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Shattering of dust grains in the interstellar medium is a viable mechanism ofsmall grain production in galaxies. We examine the robustness or uncertainty inthe theoretical predictions of shattering. We identify $P_1$ (the criticalpressure above which the deformation destroys the original lattice structures)as the most important quantity in determining the timescale of small grainproduction, and confirm that the same $P_1/t$ ($t$ is the duration ofshattering) gives the same grain size distribution [$n(a)$, where $a$ is thegrain radius] after shattering within a factor of 3. The uncertainty in thefraction of shocked material that is eventually ejected as fragments causesuncertainties in $n(a)$ by a factor of 1.3 and 1.6 for silicate andcarbonaceous dust, respectively. The size distribution of shattered fragmentshave minor effects as long as the power index of the fragment size distributionis less than ~ 3.5, since the slope of grain size distribution $n(a)$continuously change by shattering and becomes consistent with $n(a)\proptoa^{-3.5}$. The grain velocities as a function of grain radius can have animprint in the grain size distribution especially for carbonaceous dust. Wealso show that the formulation of shattering can be simplified without losingsufficient precision.

Evolution of dust grain size distribution by shattering in the interstellar medium: robustness and uncertainty