Fig. 5.From: Evolution of dust grain size distribution by shattering in the interstellar medium: Robustness and uncertaintyTime evolution of grain size distribution for Models F and G in Panels (a) and (b), respectively, for carbonaceous dust. The thin solid, dashed, dot-dashed, and thick solid lines represent t = 10, 20, 40, and 80 Myr, respectively. The dotted line presents the initial grain size distribution before shattering.Back to article page