Small satellite may shape centaur rings

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Small satellite may shape centaur rings


Small Satellite May Shape Centaur Rings
Cassini spacecraft image of shepherd moons Pandora and Prometheus (each roughly 80 kilometers in diameter) acting on Saturn’s F ring. The satellites’ gravity causes the perturbations shown here, which confines the thin ring. Here, we simulate a single shepherd moon at Chariklo that acts through the same process to confine those rings. Credit: NASA, The National Aeronautics and Space Administration/JPL/Space Science Institute

The unique two thin rings around the Centaur Chariklo can be shaped by an even smaller satellite. Chariklo is a Centaur, which are small bodies similar to asteroids in size but to comets in composition, that revolve around the sun in the outer solar system, mainly between the orbits of Jupiter and Neptune.

“Rings around minor planets have only been recently discovered, and only a small number of such systems are currently known. There has been significant research into the dazzling rings around the giant planets; however, the mechanisms of ring formation and evolution around small objects are not well understood,” said Planetary Science Institute Senior Scientist Amanda Sickafoose, lead author of “Numerical Simulations of (10199) Chariklo’s Rings with a Resonant Perturber” that appears in The Planetary Science Journal.

“We’ve shown that one of the possibilities for thin rings to exist around small bodies is that they are being sculpted by a small satellite.”

The paper reports the first N-body simulations of a small-body ring system with a satellite. N-body simulations are carried out using computer software to simulate the physical dynamics for a number (N) of components. The results from N-body simulations provide insight into the dynamical evolution of the system being modeled.

Small satellite may shape centaur rings
Simulated rings around Chariklo from this research, with an approximate 3 kilometer radius satellite in a 6:5 mean-motion-resonance. Ring particles are shown in white. Two rings are constrained at roughly the same locations and with the same widths as those observed at Chariklo. The inner ring is asymmetric around Chariklo, which is also consistent with stellar occultation data from Chariklo. Our software models millions of ring particles in a cell so this image was created by joining together the values from cells at different times over the course of one orbital period. Credit: Sickafoose & Lewis (2024).

In this case, by modeling a few million ring particles in a Chariklo-like system, it’s shown that a single, kilometer-sized moon can maintain two rings that have similar properties to those observed.

“We think that the ring particles are primarily made of water ice, like those at the giant planets. We do not know the exact characteristics, such as how ‘hard’ or ‘soft’ the ring particles are when they collide or the particle-size distribution. Further simulations can help constrain those properties,” Sickafoose said.

“Planetary rings will naturally spread or disperse over time. Chariklo exhibits two thin rings, a few kilometers in width. In order for the rings to stay this thin, there needs to be a mechanism to confine the material and prevent it from dispersing,” Sickafoose said.

“We actually show this in the paper by simulating a Chariklo-like ring system that does not have a satellite, and we find that the width of the rings increases linearly with time. This is unlike the situation when there is a satellite in resonance with the ring material, which acts to confine the rings into the km-sized widths that are observed.”

Chariklo, approximately 250 kilometers in size, is the first Centaur found to have rings, and they are constrained.

“Our paper shows that Chariklo-like rings can be constrained by a small satellite, one that is roughly 3 kilometers in radius and 1013 kilograms in mass. A satellite this size is below our current direct-imaging limits, so indirect methods or a spacecraft mission might be needed to discover it.”

“An alternate mechanism that has been proposed is that Chariklo has a gravitational anomaly on its surface, and the rings are in resonance with the spin of the nucleus; for every three rotations by Chariklo, the rings orbit once. The physics that act on the ring particles are similar for both a satellite or a spin-orbit resonance with a gravitational anomaly,” Sickafoose said.

“Interestingly, by most reasonable assumptions, Chariklo’s rings are also located near or outside of the Roche limit. The Roche limit is the rough distance beyond which rings should not exist because the material should start accreting into moons—at this distance, the gravitational perturbation from the parent planet is insufficient to shear the particles, and they can form into larger clumps,” Sickafoose said.

“A satellite in this situation can perturb the ring material and prevent it from accreting, similar to what is seen in Saturn’s F ring.”

More information:
Amanda A. Sickafoose et al, Numerical Simulations of (10199) Chariklo’s Rings with a Resonant Perturber, The Planetary Science Journal, (2024). DOI: 10.3847/PSJ/ad151c. iopscience.iop.org/article/10.3847/PSJ/ad151c

Citation:
Small satellite may shape centaur rings (2024, February 6)
retrieved 6 February 2024
from https://phys.org/news/2024-02-small-satellite-centaur.html

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