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The recently launched James Webb Space Telescope promises unparalleledadvances in our understanding of the first stars and galaxies, but realizingthis potential requires cosmological simulations that capture the key physicalprocesses that affected these objects. Here we show that radiative transfer andsubgrid turbulent mixing are two such processes. By comparing simulations withand without radiative transfer but with exactly the same physical parametersand subgrid turbulent mixing model, we show that tracking radiative transfersuppresses the Population III (Pop III) star formation density by a factor ofapproximately 4. In both simulations, $\gtrsim 90\%$ of Pop III stars are foundin the unresolved pristine regions tracked by our subgrid model, which does abetter job at modeling the regions surrounding proto-galaxy cores where metalsfrom supernovae take tens of Myrs to mix thoroughly. At the same time,radiative transfer suppresses Pop III star formation, via the development ofionized bubbles that slows gas accretion in these regions, and it results incompact high-redshift galaxies that are surrounded by isolated low masssatellites. Thus turbulent mixing and radiative transfer are both essentialprocesses that must be included to accurately model the morphology,composition, and growth of primordial galaxies.

The Effects of Radiative Feedback and Supernova Induced Turbulence on Early Galaxies