期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 423, 期 1, 页码 122-131出版社
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2012.20686.x
关键词
stars: abundances; stars: atmospheres; stars: fundamental parameters; stars: solar-type
资金
- NASA's Science Mission Directorate
- Polish Ministry [N N203 405 139]
- Spanish National Plan of RD [AYA2010-17803]
- Netherlands Organization for Scientific Research (NWO)
- White Dwarf Research Corporation
- US National Science Foundation
- UK Science and Technology Facilities Council (STFC)
- NSF [ATM-1105930]
- STFC [ST/J000035/1, ST/J001163/1, ST/G002355/1, ST/J001384/1, PP/D000955/1, PP/F000057/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/G002355/1, ST/J000035/1, PP/D000955/1, ST/J001384/1, PP/F000057/1, ST/J001163/1] Funding Source: researchfish
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 a 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 accuracy on the log g parameter is better than 0.03 dex and is held fixed in the analysis. We compare our Teff determination with a recent colour calibration of VT-KS [TYCHO V magnitude minus Two Micron All Sky Survey (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 Fe iFe ii balance, although we find a small systematic offset of 0.08 dex (asteroseismic log g values are lower). The abundance patterns of metals, a 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 a-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.
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