2025/05/29 by Ho, Meng-Yuan, Chen, Ke-Jung, Tung, Pei-Cheng
#Astrophysics of Galaxies (astro-ph.GA) #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences
paper · doi:10.48550/arxiv.2505.23768
We present high-resolution simulations of the first star-forming clouds in 15 minihalos with masses ranging from ∼ 105 to 107 M\odot at redshifts z ∼ 17 - 20, using the GIZMO code. Our simulations incorporate detailed primordial gas physics and adopt initial conditions from the state-of-the-art TNG cosmological simulations. To achieve the required resolution, we apply a particle-splitting technique that increases the resolution of the original TNG data by a factor of ∼ 105, reaching gas and dark matter particle masses of 0.2 M\odot and 80 M\odot, respectively. This enables us to resolve gas accretion during the early assembly of minihalos and to capture the emergence of strong turbulent flows. We find that turbulence, driven by gas infall into the dark matter potential wells, is predominantly supersonic, with characteristic Mach numbers ranging from 1.8 to 4.2, increasing with halo mass. The supersonic turbulence effectively fragments the central gas cloud into multiple dense clumps, some of which form gravitationally bound cores and begin to collapse into the first stars. Our results suggest that supersonic turbulence is a common feature in minihalos and plays a key role in generating clumpy star-forming clouds, with important implications for the initial mass function of the first stars.