Volume 480, Number 3, March IV 2008
|Page(s)||889 - 897|
|Section||Planets and planetary systems|
|Published online||25 January 2008|
Chemical abundances in six nearby star-forming regions*
Implications for galactic evolution and planet searches around very young stars
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: email@example.com
2 European Southern Observatory (ESO), Casilla 19001, Santiago 19, Chile
3 Department of Physics & Astronomy, Box 1807 Station B, Vanderbilt University, Nashville, TN 37235, USA
4 Departamento de Matemática Aplicada, Faculdade de Ciências da Universidade do Porto, Portugal
5 Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble, France
6 Centro de Astrofísica da Universidade de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal
Accepted: 10 January 2008
In this paper we present a study of chemical abundances in six star-forming regions. Stellar parameters and metallicities are derived using high-resolution, high S/N spectra of weak-line T-Tauri stars in each region. The results show that nearby star-forming regions have a very small abundance dispersion (only 0.033 dex in [Fe/H]). The average metallicity found is slightly below that of the Sun, although compatible with solar once the errors are taken into account. The derived abundances for Si and Ni show that the observed stars have the abundances typical of Galactic thin disk stars of the same metallicity. The impact of these observations is briefly discussed in the context of the Galactic chemical evolution, local inter-stellar medium abundances, and in the origin of metal-rich stars in the solar neighbourhood (namely, stars more likely to harbour planets). The implication for future planet-search programmes around very young, nearby stars is also discussed.
Key words: planetary systems: formation / ISM: abundances / stars: abundances / Galaxy: abundances / solar neighborhood / stars: formation
Based on observations collected at Paranal Observatory, eso (Chile) with the uves and flames/uves spectrographs at the VLT-Kueyen telescope (run IDs 075.C-0272(A) and 076.C-0524(A), respectively), with the feros spectrograph at the eso/mpi 2.2-m telescope (program ID 070.C-0507(A)), as well as with the sophie spectrograph at the ohp observatory, France.
© ESO, 2008
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