Chemical Feedback and the Extinction of Population III Stars

Details Chemical Feedback and the Extinction of Population III Stars Chemical Feedback and the Extinction of Population III Stars

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc..990..395s&link_type=abstract

FIRST STARS III: First Stars II Conference. AIP Conference Proceedings, Volume 990, pp. 395-399 (2008).

Computer Science

Population Iii Stars, Star Formation, Origin, Formation, Evolution, Age, And Star Formation, Background Radiations, Protogalaxies, Primordial Galaxies, Chemical Composition And Chemical Evolution

Scientific paper

Theoretical models suggest that a transition from massive Population III stars to normal Population II/I stars occurs when the metallicity of the star forming gas crosses the critical range Zcr = 10-5+/-1 Zsolar. According to this view, the formation of Population III stars is regulated by the rate at which heavy elements are produced and mixed in the gas surrounding the first star-forming regions. The cosmic implications of such process, generally referred to as chemical feedback, have been investigated following semi-analytic approaches which have either focused on the transport of metals through supernova-driven outflows, or on the ``genetic'' transmission of metals from parent sub-halos along the hierarchical evolution of cosmic structures. Although the above studies find that it is difficult to rapidly suppress the formation of Pop III stars, this common wisdom has to face the fact that no metal-free stars have yet been found by surveys of metal-poor stars of the Milky Way halo. Alternative probes such as the apparent excess in the cosmic near-infrared background, the equivalent width distributions of high-z Lyα emitters, and the He II 1640 A˚ line in composite spectra of LBGs, are yielding only tentative evidence for the presence of Pop III stars at z<9. The question then remains: are Pop III stars hidden (due to their very small statistical frequency or because they reside in as-yet-unexplored environments) or did they disappear as a result of chemical feedback a long time ago? The work presented here attempts to address this question using numerical simulations which follow the evolution, metal enrichment and energy deposition of both Population III and Population II stars.

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