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Investigations of the origin and evolution of the Milky Way disk have longrelied on chemical and kinematic identification of its components toreconstruct our Galactic past. Difficulties in determining precise stellar ageshave restricted most studies to small samples, normally confined to the solarneighbourhood. Here we break this impasse with the help of asteroseismicinference and perform a chronology of the evolution of the disk throughout theage of the Galaxy. We chemically dissect the Milky Way disk population using asample of red giant stars spanning out to 2~kpc in the solar annulus observedby the {\it Kepler} satellite, with the added dimension of asteroseismic ages.Our results reveal a clear difference in age between the low- and high-$\alpha$populations, which also show distinct velocity dispersions in the $V$ and $W$components. We find no tight correlation between age and metallicity nor[$\alpha$/Fe] for the high-$\alpha$ disk stars. Our results indicate that thiscomponent formed over a period of more than 2~Gyr with a wide range of [M/H]and [$\alpha$/Fe] independent of time. Our findings show that the kinematicproperties of young $\alpha$-rich stars are consistent with the rest of thehigh-$\alpha$ population and different from the low-$\alpha$ stars of similarage, rendering support to their origin being old stars that went through a masstransfer or stellar merger event, making them appear younger, instead ofmigration of truly young stars formed close to the Galactic bar.

Confirming chemical clocks: asteroseismic age dissection of the Milky Way disk(s)