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高質量 の X 線 の 二つ星 は,超新星 から 誕生 し た
Noel D Richardson1, Clarissa M Pavao2, Jan J Eldridge3
1Department of Physics and Astronomy, Embry-Riddle Aeronautical University, Prescott, AZ, USA. noel.richardson@erau.edu.
Nature
|February 1, 2023
まとめ
極小の超新星,最小の噴出物を持つ珍しい恒星爆発は,二重星系 CPD -29 2176 で確認されています. この発見は 二重星系内の中性子星の形成における その役割を確認しています
科学分野:
- 天文学と天体物理学
- スター進化
- バイナリー星系
背景:
- 超超新星とは 極小の噴出物によって特徴づけられる 巨大な恒星の終末爆発です
- 超大質量バイナリ系から 発生すると考えられています 恒星は外層を伴星に失います
- これらの事象は ニュートロン星形成に起因し 二重星を保存します
研究 の 目的:
- 高質量X線バイナリ CPD-292176の進化史を調査する
- CPD -29 2176の中性子星の構成要素が 超新星によって形成されたかどうかを確認するために
- 二重中性子星の形成における 超新星系とその役割を理解する
主な方法:
- CPD -29 2176 バイナリシステムの軌道要素 (周期と離心率) の分析.
- これらの軌道要素と既知のBe X線バイナリの比較.
- バイナリーシステムの歴史を追跡する 恒星進化モデリング
主要な成果:
- 高質量X線バイナリCPD-292176は,BeX線バイナリに似た軌道特性を有している.
- CPD -29 2176の進化史は,その中性子星の構成要素が超新星によって形成されたことを示しています.
- これは超新星系の祖先の 直接的な証拠です
結論:
- CPD -29 2176は超新星によって形成されたシステムの重要な例です.
- このような祖先系を特定することは 二重中性子星の形成経路を理解するために不可欠です
- 二重中性子星は重元素と重力波の発生に重要な役割を果たしています
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