Accurate M Dwarf Metallicities from Spectral Synthesis: A Critical Test of Model Atmospheres

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dc.creatorBean, Jacob L.
dc.creatorSneden, Christopher
dc.creatorHauschildt, Peter H.
dc.creatorJohns-Krull, Christopher M.
dc.creatorBenedict, G. Fritz
dc.date2006-08-03
dc.date.accessioned2026-07-07T10:39:43Z
dc.date.available2026-07-07T10:39:43Z
dc.descriptionWe 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 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 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 \textsc{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 a 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 \textsl{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.
dc.description39 pages, 6 tables, 8 figures, accepted to ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0608093
dc.identifierhttp://arxiv.org/abs/astro-ph/0608093
dc.identifierAstrophys.J.652:1604-1616,2006
dc.identifierdoi:10.1086/508321
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/181125
dc.subjectAstrophysics
dc.titleAccurate M Dwarf Metallicities from Spectral Synthesis: A Critical Test of Model Atmospheres
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