Fractions of Compact Object Binaries in Star Clusters: Theoretical Predictions


 Binary population in field stars and star clusters contributes to the formation of gravitational wave (GW) sources. However, the fraction of compact-object binaries (CBs), which is an important feature parameter of binary populations, is still difficult to measure and very uncertain. This paper predicts the fractions of important CBs and semi-compact object binaries (SCBs) making use of advanced stellar population synthesis (ASPS) technique. A comparison with the result of \emph{N}-body simulation is also presented. It is found that most CBs are formed within about 500\,Myrs after the starburst. The fractions of CBs and SCBs are shown to correlate with stellar metallicity. The higher the metallicity, the less the fraction of black hole binaries (BHBs), neutron star binaries (NSBs), and SCBs. This suggests that the GW sources of BHBs and NSBs are more likely to form in metal-poor environments. However, the fraction of black hole-neutron star binaries (BHNSBs) is shown to larger for metal-rich populations on average.