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 neighboring ultra-faint dwarf galaxies. Their
low metal abundances (${\rm [Fe/H]} < -3$) 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 $1.77\times 10^{6} \ {\rm M}_{\bigodot}$, a Pop III
star with mass $13 \ {\rm M}_{\bigodot}$ 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 $2.6\times
10^{-4} \ {\rm Z}_{\bigodot}$ (${\rm [Fe/H]} = -3.42$). 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.
