Simulations predict intermediate-mass black hole formation in globular clusters

• 成果类型: Article
• 署名作者: Fujii, Michiko S.; Wang, Long; Tanikawa, Ataru; Hirai, Yutaka; Saitoh, Takayuki R.
• 署名单位: University of Tokyo; Sun Yat Sen University; Fukui Prefectural University; University of Notre Dame; Tohoku University; Kobe University
• 刊物名称: SCIENCE
• ISSN/ISSBN: 0036-13840
• DOI: 10.1126/science.adi4211
• 发表日期: 2024-06-28
• 页码: 1488-1492
• 关键词: space-telescope evidence; by-star simulations; central kinematics; omega cen; EVOLUTION; catalog; integrator; parameters; algorithm; rotation

摘要

The formation process of intermediate-mass black holes (IMBHs), defined as those between 100 and 10(5) solar masses (M (circle dot)), is debated. One potential origin is the growth of less-massive black holes merging with stars and compact objects within globular clusters (GCs). However, previous simulations have indicated that this process only produces IMBHs under 500 M (circle dot) before gravitational wave recoil ejects them from the GC. We performed star-by-star simulations of GC formation, finding that high-density star formation in a GC's parent giant molecular cloud can produce sufficient mergers of massive stars to overcome that mass threshold. We conclude that GCs can form with IMBHs more than 103 M (circle dot), which is sufficiently massive to be retained within the GC even with the expected gravitational wave recoil.