Binary interactions and cluster dynamics boost PISN rates by up to 3x versus single stars, enabling constraints on stellar-wind mass loss and galaxy metallicity distributions.
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GWTC-4 data analysis yields a pair-instability mass gap lower edge at 44.3^{+5.9}_{-3.5} M_⊙, an S-factor of 268^{+195}_{-116} keV b for ^{12}C(α,γ)^{16}O, and two populations supporting both direct formation and hierarchical mergers.
Semi-analytical models show AGN disks produce repeated BBH mergers with a high-mass tail beyond the pair-instability gap, more efficiently at low viscosity, with spin and mass-ratio signatures that can match events like GW190521.
Isolated Population III binaries can form GW231123-like events if convective overshooting is inefficient, the carbon-alpha reaction rate is 2 sigma below standard, and initial orbits match those of later-generation binaries.
Slowly rotating 80-85 solar mass Pop III stars form black holes of similar mass with dimensionless spins up to 0.7, just below the pair-instability gap.
citing papers explorer
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GW231123 Formation from Population III Stars: Isolated Binary Evolution
Isolated Population III binaries can form GW231123-like events if convective overshooting is inefficient, the carbon-alpha reaction rate is 2 sigma below standard, and initial orbits match those of later-generation binaries.
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Fast-spinning massive black holes from slowly rotating low-metallicity stars: implications for GW231123
Slowly rotating 80-85 solar mass Pop III stars form black holes of similar mass with dimensionless spins up to 0.7, just below the pair-instability gap.