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Chemical abundance variations in the ISM provide important information aboutthe galactic evolution, star-formation and enrichment histories. Recentobservations of disk galaxies suggest that if large-scale azimuthal metallicityvariations appear in the ISM, they are linked to the spiral arms. In this work,using a set of chemodynamical simulations of the Milky Way-like spiralgalaxies, we quantify the impact of gas radial motions~(migration) in thepresence of a pre-existing radial metallicity gradient and the local ISMenrichment on both global and local variations of the mean ISM metallicity inthe vicinity of the spiral arms.  In all the models, we find the scatter of the gas metallicity of\approx0.04-0.06 dex at a given galactocentric distance. On large scales, weobserve the presence of spiral-like metallicity patterns in the ISM which aremore prominent in models with the radial metallicity gradient. However, in oursimulations, the morphology of the large-scale ISM metallicity distributionssignificantly differs from the spiral arms structure in stellar/gas componentsresulting in both positive and negative residual~(after subtraction of theradial gradient) metallicity trends along spiral arms. We discuss thecorrelations of the residual ISM metallicity values with the star formationrate, gas kinematics and offset to the spiral arms, concluding that thepresence of a radial metallicity gradient is essential for the azimuthalvariations of metallicity. At the same time, the local enrichment alone isunlikely to drive systematic variations of the metallicity across the spirals.

astronomy and astrophysics

ISM metallicity variations across spiral arms in disk galaxies: the  impact of local enrichment and gas migration in the presence of radial  metallicity gradient