In the age of high-resolution spectroscopic stellar surveys of the Milky Way , the number of stars with detailed abundances of multiple elements is rapidly increasing . These elemental abundances are directly influenced by the evolutionary history of the Galaxy , but this can be difficult to interpret without an absolute timeline of the abundance enrichment . We present age-abundance trends for [ M/H ] , [ \alpha /M ] , and 17 individual elements using a sample of 721 solar neighbourhood Hipparcos red giant stars observed by APOGEE . These age trends are determined through a Bayesian hierarchical modelling method presented by . We confirm that the [ \alpha /M ] -age relation in the solar neighbourhood is steep and relatively narrow ( 0.20 dex age dispersion ) , as are the [ O/M ] - and [ Mg/M ] -age relations . The age trend of [ C/N ] is steep and smooth , consistent with stellar evolution . The [ M/H ] -age relation has a mean age dispersion of 0.28 dex and a complex overall structure . The oldest stars in our sample are those with the lowest and highest metallicities , while the youngest stars are those with solar metallicity . These results provide strong constraints on theoretical models of Galactic chemical evolution ( GCE ) . We compare them to the predictions of one-zone GCE models and multi-zone mixtures , both analytic and numerical . These comparisons support the hypothesis that the solar neighbourhood is composed of stars born at a range of Galactocentric radii , and that the most metal-rich stars likely migrated from a region with earlier and more rapid star formation such as the inner Galaxy .