Formation of Supersonic Turbulence in the Primordial Star-forming Cloud
We present new simulations of the formation and evolution of the first star-forming cloud within a massive minihalo of mass of 1.05 × 10 ^7 M _⊙ , carried out using the GIZMO code with detailed modeling of primordial gas cooling and chemistry. Unlike previous studies that simulated the formation of...
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| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal Letters |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/2041-8213/adf18d |
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| Summary: | We present new simulations of the formation and evolution of the first star-forming cloud within a massive minihalo of mass of 1.05 × 10 ^7 M _⊙ , carried out using the GIZMO code with detailed modeling of primordial gas cooling and chemistry. Unlike previous studies that simulated the formation of the first stars within a smaller cosmological box size of ∼0.3–2 Mpc, our work adopts initial conditions from the large-scale cosmological simulations, IllustrisTNG spanning ∼50 Mpc to study the formation of primordial clouds that give birth to the first stars. We increase the original resolution of IllustrisTNG by a factor of ∼10 ^5 using a particle-splitting technique, achieving an extremely high resolution that allows us to resolve turbulence driven by gravitational collapse during early structure formation. We find that strong supersonic turbulence with a characteristic Mach number of ∼5.2 naturally develops within the collapsing halo. This turbulence efficiently stirs the gas, promoting fragmentation of the star-forming cloud into multiple dense clumps. Among them, we identify a gravitationally bound core with a mass of 8.07 M _⊙ and a size of 0.03 pc, which exceeds its local Jeans mass and is on the verge of collapsing into a star. Our results indicate that supersonic turbulence may be common in primordial halos and can play a crucial role in cloud-scale fragmentation, providing an alternative channel to form less massive first stars and strengthens the argument of lowering the characteristic mass for the first stars found in previous studies. |
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| ISSN: | 2041-8205 |