Following The Cosmic Evolution Of Pristine Gas I: Implications For Milky Way Halo Stars

Abstract

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.

19 pages, 13 figures, accepted by ApJ Oct 2016

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Cited by in corpus (12)

• When did Population III star formation end?
• Simulating Neutron Star Mergers as r-process Sources in Ultra Faint Dwarf Galaxies
• EPOCHS VII: Discovery of high redshift ($6.5<z<12$) AGN candidates in JWST ERO and PEARLS data
• The Most Metal-Poor Stars. V. The CEMP-no Stars in 3D and Non-LTE
• The role of faint population III supernovae in forming CEMP stars in ultra-faint dwarf galaxies
• Origin of the CEMP-no Group Morphology in the Milky Way
• Following the Cosmic Evolution of Pristine Gas III: The Observational Consequences of the Unknown Properties of Population III Stars
• Implications of inhomogeneous metal mixing for stellar archaeology
• Formation of carbon-enhanced metal-poor stars as a consequence of inhomogeneous metal mixing
• Are Faint Supernovae Responsible for Carbon-Enhanced Metal-Poor Stars?
• The Effects of Radiative Feedback and Supernova Induced Turbulence on Early Galaxies
• How Metals Are Transported In And Out Of A Galactic Disk: Dependence On The Hydrodynamic Schemes In Numerical Simulations