size distribution through the extinction curve as well as on the total dust abundance [e.g. @2001PASP..113.1449C], the two aspects of dust (namely, the total dust abundance and the grain size distribution) are important in understanding galaxy evolution.

A comprehensive model that computes the evolution of grain size distribution has been developed by [@2013MNRAS.432..637A], who took into account all major processes that drive the change of grain size distribution in a one-zone model of a galaxy. Dust condenses from the metals ejected from supernovae (SNe) [e.g. @1989ApJ...344..325K; @2001MNRAS.325..726T; @2003ApJ...598..785N; @2007MNRAS.378..973B; @2007ApJ...666..955N] and asymptotic giant branch (AGB) stars . This dust production by stellar sources is the starting point of dust evolution. Calculations of dust condensation and processing in stellar ejecta indicate that grains are biased to large sizes ($a\gtrsim 0.1~\micron$, where $a$ is the grain radius) [@2007ApJ...666..955N; @2012ApJ...745..159Y; @2017MNRAS.467.4431D]. Subsequently, dust grains are processed in the ISM as described by [@2013MNRAS.432..637A] and @2019MNRAS.482.2555H [hereafter HA19]. The interstellar processing starts with shattering, which gradually converts large grains into small ones. As the system is enriched with metals, the accretion of gas-phase metals onto dust grains becomes efficient in the dense ISM. This causes a drastic increase of [ the grain abundance at 