Oral Presentation
Primordial Turbulence: Accretion of Clouds in the Early Universe
Presenter: Meng-Yuan Ho (ASIAA)
Turbulence is a pivotal factor in the star formation process, influencing the characteristics of early stars. Existing simulations have predicted the formation of stars with significantly greater mass than observed in metal-poor stars, potentially attributed to the absence of turbulence. Recent studies indicate that turbulence can raise the temperature of primordial clouds, thereby reducing the star-forming rate (SFR) and impacting the mass of the earliest stars in the universe. Additionally, research has identified accretion-driven turbulence as a universal phenomenon in the cosmos. While implementing driven turbulence in simulations can provide valuable insights, the underlying relationship between primordial turbulence and cloud dynamics remains unclear.
This study presents N-body hydrodynamics (HD) cosmological simulations utilizing the GIZMO code, which incorporates critical physics such as radiative cooling for primordial gas and turbulence diffusion. The initial conditions are derived from halo data within the TNG project at z ~ 20, where the halo with total mass ranges from 1e6 to 1e8 solar mass. Employing particle-splitting techniques, we achieve the finest resolution of 0.1 to 1 solar mass per gas particle, enabling us to unveil the intricate structure within dense clouds. Our analysis encompasses various physical properties, including density distributions, accretion rates, and the Mach number of the turbulence spanning the entirety of our simulations. Our primary objective is to unveil the intricate relationship between halo mass and these fundamental properties, furthering our understanding of the role of turbulence in the star formation process.
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