シミュレーションにより,球状星団における中質量ブラックホールの形成が予測される
Michiko S Fujii1, Long Wang2, Ataru Tanikawa3
1Department of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan.
Science (New York, N.Y.)
|May 30, 2024
まとめ
球状星団は,太陽の質量1000倍を超える中等質量ブラックホール (IMBH) を形成することができる. 高密度の星形成は,重力波の反発を克服するために十分な合併を可能にし,IMBH保持を可能にします.
科学分野:
- 天体物理学
- スター進化
- ブラックホール形成
背景:
- 中等質量ブラックホール (IMBHs, 100105 M) の起源は,天体物理学において重要な議論となっている.
- 球状星団 (GC) は,恒星残骸と恒星の合併によって形成されたIMBHをホストすると仮定されている.
- 以前のシミュレーションでは,重力波の反発により,GCにおけるIMBH形成は<500M>に制限されていることが示唆された.
研究 の 目的:
- 球状星団が以前にシミュレートされた質量制限を超えたIMBHを形成する可能性を調査する.
- GC形成環境が,放出値を超えてIMBHの成長を容易にするかどうかを判断する.
主な方法:
- 球状星団の形成を 詳細に星ごとにシミュレーションした.
- 巨大な分子雲の内部で 高密度の恒星形成が 恒星融合やブラックホールの成長に及ぼす影響をモデル化しました
主要な成果:
- 親の巨大分子雲の内部にある 高密度の恒星形成環境は 十分な質量の恒星の合併を促すことができる.
- これらの合併は,以前はGCでIMBHの形成を制限していた質量上限を超えることができます.
- シミュレーションでは,103Mを超えるIMBHを形成する可能性を示しています.
結論:
- 球状星団は 巨大な中等質量ブラックホールの形成に適した環境です
- GC形成の初期の高密度条件は,重力波の反転制限を克服するために不可欠です.
- GCの中で形成されたIMBHは,大きな反転キックでも重力的に縛られるのに十分な質量を達成できます.
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