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 Tools annual

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 Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Observations suggest that star clusters often form in binaries or largerbound groups. Therefore, mergers between two clusters are likely to occur. Ifthese clusters both harbor an intermediate-mass black hole (IMBH; 10^{2-4}Msun) in their center, they can become a strong source of gravitational waveswhen the black holes merge with each other. In order to understand thedynamical processes that operate in such a scenario, one has to study theevolution of the merger of two such young massive star clusters, and morespecifically, their respective IMBHs. We employ the direct-summation Nbody4numerical tool on special-purpose GRAPE6 hardware to simulate a merger of twostellar clusters each containing 63,000 particles and a central IMBH. Thisallows us to study accurately the orbital evolution of the colliding clustersand the embedded massive black holes. Within ~7 Myr the clusters have mergedand the IMBHs constitute a hard binary. The final coalescence happens in ~10^8yrs. The implication of our analysis is that intermediate-mass black holesmerging as the result of coalescence of young dense clusters could provide asource for the Laser Interferometer Space Antenna (LISA) space-basedgravitational wave detector mission. We find that interactions with starsincrease the eccentricity of the IMBH binary to about 0.8. Although the binarylater circularizes by emission of gravitational waves, the residualeccentricity can be detectable through its influence on the phase of the wavesif the last few years of inspiral are observed.Comment: Accepted for publication ApJ Letts. (the abstract shown below has  been shortened

Intermediate-Mass Black Holes in Colliding Clusters: Implications for Lower Frequency Gravitational-Wave Astronomy