Dynamical Evidence for a Late Formation of Saturn's Moons
Matija \'Cuk, Luke Dones, David Nesvorn\'y

TL;DR
This paper suggests Saturn's moons are much younger than the planet, likely formed about 100 million years ago from a debris disk, challenging the idea that they are primordial and explaining their current orbital configurations.
Contribution
It introduces a new formation scenario for Saturn's moons involving recent re-accretion from a debris disk triggered by orbital instability.
Findings
The Tethys-Dione 3:2 resonance likely did not occur in the past.
The moons' orbital inclinations indicate crossing the Dione-Rhea resonance.
Most craters on interior moons are from planetocentric impactors.
Abstract
We explore the past evolution of Saturn's moons using direct numerical integrations. We find that the past Tethys-Dione 3:2 orbital resonance predicted in standard models likely did not occur, implying that the system is less evolved than previously thought. On the other hand, the orbital inclinations of Tethys, Dione and Rhea suggest that the system did cross the Dione-Rhea 5:3 resonance, which is closely followed by a Tethys-Dione secular resonance. A clear implication is that either the moons are significantly younger than the planet, or that their tidal evolution must be extremely slow (Q > 80,000). As an extremely slow-evolving system is incompatible with intense tidal heating of Enceladus, we conclude that the moons interior to Titan are not primordial, and we present a plausible scenario for the system's recent formation. We propose that the mid-sized moons re-accreted from a…
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