Hungry or Not: How Stellar-Mass Black Holes Grow (or Don't) in Dark Matter Mini-Haloes at High-Resolution

Abstract

We compare the performance of the popular Bondi-Hoyle-Lyttleton (BHL) accretion scheme with a simple mass-flux scheme applied to stellar-mass black holes (BHs) across six levels of increasing spatial resolution. Simulating the formation of black holes within cosmological mini-haloes at $z \sim 20$, we investigate scenarios both with and without supernova events, which result in BHs of initial mass $10.8 \, \text{M}_\odot$ and $270 \, \text{M}_\odot$ respectively. Our explicit focus on the stellar-mass range pushes the maximum resolution down to sub-$10^{-3} \, \text{pc}$ regimes, where more complicated gas dynamics are resolved. We observe efficient growth and rotationally supported, $\sim$$10^{-1} \, \text{pc}$-scale discs around all $270 \, \text{M}_\odot$ BHs independent of resolution and accretion scheme, though clumps, bars, and spiral arm structures impact stability at high resolution. We analyse the effect of these instabilities on the accretion cycle. In contrast, all bar one of the $10.8 \, \text{M}_\odot$ BHs fail to attract a disc and experience modest growth, even when characteristic scales of accretion and dynamical friction are reasonably resolved. While the two accretion schemes somewhat converge in mass growth for the $270 \, \text{M}_\odot$ case over $1 \, \text{Myr}$, the greater degree of gas fragmentation induces more randomness in the evolution of the $10.8 \, \text{M}_\odot$ BHs. We conclude that early universe black holes of $M_{\text{BH}} \sim 10^1 \, \text{M}_\odot$ struggle to grow even in gas-rich environments without feedback in comparison to seeds of $M_{\text{BH}} \sim 10^2 \, \text{M}_\odot$, and the latter exhibit convergent growth histories across accretion schemes below a spatial resolution of $1 \times 10^{-3} \, \text{pc}$.