English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Eccentric mergers are a signature of the dynamical formation channel ofbinary black holes (BBHs) in dense stellar environments and hierarchical triplesystems. Here, we investigate the production of eccentric mergers viabinary-single interactions, by means of $2.5\times10^{5}$ direct$\textit{N}$-body simulations. Our simulations include post-Newtonian terms upto the 2.5th order and are designed to reflect the environmental conditions ofyoung (YSCs), globular (GCs), and nuclear star clusters (NSCs). We find that$0.6\%$ ($1\%$) of the mergers in NSCs (GCs) reach the coalescence witheccentricity ${>0.1}$, while in YSCs only $0.08\%$ of the mergers is eccentric.Approximately $\sim63\%$ of these events are produced by chaotic, resonantinteractions where temporary binaries are continuously formed and destroyed,while $\sim31\%$ arise from prompt interactions where two black holes (BHs)merge almost radially. Lastly, $\sim 6\%$ of these eccentric mergers occur intemporary hierarchical triples. Binaries undergoing a flyby generally developsmaller tilt angles with respect to exchanges, with the distribution that peaksat $\sim15^{\circ}$ for the former, and $\sim90^{\circ}$ for the latter. Thisresult challenges the idea that dynamics produces perfectly isotropic spinorientations. We further study the impact of the host star cluster on thepopulation of BBH mergers. The environment dramatically affects BH retention:$0.8\%$, $12.5\%$, and $36.4\%$ of all the remnant BHs are retained in YSCs,GCs, and NSCs, respectively. The fraction of massive BHs also depends on thehost cluster properties, with pair-instability ($60\leq\,$M$_{\rmBH}$/M$_{\odot}\leq$100) and intermediate-mass (M$_{\rmBH}\geq$100$\,$M$_{\odot}$) BHs accounting for approximately $\sim44\%$ and$1.6\%$ of the mergers in YSCs, $\sim33\%$ and $0.7\%$ in GCs, and $\sim28\%$and $0.4\%$ in NSCs.

Eccentric black hole mergers via three-body interactions in young, globular and nuclear star clusters