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Solar twins are stars with similar stellar (surface) parameters to the Sunthat can have a wide range of ages. This provide an opportunity to analyze thevariation of their chemical abundances with age. Nissen (2015) recentlysuggested that the abundances of the s-process element Y and the$\alpha$-element Mg could be used to estimate stellar ages. This paper aims todetermine with high precision the Y, Mg, and Fe abundances for a sample of 88solar twins that span a broad age range ($0.3-10.0$\,Gyr) and investigate theiruse for estimating ages. We obtained high-quality Magellan Inamori KyoceraEchelle (MIKE) spectra and determined Y and Mg abundances using equivalentwidths and a line-by-line differential method within a 1D LTE framework.Stellar parameters and iron abundances were measured in Paper I of this seriesfor all stars, but a few (three) required a small revision. The [Y/Mg] ratioshows a strong correlation with age. It has a slope of -0.041$\pm$0.001 dex/Gyrand a significance of 41 $\sigma$. This is in excellent agreement with therelation first proposed by Nissen (2015). We found some outliers that turnedout to be binaries where mass transfer may have enhanced the yttrium abundance.Given a precise measurement of [Y/Mg] with typical error of 0.02 dex in solartwins, our formula can be used to determine a stellar age with $\sim$0.8 Gyrprecision in the 0 to 10 Gyr range.

The Solar Twin Planet Search III. The [Y/Mg] clock: estimating stellar ages of solar-type stars