The fate of primordial asteroids largely depended on their size and the energy of the collisions they experienced. Larger planetesimals, with greater gravitational forces, had a higher chance of surviving collisions without significant fragmentation or merging. Smaller planetesimals, on the other hand, were more susceptible to being shattered into fragments or merging with other bodies. Over time, this resulted in the survival of a certain size range of primordial asteroids that had sufficient strength and stability to resist breakup.
The similarity in size among the surviving primordial asteroids can be attributed to a number of factors. Firstly, the process of gravitational collapse during the early stages of planetary formation favored the formation of bodies within a specific size range. Secondly, the energy imparted by frequent collisions between planetesimals imposed an upper limit on their size. Large planetesimals that collided with excessive force could fracture or even be completely disrupted. Thirdly, smaller planetesimals had a greater tendency to merge or be accreted by larger bodies, further depleting their numbers.
As the Solar System continued to evolve, gravitational interactions between these similar-sized planetesimals, along with other complex dynamical processes, led to further sorting and merging, resulting in the formation of planets and larger bodies. The remnants of these primordial asteroids can be observed today in the form of asteroids and comets. By studying these objects, astronomers gain valuable insights into the early stages of our planetary system and the intricate processes that shaped its formation.
