Self-gravitating disks heated by stars reach a universal optical effective temperature of 4000-4500 K independent of accretion rate, black hole mass, and viscosity, explaining Little Red Dots.
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LRDs are interpreted as high-inclination hyper-Eddington accreting SMBHs analogous to SS 433, with V-shaped SEDs, X-ray weakness, and Balmer breaks emerging from disk self-shielding geometry.
Monte Carlo solutions to the Smoluchowski coagulation equation yield runaway timescales and mass evolution for primordial black hole clusters at different redshifts based on cluster properties.
Migration traps concentrate stellar-mass black holes in AGN disks, generating self-regulated magnetic reconnection heating that yields excess short-timescale optical/UV variability, flattened structure functions, and deviations from the τ∝λ^{4/3} lag relation.
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Smoluchowski Coagulation Equation and the Evolution of Primordial Black Hole Clusters
Monte Carlo solutions to the Smoluchowski coagulation equation yield runaway timescales and mass evolution for primordial black hole clusters at different redshifts based on cluster properties.