Spectroscopic analysis of nearby lower-main-sequence stars

Details Spectroscopic analysis of nearby lower-main-sequence stars Spectroscopic analysis of nearby lower-main-sequence stars

Nov 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009mnras.399.1264w&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 399, Issue 3, pp. 1264-1274.

Astronomy and Astrophysics

Astronomy

Line: Formation, Stars: Abundances, Stars: Late-Type, Galaxy: Evolution

Scientific paper

Abundances of O, Na, Mg, Al, Si, K, Ca, Sc, Ti, V, Cr, Fe, Ni and Ba are determined for 30 nearby lower-main-sequence stars in the Northern sky using high-resolution, high signal-to-noise ratio spectra. Our results show an equilibrium of [Fe/H]I and [Fe/H]II and a much smaller star-to-star scatter of the abundance ratios as a function of metallicity compared with the results of Kotoneva et al. The non-local thermodynamic equilibrium (non-LTE) corrections for oxygen are considered and found to be small (~-0.04dex). A flat trend of [O/Fe] exists over the whole metallicity range. The non-LTE effects for some important elements are discussed, and it is found that the abundance pattern for our programme stars is very similar to that of F and G dwarfs.

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