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Forming the First Stars in the Universe: The Fragmentation of Primordial Gas

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arxiv astro-ph/9910224 v1 pith:DQXBVKHM submitted 1999-10-13 astro-ph

Volker Bromm , Paolo S. Coppi , Richard B. Larson This is my paper
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keywords clumpsfirstfragmentationmasssolarstarsevolutionformation
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In order to constrain the initial mass function (IMF) of the first generation of stars (Population III), we investigate the fragmentation properties of metal-free gas in the context of a hierarchical model of structure formation. We investigate the evolution of an isolated 3-sigma peak of mass 2x10^6 M_solar which collapses at z_coll=30 using Smoothed Particle Hydrodynamics. We find that the gas dissipatively settles into a rotationally supported disk which has a very filamentary morphology. The gas in these filaments is Jeans unstable with M_J~10^3 M_solar. Fragmentation leads to the formation of high density (n>10^8 cm^-3) clumps which subsequently grow in mass by accreting surrounding gas and by merging with other clumps up to masses of ~10^4 M_solar. This suggests that the very first stars were rather massive. We explore the complex dynamics of the merging and tidal disruption of these clumps by following their evolution over a few dynamical times.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. A Pixel-by-Pixel Path to Population III Discovery with JWST

    astro-ph.GA 2026-06 unverdicted novelty 6.0 of 10

    Pixel-by-pixel SBI modeling recovers young massive Pop III clumps at up to 90 percent rate in favorable JWST-like configurations while integrated analyses fail due to contamination.

  2. Ultraviolet diversity of Little Red Dots as a probe for direct-collapse black hole ages

    astro-ph.GA 2026-05 unverdicted novelty 5.0 of 10

    Cosmological hydrodynamical simulations predict that UV diversity in Little Red Dots encodes direct-collapse black hole ages via a rapid transition from BH- to stellar-dominated emission after ~30 Myr.

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