EDP Sciences
Free Access
Issue
A&A
Volume 508, Number 1, December II 2009
Page(s) L17 - L20
Section Letters
DOI https://doi.org/10.1051/0004-6361/200913038
Published online 12 November 2009
A&A 508, L17-L20 (2009)
DOI: 10.1051/0004-6361/200913038

Letter

Accurate abundance patterns of solar twins and analogs

Does the anomalous solar chemical composition come from planet formation?
I. Ramírez1, J. Meléndez2, and M. Asplund1

1  Max Planck Institute for Astrophysics, Postfach 1317, 85741 Garching, Germany
    e-mail: ivan@mpa-garching.mpg.de
2  Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal

Received 31 July 2009 / Accepted 7 November 2009

Abstract
We derive the abundance of 19 elements in a sample of 64 stars with fundamental parameters very similar to solar, which minimizes the impact of systematic errors in our spectroscopic 1D-LTE differential analysis, using high-resolution ( $R\simeq60\,000$), high signal-to-noise ratio ( $S/N\simeq200$) spectra. The estimated errors in the elemental abundances relative to solar are as small as $\simeq$0.025 dex. The abundance ratios [X/Fe] as a function of ${\rm [Fe/H]}$ agree closely with previously established patterns of Galactic thin-disk chemical evolution. Interestingly, the majority of our stars show a significant correlation between [X/Fe] and condensation temperature ($T_{\rm C}$). In the sample of 22 stars with parameters closest to solar, we find that, on average, low $T_{\rm C}$ elements are depleted with respect to high $T_{\rm C}$ elements in the solar twins relative to the Sun by about 0.08 dex ($\simeq$$20\%$). An increasing trend is observed for the abundances as a function of $T_{\rm C}$ for $900<T_{\rm C}<1800$ K, while abundances of lower $T_{\rm C}$ elements appear to be roughly constant. We speculate that this is a signature of the planet formation that occurred around the Sun but not in the majority of solar twins. If this hypothesis is correct, stars with planetary systems like ours, although rare (frequency of $\simeq$15%), may be identified through a very detailed inspection of the chemical compositions of their host stars.


Key words: stars: abundances -- Sun: abundances -- planetary systems



© ESO 2009

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