Following The Cosmic Evolution Of Pristine Gas I: Implications For Milky
  Way Halo Stars
  We make use of new subgrid model of turbulent mixing to accurately follow the
cosmological evolution of the first stars, the mixing of their supernova
ejecta, and the impact on the chemical composition of the Galactic Halo. Using
the cosmological adaptive mesh refinement code RAMSES, we implement a model for
the pollution of pristine gas as described in Pan et al. Tracking the
metallicity of Pop III stars with metallicities below a critical value allows
us to account for the fraction of Z < Zcrit stars formed even in regions in
which the gas' average metallicity is well above Zcrit. We demonstrate that
such partially-mixed regions account for 0.5 to 0.7 of all Pop III stars formed
up to z = 5. Additionally, we track the creation and transport of "primordial
metals" (PM) generated by Pop III supernovae (SNe). These neutron-capture
deficient metals are taken up by second-generation stars and likely lead to
unique abundance signatures characteristic of carbon-enhanced, metal-poor
(CEMP-no) stars. As an illustrative example, we associate primordial metals
with abundance ratios used by Keller et al. to explain the source of metals in
the star SMSS J031300.36-670839.3, finding good agreement with the observed
[Fe/H], [C/H], [O/H], and [Mg/Ca] ratios in CEMP-no Milky Way halo stars.
Similar future simulations will aid in further constraining the properties of
Pop III stars using CEMP observations, as well as improve predictions of the
spatial distribution of Pop III stars, as will be explored by the next
generation of ground- and space-based telescopes.
