Discrete element simulations of self-gravitating rubble pile collisions: the effects of non-uniform particle size and rotation

TL;DR

This paper introduces a new simulation code for self-gravitating rubble piles, analyzing how particle size distribution and rotation affect collision outcomes for asteroid-sized bodies.

Contribution

The study develops and validates a novel discrete element simulation method to explore collision effects on rubble pile structures, considering particle size and rotation influences.

Findings

Rubble piles from collisions do not preserve original particle size distribution.

Low-velocity collisions produce larger particles in the remnants.

Rotation, especially aligned spin axes, significantly affects collision outcomes.

Abstract

We present a novel implementation of a soft sphere, discrete elements code to simulate the dynamics of self-gravitating granular materials. The code is used to study the outcome of sub-sonic collisions between self-gravitating rubble piles with masses ranging from $\sim6\times10^{21}$ to $\sim6\times10^{22}$ g. These masses are representative of asteroids and planetesimals in the $\sim100$~km range. We simulate rubble piles composed of a range of particle sizes and analyze the collisions outcome focusing on the properties of the largest surviving fragment. We successfully test and validate the code against previous results. The results of our study show that rubble piles formed by collision of two parent rubble piles do not maintain the same particle size distribution as their parents. Rubble piles formed in low velocity collisions are characterized by a larger fraction of large particles, while the largest fragments of high-velocity collisions show a significant decrease in their mean particle size. We ascribe this effect to the fact that large particles transmit most of the forces during the collisions. In addition, we find that the mass of the largest post-collision fragment does depend on the rotation of the colliding rubble piles. This effect is especially noticeable when the pre-collision spin axes are parallel with each other and perpendicular to the relative velocity. This finding can be particularly relevant for meter to kilometer sized bodies embedded in protostellar accretion disks, where viscous stresses can efficiently align the target and projectile spin axes.