# Super-Eddington accretion in protogalactic cores

## TL;DR

This study uses high-resolution simulations to demonstrate that super-Eddington accretion can rapidly grow black hole seeds in early protogalaxies, potentially explaining the existence of massive black holes at high redshift.

## Contribution

It provides the first detailed numerical exploration of super-Eddington accretion effects on early black hole growth in protogalaxies, considering various initial conditions and feedback.

## Key findings

- Super-Eddington accretion enables black holes to grow up to 10^5 solar masses within 10^4 years.
- Feedback regulates growth by depleting gas and affecting black hole dynamics, but does not prevent rapid growth.
- Growth stalls after about 1 million years due to local gas exhaustion, with no large-scale inflows in the simulation setup.

## Abstract

The presence of massive black holes (BHs) exceeding $10^9\,{\rm M}_{\odot}$ already at redshift $z > 6$ challenges standard models of BH growth. Super-Eddington (SE) accretion has emerged as a promising mechanism to solve this issue, yet its impact on early BH evolution in tailored numerical experiments remains largely unexplored. In this work, we investigate the growth of BH seeds embedded in a gas-rich, metal-poor protogalaxy at $z \sim 15$ using a suite of high-resolution hydrodynamical simulations that implement a slim-disc-based SE accretion model. We explored a broad parameter space, varying the initial BH mass, feedback efficiency, and spin. We find that SE accretion enables rapid growth in all cases, allowing BHs to accrete up to $10^5\,{\rm M}_{\odot}$ within a few $10^3$-$10^4$ years, independent of seed properties. Feedback regulates this process, both by depleting central gas and altering BH dynamics via star formation-driven potential fluctuations, yet even the strongest feedback regimes permit significantly greater growth than the Eddington-limited case. Growth stalls after less than $\sim$1 Myr due to local gas exhaustion, as no large-scale inflows are present in the adopted numerical setup. Our results show that SE accretion naturally leads to BHs that are overmassive relative to their host galaxy stellar content, consistent with JWST observations. We conclude that short low-duty-cycle SE episodes represent a viable pathway for assembling the most massive BHs observed at early cosmic times, even when starting from light seeds.