Explaining the high nitrogen abundances observed in high-z galaxies via population III stars of a few thousand solar masses
arxiv(2024)
摘要
The chemical enrichment of the early Universe is a crucial element in the
formation and evolution of galaxies, and Population III (PopIII) stars must
play a vital role in this process. In this study, we examine metal enrichment
from massive stars in the early Universe's embryonic galaxies. Using radiation
hydrodynamic simulations and stellar evolution modelling, we calculated the
expected metal yield from these stars. Specifically, we applied accretion rates
from a previous radiation-hydrodynamic simulation to inform our stellar
evolution modelling, executed with the Geneva code, across 11 selected
datasets, with final stellar masses between 500 and 9000 Msol. Our results
demonstrate that the first generation of Pop III stars within a mass range of
2000 to 9000 Msol result in N/O, C/O and O/H ratios compatible with the values
observed in very high-z galaxies GN-z11 and CEERS 1019. The ejecta of these Pop
III stars are predominantly composed of He, H, and N. Our Pop III chemical
enrichment model of the halo can accurately reproduce the observed N/O and C/O
ratios, and, by incorporating a hundred times more zero-metallicity
interstellar material with the stellar ejecta, it accurately attains the
observed O/H ratio. Thus, a sub-population of extremely massive PopIII stars,
with masses surpassing approximately 2000 Msol, effectively reproduces the CNO
elemental abundances observed in high-z JWST galaxies to date.
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