Symmetry Breaking in Merging Binary Black Holes from Young Massive Clusters and Isolated Binaries

Abstract

Properties of the to-date observed binary black hole (BBH) merger events suggest a preference toward spin–orbit aligned mergers. Naturally, this has caused widespread interest and speculations regarding implications on various merger formation channels. Here we show that (i) not only the BBH merger population from isolated binaries but also (ii) BBH population formed in young massive clusters (YMCs) would possess an asymmetry in favor of aligned mergers, in the distribution of the events’ effective spin parameter ( χ _eff ). In our analysis, we utilize BBH merger outcomes from state-of-the-art N -body evolutionary models of YMCs and isolated binary population synthesis. We incorporate, for the first time in such an analysis, misalignments due to both natal kicks and dynamical encounters. The YMC χ _eff distribution has a mean (an antialigned merger fraction) of 〈 χ _eff 〉 ≤ 0.04 ( f _X − ≈ 40%), which is smaller (larger) than but consistent with the observed asymmetry of 〈 χ _eff 〉 ≈ 0.06 ( f _X − ≈ 28%) as obtained from the population analysis by the LIGO–Virgo–KAGRA collaboration. In contrast, isolated binaries alone tend to produce a much stronger asymmetry; for the tested physical models, 〈 χ _eff 〉 ≈ 0.25 and f _X − ≲ 7%. Although the YMC χ _eff distribution is more similar to the observed counterpart, none of the channels correctly reproduce the observed distribution. Our results suggest that further extensive model explorations for both isolated binary and dynamical channels as well as better observational constraints are necessary to understand the physics of “the symmetry breaking” of the BBH merger population.

Keywords

• Stellar mass black holes
• Massive stars
• N-body simulations
• Gravitational wave sources
• Close binary stars
• Young massive clusters