急激に成長する銀河前ガスの雲の中で巨大なブラックホールの形成
John H Wise1, John A Regan2, Brian W O'Shea3,4
1Center for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, Atlanta, GA, USA. jwise@gatech.edu.
Nature
|January 25, 2019
まとめ
初期の巨大なブラックホールの形成は 放射線だけではなく 構造の形成のダイナミクスによって引き起こされます シミュレーションによると 超大質量恒星は 金属のないハローで 急速なガスの成長で 形成されることが示されており ブラックホールの種子が以前考えられていたよりも 多いことを示唆しています
科学分野:
- 宇宙学と天体物理学
- 初期の宇宙 の 銀河 形成
- ブラックホールの形成メカニズム
背景:
- 銀河の中心にある超大質量ブラックホール (SMBH) の起源は,天体物理学における重要な課題である.
- 巨大な恒星から形成された直接崩壊ブラックホール (approx. 理想的な種子候補として提案されています.
- 初期の宇宙におけるこれらの直接崩壊ブラックホールの存在,形成環境,および希少性は議論されています.
研究 の 目的:
- 超大質量星の形成に必要な条件を調査し,SMBHの潜在的な種となる.
- 放射性水力学シミュレーションを用いて 初期の巨大なブラックホールの種子の形成をモデル化する.
- 初期の宇宙における 巨大なブラックホールの形成の主な要因を 特定するためです
主な方法:
- 初期の銀河形成の 放射線水力学シミュレーションを行いました
- 金属のないハローに重点を置いて 質量が高い 初期恒星核を形成する
- 超大質量恒星形成に対するライマン=ヴェルナー放射の強度と急速な質量増加の影響を分析した.
主要な成果:
- シミュレーションにより,超大質量恒星を形成するのに十分な質量と転落率を持つ金属のないハローが生成されました.
- 理想的な環境では,ライマン・ワーナー強度 ~3倍の背景放射と少なくとも1つの急速な質量増加期が必要である.
- 急速なガスの増加はダイナミックな加熱を誘導し,近くの銀河からのライマン・ワーナー抑制を強める.
結論:
- 構造形成のダイナミクスは 臨界ライマン=ヴェルナー流ではなく 初期の大量ブラックホール形成の主な原動力です
- 超大質量恒星の形成は,急速なハロの成長とダイナミックな加熱によって促進され,放射線フィードバックを克服します.
- 巨大なブラックホールの種は,超密度の初期の宇宙地域 (数密度は10^-3 Mpc^-3まで) で著しく一般的です.
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