初期の宇宙における黒洞の種子の急速な成長は,超指数的増殖によるものです
Tal Alexander1, Priyamvada Natarajan2
1Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel. tal.alexander@weizmann.ac.il.
まとめ
超大質量ブラックホール (BHs) は,初期の宇宙では,新しいダイナミックメカニズムによって急速に成長します. このプロセスは,密度の高いガスを持つ恒星群で発生し,エディントン増積の限界を回避し,ビッグバン直後に観測された輝くクエーサーを説明します.
科学分野:
- 天体物理学 天体物理学
- コスモロジー・コスモロジーとは
- ブラックホール物理学 ブラックホール物理学
背景:
- ブラックホール (BH) の成長は,通常,放射線圧が重力引力を均衡させるエディントン比率によって制限されます.
- 標準的なエディントン限定増殖は,観測された超大質量BHsを形成するために遅すぎ,初期の宇宙の輝くクエーサーを動かす.
研究 の 目的:
- 初期の宇宙における超指数的ブラックホールの蓄積のためのダイナミックなメカニズムを提案する.
- 超大質量ブラックホールにシードブラックホールの急速な形成を説明するために,光るクエーサーを動かす超大質量ブラックホールを動かす.
主な方法:
- BHシードが恒星群の中に存在するシナリオを調査する.
- 濃厚で冷たい高不透明ガスの流れにおける蓄積を分析する.
- BHのランダムな動きが蓄積円盤形成に与える影響を検討する.
主要な成果:
- 超指数的増殖を可能にするダイナミックなメカニズムが提案されています.
- 高ガスの不透明性は,増殖放射線を捕捉し,成長の上限を防止します.
- BH星団のランダムな動きは,緩やかな増殖円盤形成を抑制する.
結論:
- 超指数的増加は,超大質量ブラックホールの急速な出現を説明することができます.
- このメカニズムは,初期の宇宙で観測された輝くクエザーのパズルを解決する.
- 提案されたモデルは,恒星質量シードからブラックホールの急速な成長に対する解決策を提供します.
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