$^7$Li Abundances in Halo Stars: Testing Stellar Evolution Models and the Primordial $^7$Li Abundance

Details $^7$Li Abundances in Halo Stars: Testing Stellar Evolution Models and the Primordial $^7$Li Abundance $^7$Li Abundances in Halo Stars: Testing Stellar Evolution Models and the Primordial $^7$Li Abundance

1994-03-21

arxiv.org/abs/astro-ph/9403043v1

Astrophys.J. 433 (1994) 510

Astronomy and Astrophysics

Astrophysics

27 pages, AAS LaTeX, complete postscript file (with figures) available via anonymous ftp from: ftp.cita.utoronto.ca in /cita

Scientific paper

10.1086/174662

A large number of stellar evolution models with [Fe/H] = -2.3 and -3.3 have been calculated in order to determine the primordial $^7$Li abundance and to test current stellar evolution models by a comparison to the extensive database of Li abundances in extremely metal poor halo stars observed by Thorburn (1994). Standard models do a good job of fitting the observed Li abundances in stars hotter than 5600 K. They predict a primordial $^7$Li abundance of Log N(Li) = 2.24\pm 0.03$. Models which include microscopic diffusion predict a downward curvature in the $^7$Li destruction isochrones at hot temperatures which is not present in the observations. Thus, the observations clearly rule out models which include uninhibited microscopic diffusion of $^7$Li from the surface of the star. The [Fe/H] = -2.3 stellar models which include both diffusion and rotational mixing provide an excellent match to the observations. Both the plateau stars and the heavily depleted cool stars are well fit by these models. The rotational mixing leads to considerable $^7$Li depletion in these models and the primordial $^7$Li abundance inferred from these models is Log N(Li) = $3.08\pm 0.1$.

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