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The use of abundance ratios involving Y, or other slow-neutron captureelements, are routinely used to infer stellar ages.Aims.We aim to explain theobserved [Y/H] and [Y/Mg] abundance ratios of star clusters located in theinner disc with a new prescription for mixing in Asymptotic Giant Branch (AGB)stars. In a Galactic chemical evolution model, we adopt a new set of AGBstellar yields in which magnetic mixing is included. We compare the results ofthe model with a sample of abundances and ages of open clusters located atdifferent Galactocentric distances. The magnetic mixing causes a less efficientproduction of Y at high metallicity. A non-negligible fraction of stars withsuper-solar metallicity is produced in the inner disc, and their Y abundancesare affected by the reduced yields. The results of the new AGB modelqualitatively reproduce the observed trends for both [Y/H] and [Y/Mg] vs age atdifferent Galactocetric distances. Our results confirm from a theoretical pointof view that the relationship between [Y/Mg] and stellar age cannot beuniversal, i.e., the same in every part of the Galaxy. It has a strongdependence on the star formation rate, on the s-process yields and theirrelation with metallicity, and thus it varies across the Galactic disc.

Magnetic-buoyancy-induced mixing in AGB Stars: a theoretical explanation of the non-universal [Y/Mg]-age relation