tokens: age uncertainties of these stars (that can be substantial as these solar twin stars are located on the upper main sequence). The diagonal line shows the relationship between Li and stellar age from Carlos et al. (2016) . 3.7. Li in stars with planets Since King et al. (1997) claimed a possibility that the low Li abundances in the Sun and 16 Cyg B relative to 16 Cyg A could be due to the presence of planetary companions in the former two, several studies have presented disparate results regarding whether or not stars with detected planets have different Li abundance patterns compared to those with no thus-far detected planets. Studies that support the idea that there is no difference include Ryan (2000) , Luck Heiter (2006) , Baumann et al. (2010) , Ghezzi et al. (2010) , Ramírez et al. (2012) , and Pavlenko et al. (2018) , while those that find that indeed there is a difference include Israelian et al. ( 2004 , 2009 ), Takeda Kawanomoto (2005) , Chen Zhao (2006) , Gonzalez ( 2008 , 2014 , 2015 ), Figueira et al. (2014) , Delgado Mena et al. (2014) , and Mishenina et al. (2016) . To see whether this study can add some further clues to this controversy the exoplanets website 1 ( Han et al. 2014 ) was queried on February 14, 2018. We find that 36 stars in our sample have detected exoplanets, that 18 of those have well-determined Li abundances, and that 6 have upper limit Li detections. These 18 + 6 stars are marked in red in Fig. 8 . They span a range of effective temperatures from about 5600 K to 6500 K. The bottom panel in Fig. 8 shows the differences between the Li abundance of the exoplanet stars and the mean Li abundance of other stars in the sample that have effective temperatures within ±75 K, log g within ±0.25 dex, and [Fe/H] within ±0.25 dex of each exoplanet star. Due to the low number statistics of stars with similar atmospheric parameters at higher T eff , the temperature range was expanded to ±200 K for stars with T eff > 6100 K. As stars at these temperatures have less Li depleted atmospheres, this expansion should not affect the results. The stars with detected exoplanets have on average 0.08 dex higher Li abundances than those without planet detections, with a dispersion of 0.36 dex. Using the median instead gives a Li-enhancement of 0.04 dex. These numbers are well within the uncertainties and our sample reveals no statistically significant difference in Li abundances between stars with and without exoplanet detections. Fig. 8. Upper panel : red circles mark the 18 stars in the sample that have exoplanets detected and good Li measurements. Bottom panel : difference between the A (Li) for individual stars to the mean A (Li) for stars that have no exoplanet detections and that have effective temperatures, surface gravities, and metallicities, within ±75 K, ±0.2 dex, and ±0.2 dex. For stars with T eff > 6100 K, the temperature range is expanded to ±200 K. 3.8. Li trends in the thin and thick disks It is not straightforward
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