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Investigations of elemental abundances in the ancient and most metaldeficient stars are extremely important because they serve as tests of variablenucleosynthesis pathways and can provide critical inferences of the type ofstars that lived and died before them. The presence of r-process elements in ahandful of carbon-enhanced metal-poor (CEMP-r) stars, which are assumed to beclosely connected to the chemical yield from the first stars, is hard toreconcile with standard neutron star mergers. Here we show that the productionrate of dynamically assembled compact binaries in high-z nuclear star clusterscan attain a sufficient high value to be a potential viable source of heavyr-process material in CEMP-r stars. The predicted frequency of such events inthe early Galaxy, much lower than the frequency of Type II supernovae but withsignificantly higher mass ejected per event, can naturally lead to a high levelof scatter of Eu as observed in CEMP-r stars.

Compact Stellar Binary Assembly in the First Nuclear Star Clusters and r-Process Synthesis in the Early Universe