  Context: The chemical composition of stars is intimately linked to the Galaxy
formation and evolution. Aims: We aim to trace the chemical evolution of the
Galactic disk through the inspection of the [X/Fe]-age relations of 24 species
from C to Eu. Methods: Using high-resolution and high-signal-to-noise UVES
spectra of nine solar twins, we obtained precise estimates of stellar ages and
chemical abundances. These determinations have been integrated with additional
accurate age and abundance determinations from recent spectroscopic studies of
solar twins existing in the literature, comprising superb abundances with
0.01~dex precision. Based on this data set, we outlined the [X/Fe]-age
relations over a time interval of 10~Gyr. Results: We present the [X/Fe] - age
relations for 24 elements (C, O, Na, Mg, Al, Si, S, K, Ca, Sc, Ti, V, Cr, Mn,
Co, Ni, Cu, Zn, Y, Ba, La, Ce, Nd, and Eu). Each different class of elements
showed distinct evolution with time that relies on the different
characteristics, rates and timescales of the nucleosynthesis' sites from which
they are produced. The $\alpha$-elements are characterised by a [X/Fe]
decrement as time goes on. Strikingly, an opposite behaviour is observed for
Ca. The iron-peak elements show an early [X/Fe] increase followed by a decrease
towards the youngest stars. The [X/Fe] for the n-capture elements decrease with
age. We also found that both [Mg/Y] and [Al/Y] are precise stellar clocks, with
[Al/Y] showing the steepest dependence with age. Conslusions: Knowledge of the
[X/Fe]-age relations is a gold mine from which we can achieve a great
understanding about the processes that governed the formation and evolution of
the Milky Way. Through the reverse engineering of these relations we will be
able to put strong constraints on the nature of the stellar formation history,
the SNe rates, the stellar yields, and the variety of the SNe progenitors.
