Physics
Scientific paper
May 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..oss..ca07p&link_type=abstract
American Physical Society, Ohio Section Spring Meeting, 1-2 May 1998 Muncie, Indiana, abstract #CA.07
Physics
Scientific paper
The oxygen-to-iron ratio in field stars in the solar neighborhood shows a significant change near [Fe/H] ~ -1. At lower iron abundances the O/Fe ratio is roughly constant at about 3 times the solar value, whereas for more iron-rich stars O/Fe gradually decreases to the solar ratio. Because O and Fe are primarily produced in stars of different lifetimes, the change in the [O/Fe]-[Fe/H] relation is expected to occur at a fixed time after the onset of star formation, providing a valuable date in the Galaxy's chemical evolution. The sharpness of the transition indicates the uniformity of the chemical evolution rate in different star-forming regions. Unfortunately few data exist near the transition. We have measured [Fe/H] and [O/Fe] in 20 field dwarf stars in the range -1.65 < [Fe/H] < -0.65 in order to define better the location and sharpness of the transition. We find a gradual change in [O/Fe] over our full range of [Fe/H]. The transition does not appear to be sharp, and the star-to-star scatter is somewhat larger than our estimated observational uncertainties.
Laird John B.
Pandjiaris Michael
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