Oxygen abundances in F and G dwarfs derived from the forbidden OI line at 6300 A

Details Oxygen abundances in F and G dwarfs derived from the forbidden OI line at 6300 A Oxygen abundances in F and G dwarfs derived from the forbidden OI line at 6300 A

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...261..255n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 261, no. 1, p. 255-262.

Astronomy and Astrophysics

Astrophysics

94

Abundance, Dwarf Stars, F Stars, G Stars, Oxygen, Stellar Spectra, Metallicity, Spectral Line Width, Stellar Atmospheres, Stellar Models

Scientific paper

High resolution, high-S/N spectra at 6300 A have been obtained for 23 F and G main sequence stars ranging in metallicity, Fe/H, from -0.8 to +0.3. From these spectra the equivalent width of the faint, forbidden OI line at 6300.3 A has been measured to an accuracy of about +/- 0.6 mA. The data has been analyzed using line blanketed, flux constant, model atmospheres with fundamental parameters determined from Stromgren photometry. The errors in the derived O/Fe values are found to be about 0.05 dex, when the iron abundances are determined from Fe II lines. In the metallicity range -0.3 to +0.3 the O/Fe ratio is solar with a dispersion of only 0.04 dex. Below Fe/H = -0.3 the O/Fe ratio increases with decreasing Fe/H to O/Fe = 0.4 dex at Fe/H = -0.8. There is, however, no universal O/Fe-Fe/H relation in this metallicity range. Stars born in the inner part of the disk tend to have higher O/Fe ratios at a given metallicity than stars belonging to the solar neighborhood. Oxygen abundances derived from the OI triplet at 7774 A are higher than the abundances derived from the forbidden line. The difference increases with decreasing Fe/H and amounts to about 0.2 dex at Fe/H = -0.8 if the difference is normalized to zero for the sun.

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