We investigate the formation of extremely metal-poor ( EMP ) stars that are observed in the Galactic halo and neighboring 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 a EMP star through the feedback effects of photo-ionization 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 \times 10 ^ { 6 } { 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 \times 10 ^ { -4 } { Z _ { \bigodot } } ( { [ Fe / H ] } = -3.42 ) .
The recollapsing cloud undergoes cooling by HD , CO , and OH molecules and heating along with H _ { 2 } 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 .