Properties of black hole-star binaries formed in N-body simulations of massive star clusters: implications for Gaia black holes

被引：2

作者：

Fantoccoli, Federico ^{[1
,2
]}

Barber, Jordan ^{[1
]}

Dosopoulou, Fani ^{[1
]}

Chattopadhyay, Debatri ^{[1
]}

Antonini, Fabio ^{[1
]}

机构：

[1] Cardiff Univ, Grav Explorat Inst, Sch Phys & Astron, Cardiff CF24 3AA, Wales

[2] Univ Milano Bicocca, Dept Phys G Occhialini, Piazza Sci 3, I-20126 Milan, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2025年 / 538卷 / 01期

基金：

英国科学技术设施理事会;

关键词：

methods: numerical; stars: black holes; stars: kinematics and dynamics; globular clusters: general; galaxies: star clusters: general; ORBITAL EVOLUTION; MECHANISM; CATALOG; SYSTEM;

D O I：

10.1093/mnras/staf303

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We investigate black hole-star binaries formed in N-body simulations of massive, dense star clusters. We simulate 32 clusters with varying initial masses (10(4) M-circle dot to 10(6) M-circle dot), densities (1200 M(circle dot)pc(-3) to 10(5) M-circle dot pc(-3)), and metallicities (Z=0.01,0.001,0.0001). Our results reveal that star clusters produce a diverse range of BH-star binaries, with dynamical interactions leading to extreme systems characterized by large orbital separations and high black hole masses. Of the ejected BH-main sequence (BH-MS) binaries, 20 per cent form dynamically, while the rest originate from the primordial binary population initially present in the cluster. Ejected BH-MS binaries that are dynamically formed have more massive black holes, lower-mass stellar companions, and over half are in a hierarchical triple system. All unbound BH-giant star (BH-GS) binaries were ejected as BH-MS binaries and evolved into the BH-GS phase outside the cluster. Due to their lower-mass companions, most dynamically formed binaries do not evolve into BH-GS systems within a Hubble time. Consequently, only 2 of the 35 ejected BH-GS binaries are dynamically formed. We explore the formation pathways of Gaia-like systems, identifying two Gaia BH1-like binaries that formed through dynamical interactions, and two Gaia BH2-like systems with a primordial origin. We did not find any system resembling Gaia BH3, which may however be attributed to the limited sample size of our simulations.

引用

页码：243 / 257

页数：15

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