Radiating Bondi Flows II: Giant Planet Accretion Models

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ID: 330721
2026
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Abstract
Abstract In the core accretion model of giant planet formation, the late stages of runaway growth are regulated by the hydrodynamic infall of gas from the protoplanetary disk. For a subset of planet-disk pairings, this scenario is analogous to the classical Bondi problem, which has motivated a Bondi-like parameterization of accretion in some population synthesis models. Existing models and the associated classical Bondi rate however, are predicated upon an adiabatic equation of state. In reality, the planet and its associated accretion shock supply a luminosity that substantially heats the accretion flow. In Paper I of this series, we demonstrate that such radiative feedback can dramatically suppress accretion by orders of magnitude. Here we quantify this effect under realistic planet-forming conditions. We find that for planets forming in an unperturbed disk, accretion is suppressed by 1-2 orders of magnitude interior to ∼10 AU. For planets that open a gap, this feedback is less dramatic and the effect is ∼ 1 order in magnitude. We investigate the effect of various assumptions regarding dust opacities, shock efficiency, and planet radius and find this radiative suppression mechanism to be fairly insensitive to these effects. We also perform full time-dependent simulations demonstrating that the associated adverse entropy profiles are accurate and stable to convection. A simple and flexible set of open-source tools are provided to incorporate this radiative feedback into existing accretion models and population synthesis frameworks.
Reference Key
openalex_W7140219424 Use this key to autocite in the manuscript while using SciMatic Manuscript Manager or Thesis Manager
Authors Avery P. Bailey, Kaitlin Kratter, Andrew N. Youdin
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1836
URL
https://doi.org/10.1093/mnras/stag1836
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