Chemical Composition of the Planet-harboring Star TrES-1
| Autor: | Guillermo Torres, Bruce W. Carney, David Yong, David W. Latham, John B. Laird, Alessandro Sozzetti |
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| Rok vydání: | 2006 |
| Předmět: |
Physics
Metallicity Milky Way Astrophysics (astro-ph) FOS: Physical sciences Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics 01 natural sciences Exoplanet Accretion (astrophysics) Stars Thin disk 13. Climate action Space and Planetary Science Planet 0103 physical sciences Thick disk Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics 010306 general physics 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics |
| Zdroj: | NASA Astrophysics Data System |
| ISSN: | 1538-3881 0004-6256 |
| Popis: | We present a detailed chemical abundance analysis of the parent star of the transiting extrasolar planet TrES-1. Based on high-resolution Keck/HIRES and HET/HRS spectra, we have determined abundances relative to the Sun for 16 elements (Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, Zn, Y, and Ba). The resulting average abundance of $$ $= -0.02\pm0.06$ is in good agreement with initial estimates of solar metallicity based on iron. We compare the elemental abundances of TrES-1 with those of the sample of stars with planets, searching for possible chemical abundance anomalies. TrES-1 appears not to be chemically peculiar in any measurable way. We investigate possible signs of selective accretion of refractory elements in TrES-1 and other stars with planets, and find no statistically significant trends of metallicity [$X$/H] with condensation temperature $T_c$. We use published abundances and kinematic information for the sample of planet-hosting stars (including TrES-1) and several statistical indicators to provide an updated classification in terms of their likelihood to belong to either the thin disk or the thick disk of the Milky Way Galaxy. TrES-1 is found to be a very likely member of the thin disk population. By comparing $\alpha$-element abundances of planet hosts and a large control sample of field stars, we also find that metal-rich ([Fe/H]$\gtrsim 0.0$) stars with planets appear to be systematically underabundant in [$\alpha$/Fe] by $\approx 0.1$ dex with respect to comparison field stars. The reason for this signature is unclear, but systematic differences in the analysis procedures adopted by different groups cannot be ruled out. Comment: 52 pages, 15 figures, 5 tables, accepted for publication in the Astronomical Journal |
| Databáze: | OpenAIRE |
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