Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...452..102k&link_type=abstract
Astrophysical Journal v.452, p.102
Astronomy and Astrophysics
Astronomy
41
Cosmology: Theory, Stars: Abundances, Stars: Atmospheres, Stars: Population Ii
Scientific paper
The D lines of Li I in extreme Population II stars hotter than 5500 K are highly temperature sensitive because lithium is nearly all ionized. A one-dimensional model atmosphere represents a space and time average over the actual three-dimensional, moving, hot and cold convective structure. Neutral Li does not have the average behavior represented by the one-dimensional model. Lithium is overionized by a factor of 10 so that the Li abundance computed from a one-dimensional model is too small by this same factor. Consequently, log (NLi/Ntotal) + 12 > 3.0.
This higher Li abundance resolves the only discrepancy in the radiatively driven cosmological model of the universe previously discussed by Kurucz. Because the baryon density is high enough to produce a flat, or nearly flat, universe, the number of stars can increase by a factor of 10, and the amount of radiation given off by those stars in the first billion years can increase by a factor of 10 over what is possible with a low baryon density. This model can explain the formation of Population III stars, globular clusters, galaxies, quasars, voids, galaxy clusters, streaming, and large-scale structure. It can explain isolated galactic evolution and morphology including bulges, disks, and abundances.
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