Lithium and Iron Abundances in Low Mass Pre-Main Sequence Stars

Details Lithium and Iron Abundances in Low Mass Pre-Main Sequence Stars Lithium and Iron Abundances in Low Mass Pre-Main Sequence Stars

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.5905p&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #59.05; Bulletin of the American Astronomical Society, Vol. 24, p.824

Astronomy and Astrophysics

Astronomy

Scientific paper

Using high resolution echelle spectroscopy, iron and lithium abundances have been determined for 30 weak-line T Tauri stars in four star formation regions. The results for iron indicate that the current metallicities in the Orion and Ophiuchus clouds are slightly in excess of solar values, while the Taurus-Auriga and Chamaeleon molecular clouds have roughly solar iron abundances. The mean lithium abundance for this sample of very young G and K stars was found to be log N(Li) = 3.6 +/- 0.07 on the scale where log N(H) = 12. This value is approximately 0.5 dex higher than the "canonical" maximum Population I lithium abundance found for young main sequence stars and 0.3 dex higher than the log N(Li) = 3.31 +/- 0.04 for chondrites. The abundances determined in this paper utilize new PMS stellar temperatures derived from high resolution spectral line ratios.

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