Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pasp...97..784b&link_type=abstract
Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 97, Sept. 1985, p. 784-789.
Astronomy and Astrophysics
Astronomy
21
Dwarf Stars, Lithium, Metallicity, Stellar Composition, Stellar Mass, Hydrogen, Iron, Stellar Models, Stellar Temperature
Scientific paper
The hottest of the halo dwarfs observed by Spite and Spite (1982) and Spite. Maillard and Spite (1984) has been reobserved to investigate the character of the relationship between Li abundance and temperature. For that very metal-deficient star (Fe/H = 2.1) the new equivalent width and Li abundance are about 25 percent larger than the Spite value, or Li/H = 1.4 x 10 to the -10th. The relationship between Li content and metallicity in halo dwarfs and old disk stars is also studied; the mean Li abundance in metal-poor stars hotter than 5600 K does not appear to change while the Fe/H abundance changes over nearly two orders of magnitude. In order to compare stars with vastly different metallicity, and thus internal structure, masses were estimated for each star from theoretical calculations of VandenBerg. The mean mass so determined for the halo stars is 0.77 + or -0.06 solar mass with most having values between 0.75-0.82 solar mass A Livs. stellar mass plot indicates that the depletion in the lower mass, lower metallicity stars has the same character as the depletion found in the cooler Hyades by Cayrel et al. (1984), but it sets in at lower masses. The possibility exists that the halo dwarfs began with the same Li content as the Hyades and are in the process of depleting it.
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