Isolated and dynamical black hole mergers with B-POP: the role of star formation and dynamics, star cluster evolution, natal kicks, mass and spins, and hierarchical mergers

被引：22

作者：

Sedda, Manuel Arca ^{[1
,2
,3
]}

Mapelli, Michela ^{[2
,4
,5
]}

Benacquista, Matthew ^{[6
]}

Spera, Mario ^{[7
,8
,9
]}

机构：

[1] Gran Sasso Sci Inst GSSI, I-67100 L'Aquila, Italy

[2] Univ Padua, Phys & Astron Dept Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy

[3] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Monchhoofstr12-14, D-69120 Heidelberg, Germany

[4] INFN Padova, Via Marzolo 8, I-35131 Padua, Italy

[5] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[6] Univ Texas Rio Grande Valley Emeritus, Box 2044, Red Lodge, MT 59068 USA

[7] Scuola Int Super Avanzati SISSA, Via Bonomea 265, I-34136 Trieste, Italy

[8] INFN Trieste, Via Valerio 2, I-34127 Trieste, Italy

[9] IFPU Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 520卷 / 04期

基金：

欧洲研究理事会;

关键词：

gravitational waves; black holes; stellar evolution; star clusters; globular clusters; galaxies: nuclei; GALACTIC NUCLEI; NEUTRON-STAR; POPULATION SYNTHESIS; COMPACT BINARIES; RATE DENSITY; MILKY-WAY; YOUNG; ORIGIN; METALLICITY; GALAXIES;

D O I：

10.1093/mnras/stad331

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The current interpretation of LIGO-Virgo-KAGRA data suggests that the primary mass function of merging binary black holes (BBHs) at redshift z ? 1 contains multiple structures, while spins are relatively low. Theoretical models of BBH formation in different environments can provide a key to interpreting the population of observed mergers, but they require the simultaneous treatment of stellar evolution and dynamics, galaxy evolution, and general relativity. We present B-POP , a population synthesis tool to model BBH mergers formed in the field or via dynamical interactions in young, globular, and nuclear clusters. Using B-POP , we explore how black hole (BH) formation channels, star cluster evolution, hierarchical mergers, and natal BH properties affect the population of BBH mergers. We find that the primary mass distribution of BBH mergers extends beyond M-1 ? 200 M-?, and the ef fecti ve spin parameter distribution hints at different natal spins for single and binary BHs. Observed BBHs can be interpreted as members of a mixed population comprised of similar to 34 per cent (66 per cent ) isolated (dynamical) BBHs, with the latter likely dominating at redshift z > 1. Hierarchical mergers constitute the 4 . 6 -7 . 9 per cent of all mergers in the reference model, dominating the primary mass distribution beyond M-1 > 65 M-?. The inclusion of cluster mass-loss and expansion causes an abrupt decrease in the probability for mergers beyond the third generation to occur. Considering observational biases, we find that 2 . 7 -7 . 5 per cent of mock mergers involve intermediate-mass black hole (IMBH) seeds formed via stellar collisions. Comparing this percentage to observed values will possibly help us to constrain IMBH formation mechanisms.

引用

页码：5259 / 5282

页数：24

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