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Constraints on Mimas’ interior from Cassini ISS libration measurements
TLDR
The precise difference between rotational and orbital periods suggests an unexpected interior for one of Saturn’s moons, and it is argued that the satellite has either a large nonhydrostatic interior, or a hydrostatic one with an internal ocean beneath a thick icy shell.
Uranus Pathfinder: exploring the origins and evolution of Ice Giant planets
The “Ice Giants” Uranus and Neptune are a different class of planet compared to Jupiter and Saturn. Studying these objects is important for furthering our understanding of the formation and evolution
The rotation of Mimas
Context. The Cassini mission in the Saturnian system is an outstanding opportunity to improve our knowledge of the satellites of Saturn. The data obtained thanks to this mission must be balanced with
Tilting Styx and Nix but not Uranus with a Spin-Precession-Mean-motion resonance
TLDR
A Hamiltonian model is constructed for the spin axis of a planet perturbed by a nearby planet with both planets in orbit about a star and explains how Styx and Nix can be tilted to high obliquity via outward migration of Charon.
A numerical exploration of Miranda's dynamical history
The Uranian satellite Miranda presents a high inclination (4.338 ◦ ) and evidences of resurfacing. It is accepted since 20 years (e.g. Tittemore and Wisdom 1989, Malhotra and Dermott 1990) that this
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