Magnetized Super-Eddington Accretion as a Growth Regime for Early Supermassive Black Holes

This work presents the Magnetized Super-Eddington (MSE) hypothesis, a phenomenological framework aimed at explaining the rapid growth of some early supermassive black holes without invoking violations of the classical Eddington limit or introducing new fundamental physics. The model explores how strongly magnetized accretion flows can reduce the effective radiative efficiency by channeling a significant fraction of the liberated gravitational energy into magnetic stresses and advective transport rather than radiation. This weakens radiation–matter coupling and relaxes radiative feedback, naturally allowing enhanced mass accretion rates. Under this interpretation, super-Eddington growth emerges as a consequence of magnetically dominated relativistic MHD regimes similar to those already observed in modern GRMHD simulations (e.g., MAD-like states). The work develops a minimal energetic formulation, introduces a phenomenological closure for radiative decoupling, provides order-of-magnitude estimates, and outlines observational consequences and testable predictions. This study should be understood as a theoretical framework and plausibility analysis rather than a first-principles GRMHD simulation. Its goal is to extend existing magnetized disk physics to cosmological growth timescales and to provide a physically consistent pathway for the formation of ultramassive black holes in the early universe.