A case for Case A: Detailed look at binary black hole formation through stable mass transfer

Context. In isolated binary evolution, binary black hole (BBH) mergers are generally formed through stable mass transfer (SMT) or common envelope evolution. In recent years, the SMT channel has received significant attention due to detailed binary models showing increased mass transfer stability compared to previous studies. Aims. In this work, we perform a full zero-age-main-sequence to compact object merger analysis using detailed binary models at eight metallicities between 10 −4 Z ⊙ and 2 Z ⊙ to self-consistently model the population properties of BBH mergers in the SMT channel, determined their progenitor initial conditional, and investigate the binary physics governing their formation and metallicity dependence. Methods. We used the population synthesis code POSYDON that incorporates detailed single-star and binary model grids to determine the population of BBH mergers from SMT. Using its extended grids of MESA binary models, we determined the essential physics in the formation of BBH mergers. Results. The SMT channel produces BBH mergers predominantly from systems with P ZAMS ≤ 10 days. In these systems, both the initial mass transfer between two stars and the subsequent interaction between the remaining star and the first-born BH take place while the respective donor star is on the main sequence (Case A). We find a limited contribution from wider Case B or C systems. Without a natal kick, the SMT channel does not produce BBH mergers above Z > 0.2 Z ⊙ due to orbital widening from stellar wind mass loss. The primary BH mass distribution shows a strong dependence on metallicity, while the mass ratio prefers unity independent of metallicity due to mass ratio reversal. Additionally, the χ eff distributions contain peaks at χ eff = 0 and ∼0.15, of which the former disappears at high metallicities. A mass-scaled natal kick leave this subpopulation unchanged but introduce a low-mass, unequal mass ratio subpopulation that merges within the Hubble time due to their eccentricity.