Primordial black holes captured by stars lead to either quiet consumption or explosive disruption via disk formation, producing transients and high-spin remnants with potentially observable event rates.
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N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.
Efficient mass transfer in binaries naturally limits the mass of the first-born black hole and produces a sharp drop above 45 solar masses that mimics the pair-instability gap.
High-resolution cosmological zoom-in simulations find that major mergers do not trigger sustained super-Eddington black hole accretion in low-mass halos when feedback is included; episodes occur only immediately after seeding or with feedback disabled.
citing papers explorer
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Rapid intermediate-mass black hole formation via runaway mergers of black holes
N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.
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The role of major mergers in triggering super-Eddington accretion
High-resolution cosmological zoom-in simulations find that major mergers do not trigger sustained super-Eddington black hole accretion in low-mass halos when feedback is included; episodes occur only immediately after seeding or with feedback disabled.