Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....106.1080s&link_type=abstract
Astronomical Journal (ISSN 0004-6256), vol. 106, no. 3, p. 1080-1086.
Astronomy and Astrophysics
Astronomy
71
Abundance, F Stars, G Stars, Lithium, Star Clusters, Stellar Evolution, Binary Stars, Color-Magnitude Diagram, Spectral Line Width, Stellar Composition, Stellar Spectrophotometry, Stellar Temperature
Scientific paper
Echelle observations are presented of lithium in 63 F and G dwarfs of the Praesepe cluster. For stars earlier than about G0V, Praesepe follows the same trends seen in the Hyades, which has approximately the same age and composition. Stars in Praesepe later than about G5V have more Li than their Hyades counterparts, possibly because Praesepe is slightly younger than the Hyades or has slightly lower metallicity. Significant differences in the abundance of Li are seen among stars of the same color, and, as in the Hyades, there is a tendency for the deviant stars to be binaries to the extent that duplicity in Praesepe is known. There are also stars with much less Li than most cluster members yet which appear to be true members of Praesepe. The close binary KW 181 has a normal Li abundance, despite the fact that similar close binaries in the Hyades are Li rich.
David Soderblom R.
Fedele Stephen B.
Jones Burton F.
Prosser Charles F.
Stauffer John R.
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