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19 April 2024

» arxiv » 1203.0611

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Accurate parameters of 93 solar-type Kepler targets
H. Bruntt ; S. Basu ; B. Smalley ; W. J. Chaplin ; G. A. Verner ; T. R. Bedding ; C. Catala ; J.-C. Gazzano ; J. Molenda-Zakowicz ; A. O. Thygesen ; K. Uytterhoeven ; S. Hekker ; D. Huber ; C. Karoff ; S. Mathur ; B. Mosser ; T. Appourchaux ; T. L. Campante ; Y. Elsworth ; R. A. Garcia ; R. Handberg ; T. S. Metcalfe ; P.-O. Quirion ; C. Regulo ; I. W. Roxburgh ; D. Stello ; J. Christensen-Dalsgaard ; S. D. Kawaler ; H. Kjeldsen ; R. L. Morris ; E. V. Quintana ; D. T. Sanderfer ;
Date:	3 Mar 2012
Abstract:	We present a detailed spectroscopic study of 93 solar-type stars that are targets of the NASA/Kepler mission and provide detailed chemical composition of each target. We find that the overall metallicity is well-represented by Fe lines. Relative abundances of light elements (CNO) and alpha-elements are generally higher for low-metallicity stars. Our spectroscopic analysis benefits from the accurately measured surface gravity from the asteroseismic analysis of the Kepler light curves. The log g parameter is known to better than 0.03 dex and is held fixed in the analysis. We compare our Teff determination with a recent colour calibration of V-K (TYCHO V magnitude minus 2MASS Ks magnitude) and find very good agreement and a scatter of only 80 K, showing that for other nearby Kepler targets this index can be used. The asteroseismic log g values agree very well with the classical determination using Fe1-Fe2 balance, although we find a small systematic offset of 0.08 dex (asteroseismic log g values are lower). The abundance patterns of metals, alpha elements, and the light elements (CNO) show that a simple scaling by [Fe/H] is adequate to represent the metallicity of the stars, except for the stars with metallicity below -0.3, where alpha-enhancement becomes important. However, this is only important for a very small fraction of the Kepler sample. We therefore recommend that a simple scaling with [Fe/H] be employed in the asteroseismic analyses of large ensembles of solar-type stars.
Source:	arXiv, 1203.0611
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