期刊
PHYSICAL REVIEW D
卷 100, 期 4, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.100.043027
关键词
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资金
- Pappalardo Postdoctoral Fellowship at MIT
- NASA [NNX14AP92G]
- NSF at Northwestern University [AST-1716762]
- Ramon y Cajal Programme of the Ministry of Economy, Industry and Competitiveness of Spain
- COST Action GWverse [CA16104]
- Kavli Foundation
- DNRF
- NSF [PHY-1607611]
When two black holes merge in a dense star cluster, they form a new black hole with a well-defined mass and spin. If that second-generation black hole remains in the cluster, it will continue to participate in dynamical encounters, form binaries, and potentially merge again. Using a grid of 96 dynamical models of dense star clusters and a cosmological model of cluster formation, we explore the production of binary black hole mergers where at least one component of the binary was forged in a previous merger. We create four hypothetical universes where every black hole born in the collapse of a massive star has a dimensionless Kerr spin parameter, chi(birth), of 0.0, 0.1, 0.2, or 0.5. We show that if all stellar-born black holes are nonspinning (chi(birth) = 0.0), then more than 10% of merging binary black holes from clusters have components formed from previous mergers, accounting for more than 20% of the mergers from globular clusters detectable by LIGO/Virgo. Furthermore, nearly 7% of detectable mergers would have a component with a mass greater than or similar to 55 M-circle dot, placing it clearly in the mass gap region where black holes cannot form from isolated collapsing stars due to the pulsational-pair instability mechanism. On the other hand, if black holes are born spinning, then the contribution from these second-generation mergers decreases, making up as little as 1% of all detections from globular clusters when chi(birth) = 0.5. We make quantitative predictions for the detected masses, mass ratios, and spin properties of first- and second-generation mergers from dense star clusters, and show how these distributions are highly sensitive to the birth spins of black holes.
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