A model based on Chandrasekhar's 1951 time-invariant quantity quantitatively explains the Mach-number dependence of the density power spectrum slope in isothermal supersonic turbulence and demonstrates that the slope cannot reliably determine the Mach number.
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A modeling framework for Population III stars improves thermochemistry, spectra, and feedback in cosmological simulations, showing impacts on early evolution and explaining high-z HeII observations.