Li I and K I Scatter in Cool Pleiades Dwarfs
J.R. King, S.C. Schuler, L.M. Hobbs, M.H. Pinsonneault

TL;DR
This study investigates the star-to-star scatter in lithium line strengths among cool Pleiades dwarfs, finding evidence for real abundance differences likely caused by pre-main-sequence processes rather than measurement errors or chromospheric effects.
Contribution
It provides evidence that the lithium scatter is due to genuine abundance variations, not observational biases, and discusses models linking these differences to pre-main-sequence stellar activity.
Findings
Li I scatter is not correlated with K I or O I lines.
No abundance difference between subordinate and resonance Li I lines.
Observed data supports real abundance variations over measurement errors.
Abstract
We utilize high-resolution (R~60,000), high S/N (~100) spectroscopy of 17 cool Pleiades dwarfs to examine the confounding star-to-star scatter in the 6707 Li I line strengths in this young cluster. Our Pleiads, selected for their small projected rotational velocity and modest chromospheric emission, evince substantial scatter in the linestrengths of 6707 Li I feature that is absent in the 7699 K I resonance line. The Li I scatter is not correlated with that in the high-excitation 7774 O I feature, and the magnitude of the former is greater than the latter despite the larger temperature sensitivity of the O I feature. These results suggest that systematic errors in linestrength measurements due to blending, color (or color-based T_eff) errors, or line formation effects related to an overlying chromosphere are not the principal source of Li I scatter in our stars. There do exist analytic…
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