Modeling Recent Asteroid Disruptions in the Solar System
Abstract
We study the dynamical evolutions of the byproducts of recent asteroid disruptions to understand the population of small particles in near-Earth and cislunar space, which can post threats to spacecraft, satellites, and long-term lunar missions like Artemis. To assess this population, we track the dynamical evolution of dust particles created in a catastrophic asteroid disruption. Particle sizes ranging from a few microns to a few cm are modeled using a code that accounts for both the gravitational and radiative forces to accurately predict the orbital elementals of the dust particles in the Datura and Emilkowalski asteroid clusters. The resulting models show that the smaller particles decay into the inner solar system at a faster rate than their larger counterparts, meaning they are more likely to be dispersed throughout the solar system. Comparison of these models with infrared satellite observations allows us to put constraints on the size-distribution and amount of dust present which not only helps us contain the treat these particles may pose, but also understand the amount of surface regolith that was on the parent body asteroids.
Modeling Recent Asteroid Disruptions in the Solar System
We study the dynamical evolutions of the byproducts of recent asteroid disruptions to understand the population of small particles in near-Earth and cislunar space, which can post threats to spacecraft, satellites, and long-term lunar missions like Artemis. To assess this population, we track the dynamical evolution of dust particles created in a catastrophic asteroid disruption. Particle sizes ranging from a few microns to a few cm are modeled using a code that accounts for both the gravitational and radiative forces to accurately predict the orbital elementals of the dust particles in the Datura and Emilkowalski asteroid clusters. The resulting models show that the smaller particles decay into the inner solar system at a faster rate than their larger counterparts, meaning they are more likely to be dispersed throughout the solar system. Comparison of these models with infrared satellite observations allows us to put constraints on the size-distribution and amount of dust present which not only helps us contain the treat these particles may pose, but also understand the amount of surface regolith that was on the parent body asteroids.