OSSOS. XXI. Collision Probabilities in the EdgeworthKuiper Belt
Abstract
Here, we present results on the intrinsic collision probabilities, P_{I}, and range of collision speeds, V_{I}, as a function of the heliocentric distance, r, in the transNeptunian region. The collision speed is one of the parameters that serves as a proxy for a collisional outcome (e.g., disruption and scattering of fragments, or formation of a crater, as both processes are related to the impact energy). We utilize an improved and debiased model of the transNeptunian object (TNO) region from the "Outer Solar System Origins Survey" (OSSOS). It provides a welldefined model of TNO orbital distribution, based on multiple opposition observations of more than 1000 bodies. We compute collisional probabilities for the OSSOS models of the main classical, resonant, detached+outer, and scattering TNO populations. The intrinsic collision probabilities and collision speeds are computed using Öpik's approach, as revised and modified by Wetherill for noncircular and inclined orbits. The calculations are carried out for each of the dynamical TNO groups, allowing for interpopulation collisions as well as collisions within each TNO population, resulting in 28 combinations in total. Our results indicate that collisions in the transNeptunian region are possible over a wide range in (r, V_{I}) phase space. Although collisions are calculated to happen within r ∼ 20200 au and V_{I} ∼ 0.1 km s^{1} to as high as V_{I} ∼ 9 km s^{1}, most of the collisions are likely to happen at low relative velocities V_{I} < 1 km s^{1} and are dominated by the main classical belt.
 Publication:

The Astronomical Journal
 Pub Date:
 April 2021
 DOI:
 10.3847/15383881/abe418
 arXiv:
 arXiv:2104.14039
 Bibcode:
 2021AJ....161..195A
 Keywords:

 TransNeptunian objects;
 Collision processes;
 Small solar system bodies;
 1705;
 2065;
 Astrophysics  Earth and Planetary Astrophysics
 EPrint:
 13 pages, 6 figures