Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21340616p&link_type=abstract
American Astronomical Society, AAS Meeting #213, #406.16; Bulletin of the American Astronomical Society, Vol. 41, p.201
Astronomy and Astrophysics
Astronomy
Scientific paper
We determine the Fe, Ti, V, Cr, Ni, Al, Si, and S abundances of seventeen late-F, G, and early-K type main-sequence dwarfs in the Pleiades open cluster using high-resolution, moderate signal-to-noise spectra obtained with the Hobby-Eberly Telescope and High Resolution Spectrograph. Abundances have been derived from a selection of features within the wavelength span 5778 - 7850 Å. Equivalent widths of the features have been measured using a consistent technique of fitting Gaussian profiles to the absorption features, and abundances have been derived using model atmospheres interpolated from Kurucz grids. Abundances derived from FeI lines are found to be in star-to-star agreement, whereas those derived from FeII lines show a stark increase with decreasing T(eff) for stars with T(eff) < 5400 K. The mean cluster abundance as determined by the FeI abundances of fifteen stars is [Fe/H] = +0.07 ± 0.01. Similar to Fe abundances derived from FeII lines, T(eff)-dependent overabundances of Si and S derived from high-excitation lines (4.93 < ξ < 7.87 eV) are also seen in the cool Pleiads. These overionization and overexcitation effects mimick those found for cool dwarfs in the Hyades and M34 open clusters, as well as in the Ursa Major moving group. The anomalous cool dwarf abundances are not believed to be real; rather, the T(eff)-dependent trends suggest an incomplete understanding of the atmospheric conditions in cool open cluster dwarfs.
This research began in 2008 during the CTIO REU program under grant AST-0647604. We acknowledge J. King for providing HET/HRS spectra.
Plunkett Adele
Schuler Simon C.
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