摘要：Shattering of dust grains in the interstellar medium is a viable mechanism of small grain production in galaxies.We examine the robustness or uncertainty in the theoretical predictions of shattering.We identify P 1 (the critical pressure above which the deformation destroys the original lattice structures) as the most important quantity in determining the timescale of small grain production, and confirm that the same P 1/ t ( t is the duration of shattering) gives the same grain size distribution [ n ( a ), where a is the grain radius] after shattering within a factor of 3.The uncertainty in the fraction of shocked material that is eventually ejected as fragments causes uncertainties in n ( a ) by a factor of 1.3 and 1.6 for silicate and carbonaceous dust, respectively.The size distribution of shattered fragments have minor effects as long as α f ≲ 3.5 (the size distribution of shattered fragments \( \propto a^{ - \alpha _{\text{f}} } \) ), since the slope of grain size distribution n ( a ) continuously changes by shattering and becomes consistent with n ( a ) ∝ a −3.5.The grain velocities as a function of grain radius can have an imprint in the grain size distribution especially for carbonaceous dust.We also show that the formulation of shattering can be simplified without losing sufficient precision. Key words Cosmic dust galaxy evolution grain size distribution interstellar medium.
关键词：Cosmic dust ;galaxy evolution ;grain size distribution ;interstellar medium
