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In-situ Tapering of Chalcogenide Fiber for Mid-infrared Supercontinuum Generation
Published on: May 27, 2013
ヘリウムに富んだ伴侶を持つ白矮星からの淡いタイプの超新星です
H B Perets1, A Gal-Yam, P A Mazzali
1Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel. hperets@cfa.harvard.edu
Nature
|May 21, 2010
まとめ
淡い超新星SN 2005Eは,既存のモデルに挑戦しています. その低質量と古い恒星環境は,典型的なコア崩壊またはタイプIア超新星とは異なる,ヘリウムが蓄積する白矮星からの新しい起源を示唆しています.
科学分野:
- 天文学と天体物理学について
- 恒星の進化について
- 超新星物理学 超新星物理学
背景:
- 超新星は,巨大な星の核の崩壊 (タイプIb/c,II) または白矮星の爆発 (タイプIa) から発生します.
- タイプIa超新星は,若い恒星環境と古い恒星環境の両方で発生します.
- 核崩壊超新星は,若い恒星集団と関連しています.
研究 の 目的:
- 弱いタイプIb超新星であるSN 2005Eの起源を調査する.
- SN 2005Eが既定の超新星形成モデルに適合するかどうかを判断する.
主な方法:
- 銀河NGC 1032の古い恒星環境におけるSN 2005Eの位置の分析.
- 射出物の組成と速度を判定するためのスペクトル観測.
- 射出された物質の質量推定.
主要な成果:
- SN 2005Eは,非常に低い噴出質量 (約0.3太陽質量) を表しています.
- エジェクトの組成は,ヘリウム燃焼産物,高速で支配されています.
- 超新星環境は古い恒星集団であり,核崩壊と矛盾しています.
- カルシウムの豊富さは典型的な超新星よりも高く,放射性44Tiが存在する可能性が高い.
結論:
- SN 2005Eの特徴は,核崩壊の起源を強く否定しています.
- 射出物の構成により,亜光または通常のタイプIア超新星である可能性は低い.
- 最も妥当な起源は,低質量で古い祖先であり,おそらくバイナリ系におけるヘリウムを蓄積する白矮星である.
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