2006/08/03 by Jacob L. Bean, C. Sneden, Christopher Sneden +6 · 2 citations
Engineering · Mathematics · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Binary number #Exoplanet #Mathematics #Metallicity #Physics #Spectral line #Stars #Stellar classification #Stellar, planetary, and galactic studies #White dwarf #astro-ph
paper · pdf · doi:10.1086/508321
published as Astrophys.J.652:1604-1616,2006 · 39 pages, 6 tables, 8 figures, accepted to ApJ
arxiv created 2006/08/03 · openalex publication_date 2006/11/27 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We describe a method for accurately determining M dwarf metallicities with spectral synthesis based on abundance analyses of visual binary stars. We obtained high-resolution, high-signal-to-noise ratio spectra of each component of five visual binary pairs at McDonald Observatory. The spectral types of the components range from F7 to K3 V for the primaries and from M0.5 to M3.5 V for the secondaries. We have determined the metallicities of the primaries differentially with respect to the Sun by fitting synthetic spectra to Fe I line profiles in the observed spectra. In the course of our analysis of the M dwarf secondaries, we have made significant improvements to the PHOENIX cool-star model atmospheres and the spectrum analysis code MOOG. Our analysis yields an rms deviation of 0.11 dex in metallicity values between the binary pairs. We estimate the uncertainties in the derived stellar parameters for the M dwarfs to be 48 K, 0.10 dex, 0.12 dex, 0.15 km s -1 , and 0.20 km s -1 for T eff , log g , [M/H], ξ, and η, respectively. Accurate stellar evolutionary models are needed to progress further in the analysis of cool-star spectra; the new model atmospheres warrant recalculation of the evolutionary models.