13 chemical abundances (H, He, C, N, O, Ne, Mg, Si, S, Ca, Fe, Ni, and Eu). The ejection of metals and energy from stars are treated separately for SNe Ia, II, and AGB stars as a function of time after the onset of star formation. The delay-time distribution function of SN Ia rate is modeled with a power-law of $t^{-1}$ [@2008PASJ...60.1327T; @2012PASA...29..447M]. In comparison, in A17, the metal and dust were injected instantaneously after 4Myr from the onset of star formation, whose masses were simply proportional to the stellar mass. For more details of the stellar feedback with CELib in our simulations, we refer the interested reader to @2019MNRAS.484.2632S. We further describe the dust enrichment by stellar sources in the next subsection.

Evolution of grain size distribution {#subsec:size_distribution}
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We use the same model as in HA19 for the evolution of grain size distribution. The model is based on [@2013MNRAS.432..637A], but with simplifications that do not lose the physical essence of the relevant processes. These simplifications are useful for the implementation in hydrodynamic simulations. For the dust evolution processes, we consider stellar dust production, dust destruction by SN shocks in the ISM, dust growth by accretion and coagulation in 