The presence of possible blends in the spectral region of the Li resonance line at 6708 Ã Â 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 à  with the low excitation 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 Si i line originally proposed by Müller et al. ( 1975 ) .
Reanalysis of the ^ { 6 } Li/ ^ { 7 } Li isotopic ratio in HD 82943 was performed by taking the 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 ^ { 6 } Li in the star ’ s atmosphere while the updated value for the isotopic ratio is f ( ^ { 6 } Li ) = 0.05 \pm 0.02 .