MAGRINI, LAURALAURAMAGRINIVESCOVI, DiegoDiegoVESCOVICasali, G.G.CasaliCRISTALLO, SergioSergioCRISTALLOViscasillas Vázquez, C.C.Viscasillas VázquezCESCUTTI, GABRIELEGABRIELECESCUTTISpina, L.L.SpinaVAN DER SWAELMEN, Mathieu Benoit JeanMathieu Benoit JeanVAN DER SWAELMENRANDICH, Maria SofiaMaria SofiaRANDICH2022-03-112022-03-1120210004-6361http://hdl.handle.net/20.500.12386/31548Context. Abundance ratios involving Y or other slow-neutron capture elements are routinely used to infer stellar ages. <BR /> Aims: We aim to explain the observed [Y/H] and [Y/Mg] abundance ratios of star clusters located in the inner disc with a new prescription for mixing in asymptotic giant branch (AGB) stars. <BR /> Methods: In a Galactic chemical evolution model, we adopted a new set of AGB stellar yields in which magnetic mixing was included. We compared the results of the model with a sample of abundances and ages of open clusters located at different Galactocentric distances. <BR /> Results: The magnetic mixing causes a less efficient production of Y at high metallicity. A non-negligible fraction of stars with super-solar metallicity is produced in the inner disc, and their Y abundances are affected by the reduced yields. The results of the new AGB model qualitatively reproduce the observed trends for both [Y/H] and [Y/Mg] versus age at different Galactocetric distances. <BR /> Conclusions: Our results confirm from a theoretical point of view that the relation between [Y/Mg] and stellar age cannot be `universal', that is, cannot be the same in every part of the Galaxy. It has a strong dependence on the star formation rate, on the s-process yields, and on their relation with metallicity, and it therefore varies throughout the Galactic disc.STAMPAenArticle10.1051/0004-6361/2020401152-s2.0-85100422851WOS:000616953800001https://www.aanda.org/articles/aa/full_html/2021/02/aa40115-20/aa40115-20.htmlhttp://arxiv.org/abs/2101.04429v12021A&A...646L...2MFIS/05 - ASTRONOMIA E ASTROFISICA