Spitoni, E.E.SpitoniSilva Aguirre, V.V.Silva AguirreMatteucci, F.F.MatteucciCALURA, FrancescoFrancescoCALURAGRISONI, ValeriaValeriaGRISONI2021-04-272021-04-2720190004-6361http://hdl.handle.net/20.500.12386/30932Context. Precise stellar ages from asteroseismology have become available and can help to set stronger constraints on the evolution of the Galactic disc components. Recently, asteroseismology has confirmed a clear age difference in the solar annulus between two distinct sequences in the [α/Fe] versus [Fe/H] abundance ratios relation: the high-α and low-α stellar populations. <BR /> Aims: We aim to reproduce these new data with chemical evolution models including different assumptions for the history and number of accretion events. <BR /> Methods: We tested two different approaches: a revised version of the "two-infall" model where the high-α phase forms by a fast gas accretion episode and the low-α sequence follows later from a slower gas infall rate, and the parallel formation scenario where the two disc sequences form coevally and independently. <BR /> Results: The revised two-infall model including uncertainties in age and metallicity is capable of reproducing: i) the [α/Fe] versus [Fe/H] abundance relation at different Galactic epochs, ii) the age-metallicity relation and the time evolution [α/Fe]; iii) the age distribution of the high-α and low-α stellar populations, iv) the metallicity distribution function. The parallel approach is not capable of properly reproducing the stellar age distribution, in particular at old ages. <BR /> Conclusions: The best chemical evolution model is the revised two-infall one, where a consistent delay of ∼4.3 Gyr in the beginning of the second gas accretion episode is a crucial assumption to reproduce stellar abundances and ages.STAMPAenArticle10.1051/0004-6361/2018341882-s2.0-85062854631http://arxiv.org/abs/1809.00914v2https://www.aanda.org/articles/aa/full_html/2019/03/aa34188-18/aa34188-18.html2019A&A...623A..60SFIS/05 - ASTRONOMIA E ASTROFISICA