Population Synthesis of Black Hole Binaries with Compact Star Companions

Abstract

We perform a systematic study of merging black hole (BH) binaries with compact star (CS) companions, including black hole--white dwarf (BH--WD), black hole--neutron star (BH--NS) and black hole--black hole (BH--BH) systems. Previous studies have shown that mass transfer stability and common envelope evolution can significantly affect the formation of merging BH--CS binaries through isolated binary evolution. With detailed binary evolution simulations, we obtain easy-to-use criteria for the occurrence of the common envelope phase in mass-transferring BH binaries with a nondegenerate donor, and incorporate into population synthesis calculations. To explore the impact of possible mass gap between NSs and BHs on the properties of merging BH--CS binary population, we adopt different supernova mechanisms involving the \textit{rapid}, \textit{delayed} and \textit{stochastic} prescriptions to deal with the compact remnant masses and the natal kicks. Our calculations show that there are $\sim 10^5-10^6$ BH--CS binaries in the Milky Way, among which dozens are observable by future space-based gravitational wave detectors. We estimate that the local merger rate density of all BH--CS systems is $\sim 60-200\mathrm{Gp}{\mathrm{c}}^{-3}\mathrm{y}{\mathrm{r}}^{-1}$. While there are no low-mass BHs formed via \textit{rapid} supernovae, both \textit{delayed} and \textit{stochastic} prescriptions predict that $\sim 100\%$/$\sim 70\%$/$\sim 30\%$ of merging BH--WD/BH--NS/BH--BH binaries are likely to have BH components within the mass gap.

arXiv comment21 pages, 12 figures, 1 table, submitted to ApJ after incorporating referee's comments

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