Dust grain shattering in protoplanetary discs: collisional fragmentation or rotational disruption?

In protoplanetary discs, the coagulation of dust grains into large aggregates still remains poorly understood. Grain porosity appears to be a promising solution allow survive and form planetesimals. Furthermore, shattering has generally been considered come only from collisional fragmentation; however, new process was recently introduced, rotational disruption. We wrote one-dimensional code that models growth evolution as they drift study their final outcome when two processes are included. When simulating in disc model reproduces observations, we find disruption is not negligible compared fragmentation radial drift. Disruption becomes dominant turbulence parameter $\alpha \lesssim 5\xtenpow{-4}$, if slow enough. show importance history strongly depends on tensile strength.