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Using idealised N-body simulations of a Milky Way-sized disc galaxy, wequalitatively study how the metallicity distributions of the thin disc starparticles are modified by the formation of the bar and spiral arm structures.The thin disc in our numerical experiments initially has a tight negativeradial metallicity gradient and a constant vertical scale-height. We show thatthe radial mixing of stars drives a positive vertical metallicity gradient inthe thin disc. On the other hand, if the initial thin disc is flared, withvertical scale-height increasing with galactocentric radius, the metal poorstars originally in the outer disc become dominant in regions above the discplane at every radii. This process can drive a negative vertical metallicitygradient, which is consistent with the current observed trend. This modelmimics a scenario where the star-forming thin disc was flared in the outerregion at earlier epochs. Our numerical experiment with an initial flared discpredicts that the negative vertical metallicity gradient of the mono-agerelatively young thin disc population should be steeper in the inner disc, andthe radial metallicity gradient of the mono-age population should be shallowerat greater heights above the disc plane. We also predict that the metallicitydistribution function of mono-age young thin disc populations above the discplane would be more positively skewed in the inner disc compared to the outerdisc.

Impacts of a Flaring Star-forming Disc and Stellar Radial Mixing on the Vertical Metallicity Gradient