Unraveling the mysteries of small-body ring systems through numerical modeling
National Science Foundation
Astronomy and Astrophysics Research Grants Program
PSI Personnel
External Partners
- Trinity U
Project Description
Until 2013, planetary ring systems were only known to exist around the giant planets. We are now aware of three ring systems around minor Solar-System bodies: two narrow rings around Chariklo (a ~250-km diameter centaur), a likely two-ring system around Chiron (a ~215-km diameter centaur), and a single, broad ring around the dwarf planet Haumea (a ~2300x1700x1000-km trans-Neptunian object). These systems are on a significantly smaller scale than the well-known rings and ring arcs around Jupiter, Saturn, Uranus, and Neptune, raising questions about how such modest ring systems form and evolve. Planetary ring material naturally dissipates over time; thus, a critical question is how small-body rings are confined. We propose to use numerical models to study the orbits and characteristics of material around small bodies in our Solar System, specifically investigating ring confinement and structure caused by a shepherd moon. Our methodology is to employ N-body simulations of ring particles moving past a satellite. The model was originally developed for studying the Saturn system, and we have modified it to be applicable at smaller scales. We will verify the model results by using existing data from stellar occultations and other observations of Chariklo and Chiron.
The overarching objective of this proposal is to understand the dynamics of rings systems around minor planets. To reach this goal, we will conduct groundbreaking research to (i) confirm whether a shepherd moon can confine material as observed at Chariklo and Chiron, including constraining the moon’s size and location; (ii) discover the mechanisms and underlying causes of unusual structures or features observed in rings around Chariklo; (iii) parameterize the required conditions (including nucleus size, shape, and spin rate) for rings to be stable around small, axisymmetric bodies; and (iv) compare what we learn about these small-body ring systems with the rings of the giant planets. As a new field of study, very little is known about the underlying orbital dynamics and evolution of rings around minor planets: this work will significantly advance our understanding of these small-scale systems as well as provide insight into the rings around the giant planets. A better understanding of orbital dynamics on a smaller scale could additionally be applicable on a much larger scale, such as for exoplanetary ring systems and protoplanetary disks.