Seeding the second star: enrichment from population III, dust evolution, and cloud collapse

We investigate the formation of extremely metal-poor (EMP) stars that are observed in the Galactic halo and neighbouring ultra-faint dwarf galaxies. Their low metal abundances ([Fe/H] < -3) indicate that their parent clouds were enriched by a single or several supernovae (SNe) from the first (Pop III) stars. In this study, we perform numerical simulations of the entire formation sequence of an EMP star through the feedback effects of photoionization and metal-enrichment by a Pop III SN. We for the first time employ a metal/dust properties calculated consistently with the progenitor model, and solve all relevant radiative cooling processes and chemical reactions including metal molecular formation and grain growth until the protostar formation. In a minihalo (MH) with mass 1.77× 10⁶ {M_{\bigodot }}, a Pop III star with mass 13 {M_{\bigodot }} forms at redshift z = 12.1. After its SN explosion, the shocked gas falls back into the central MH internally enriching itself. The metallicity in the recollapsing region is 2.6× 10^{-4} {Z_{\bigodot }} ([Fe/H] = -3.42). The recollapsing cloud undergoes cooling by HD, CO, and OH molecules and heating along with H₂ formation. Eventually by grain growth and dust cooling, knotty filaments appear in the central 100 au region with the help of turbulence driven by the SN, leading to the formation of low-mass EMP stars surviving until the present day.