Analysis of three field halo stars and the chemical evolution of the Galaxy

Details Analysis of three field halo stars and the chemical evolution of the Galaxy Analysis of three field halo stars and the chemical evolution of the Galaxy

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...144..343b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 144, no. 2, March 1985, p. 343-354.

Astronomy and Astrophysics

Astrophysics

38

Chemical Evolution, Cosmochemistry, Galactic Evolution, Halos, Late Stars, Stellar Temperature, Abundance, Dwarf Stars, Giant Stars, Metallicity, Population Theory, Signal To Noise Ratios, Stellar Color

Scientific paper

High resolution electronographic plates were used to study three extreme Population II stars. Abundances of M/H = -2.2, -2.5, and -3.0 are found, increasing the number of extreme halo stars of M/H lower than -2 analyzed to about 35, and of M/H equal to less than -2.5 to about 10. Abundance determinations from detailed analysis and from spectrum synthesis techniques are presented. The following elements are considered: the light elements, C, N; the carbon-burning products: Mg, Al; the silicon-burning products: Ca, Ti, Cr, Fe, Ni; and the s and r-process elements Y, Ba, and Eu. The nitrogen-to-iron ratio is always above solar, which is evidence for mixing in giants, but could be also due to a primary production of nitrogen at early times, as indicated in particular by the dwarf star. The abundance of the light metal Al varies from star to star. There seems to be a trend for Ca to be overabundant. The s-process elements are always overdeficient, whereas the europium-to-iron ratio seems to be solar at all metallicities.

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