供します.
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