Do you know what those extreme avalanche slides are? Even the Hungarian astronomers studied this.

Research examining extreme impact craters in circumstellar disks revealed two primary types of collisions based on the composition of the disks: collisions of high-energy objects between Mars-sized bodies in silicon dioxide-rich disks, and collisions of lunar-sized objects in silicon dioxide-poor systems. These events occurred around stars younger than 300 million years, correlating with the presumed period of protoplanetary disk formation. The discovery was facilitated by data from the James Webb telescope's medium-infrared spectrometer, which allowed researchers to identify dust particles whose size and composition indicated the collision type. The results support models suggesting that silicon dioxide-rich disks are consistent with the formation of the Moon and young Earth through a collision involving a Mars-sized body approximately 100 million years after Solar System formation. Furthermore, the older, silicon dioxide-poor disks suggest a period of late intense bombardment caused by the gravitational influence of gas giants disturbing orbits and causing collisions.

The framework presented contrasts two distinct evolutionary pathways for protoplanetary disk evolution, mediated by compositional differences in the surrounding material. The distinction between silicon dioxide-rich and silicon dioxide-poor systems suggests that the gravitational environment—specifically the presence of massive bodies like gas giants—significantly altered the collision dynamics across different epochs. This implies that the history of Solar System accretion is not monolithic but a spectrum shaped by evolving gravitational influences. The identification of dust particle signatures provides physical evidence linking these theoretical collisional scenarios to observable material properties, moving the discussion from pure orbital mechanics to observable astrophysics. The narrative of early Solar System history is constructed by mapping observed impact types onto disk composition, offering a mechanism for integrating disparate events into a coherent evolutionary sequence. One must consider what biases might favor certain collision models over others when interpreting these compositional correlations; specifically, how does the assumed initial distribution of silicon dioxide correlate with the inferred energetic outcome? What alternative mechanisms for mass redistribution exist that could explain the divergence between late bombardment scenarios and early formation events?