2003A&A...405..753I

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 6708.025Å with the low excitation TiI line proposed by Reddy et al. (2002MNRAS.335.1005R). Our spectrum synthesis suggests that the unidentified absorption is most probably produced by a high excitation SiI line originally proposed by Mueller et al. (1975SoPh...41...53M). Reanalysis of the ⁶Li/⁷Li isotopic ratio in HD82943 was performed by taking the SiI line into account and using new VLT/UVES spectra of HD82943 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(⁶Li)=0.05±0.02.