EDP Sciences
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Volume 458, Number 3, November II 2006
Page(s) 997 - 1005
Section Planets and planetary systems
DOI http://dx.doi.org/10.1051/0004-6361:20065683

A&A 458, 997-1005 (2006)
DOI: 10.1051/0004-6361:20065683

Chemical abundances for the transiting planet host stars OGLE-TR-10, 56, 111, 113, 132, and TrES-1

Abundances in different galactic populations
N. C. Santos1, 2, 3, A. Ecuvillon4, G. Israelian4, M. Mayor2, C. Melo5, D. Queloz2, S. Udry2, J. P. Ribeiro1 and S. Jorge1

1  Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal
    e-mail: nuno@oal.ul.pt
2  Observatoire de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
3  Centro de Geofisica de Évora, Rua Romão Ramalho 59, 7002-554 Évora, Portugal
4  Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
5  European Southern Observatory, Casilla 19001, Santiago 19, Chile

(Received 24 May 2006 / Accepted 22 June 2006 )

Aims.We used the UVES spectrograph (VLT-UT2 telescope) to obtain high-resolution spectra of 6 stars hosting transiting planets, namely for OGLE-TR-10, 56, 111, 113, 132, and TrES-1. These spectra are now used to derive and discuss the chemical abundances for C, O, Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, and Zn.
Methods.Abundances were derived in LTE, using 1D plane-parallel Kurucz model atmospheres. For S, Zn, and Cu, we used a spectral synthesis procedure, while for the remaining cases the abundances were derived from measurements of line-equivalent widths.
Results.The resulting abundances were compared with those found for stars in the solar neighborhood. Distances and galactic coordinates were estimated for the stars. We conclude that, besides being particularly metal-rich and with small possible exceptions, OGLE-TR-10, 56, 111, 113, 132, and TrES-1 are chemically undistinguishable from the field (thin disk) stars regarding their [X/Fe] abundances. This is particularly relevant for the most distant of the targets, located up to ~2 kpc from the Sun. We also did not find any correlation between the abundances and the condensation temperature of the elements, evidence that strong accretion of planetary-like material, tentatively connected to planetary migration, did not occur.

Key words: stars: abundances -- stars: fundamental parameters -- stars: planetary systems -- Galaxy: abundances -- stars: solar neighbourhood

© ESO 2006

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