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We present the first detailed chemical abundance analysis of the old 8.2 Gyrsolar twin, HIP 102152. We derive differential abundances of 21 elementsrelative to the Sun with precisions as high as 0.004 dex ($\lesssim$1%), usingultra high-resolution (R = 110,000), high S/N UVES spectra obtained on the8.2-m Very Large Telescope. Our determined metallicity of HIP 102152 is [Fe/H]= -0.013 $\pm$ 0.004. The atmospheric parameters of the star were determined tobe 54 K cooler than the Sun, 0.09 dex lower in surface gravity, and amicroturbulence identical to our derived solar value. Elemental abundanceratios examined vs. dust condensation temperature reveal a solar abundancepattern for this star, in contrast to most solar twins. The abundance patternof HIP 02152 appears to be the most similar to solar of any known solar twin.Abundances of the younger, 2.9 Gyr solar twin, 18 Sco, were also determinedfrom UVES spectra to serve as a comparison for HIP 102152. The solar chemicalpattern of HIP 102152 makes it a potential candidate to host terrestrialplanets, which is reinforced by the lack of giant planets in its terrestrialplanet region. The following non-local thermodynamic equilibrium Li abundanceswere obtained for HIP 102152, 18 Sco, and the Sun: log $\epsilon$ (Li) = 0.48$\pm$ 0.07, 1.62 $\pm$ 0.02, and 1.07 $\pm$ 0.02, respectively. The Liabundance of HIP 102152 is the lowest reported to date for a solar twin, andallows us to consider an emerging, tightly constrained Li-age trend for solartwin stars.

High Precision Abundances of the Old Solar Twin HIP 102152: Insights on Li Depletion from the Oldest Sun