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We present a multi-zone galactic chemical evolution (GCE) model for the MilkyWay that takes the most recently updated yields of major nucleosynthesischannels into account. It incorporates physical processes commonly found inprevious GCE models like supernova and star formation feedback, the radial flowof gas in the disk, and the infall of fresh gas, along with stellar scatteringprocesses like radial migration. We individually analyse the effect ofdifferent physical processes present in our model on the observed properties ofthe Galaxy. The radial flow of gas in the disk plays an important role inestablishing the radial gradient for \feh{} in the low-\alphafe{} sequence. Ourmodel with one episode of smooth gas infall and constant star formationefficiency is capable of reproducing the observed \fehalpha{} distribution ofstars at different ($R$, $|z|$) positions in the Milky Way. Our results pointto the rapid evolution of \alphafe{} after the onset of Type Ia supernovae anda high star formation rate during the formation of the high-\alphafe{} sequenceas the origin of dual peaks in \alphafe{}. A secondary infall is unnecessary toreproduce the \alphafe{}-gap and chemical spread in the disk in our model. Weadditionally compare the median age for various mono-abundance populations andthe age-metallicity relation at different ($R$, $|z|$) positions from ourfiducial model to observations. We discuss our results in relation to otherrelated work in detail.

Chemical Evolution with Radial Mixing Redux: Extending beyond the Solar Neighborhood