Author: Oey, M.S.

Source: Astrophysics and Space Science, Volume 281, Numbers 1-2, July 2002 , pp. 483-486(4)

Publisher: Springer

Abstract:

Two fundamental constraints on the earliest star formation conditions in the Galaxy are an apparent empirical low-metallicity threshold of-4 ≲ [Fe/H], an and upper limit to the fraction of Population III halo stars of F _III < 4 × 10^-4. How do these observed constraints compare with predictions of simple models? This is investigated within the framework of element dispersal from clustered core-collapse SNe. Simple arguments considering turbulent mixing within multi-phase ISM suggest that the observed low-metallicity threshold is consistent with rough expected values. However, the observed limit on F _III is two orders of magnitude larger than predictions from this simple, one-zone inhomogeneous chemical evolution.

Keywords: stars: abundances; ISM: abundances; Galaxy: formation; Galaxy: halo; galaxies: evolution; early universe

Document Type: Research article

DOI: http://dx.doi.org/10.1023/A:1019565329719

Publication date: 2002-07-01

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