EDP Sciences
Free Access
Volume 405, Number 2, July II 2003
Page(s) 753 - 762
Section Formation and evolution of planetary systems
DOI https://doi.org/10.1051/0004-6361:20030591
Published online 19 June 2003

A&A 405, 753-762 (2003)
DOI: 10.1051/0004-6361:20030591

New measurement of the $\mathsf{^6Li/^7Li}$ isotopic ratio in the extra-solar planet host star HD 82943 and line blending in the Li 6708 Å region

G. Israelian1, N. C. Santos2, 3, M. Mayor2 and R. Rebolo1

1  Insituto de Astrofisica de Canarias, 38205 La Laguna, Tenerife, Spain
2  Observatoire de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland
3  Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal

(Received 7 October 2002 / Accepted 14 April 2003)

The presence of possible blends in the spectral region of the Li resonance line at 6708 Å in solar-type metal-rich stars is investigated using high resolution and high signal-to-noise spectroscopic observations. Our analysis does not confirm the identification of a weak absorption feature at 6708.025 Å with the low excitation $\ion{Ti}{i}$ line proposed by Reddy et al. (2002). Our spectrum synthesis suggests that the unidentified absorption is most probably produced by a high excitation $\ion{Si}{i}$ line originally proposed by Müller et al. (1975). Reanalysis of the 6Li/ 7Li isotopic ratio in HD 82943 was performed by taking the $\ion{Si}{i}$ line into account and using new VLT/UVES spectra of HD 82943 with a signal-to-noise ratio close to 1000. We confirm the presence of  6Li in the star's atmosphere while the updated value for the isotopic ratio is $f(^6\rm Li) = 0.05\pm0.02$.

Key words: stars: abundances -- stars: chemically peculiar -- line: identification -- line: profiles

Offprint request: G. Israelian, gil@iac.es

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© ESO 2003

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