The \(3:1\) mean motion resonance between Miranda and the inner Uranian satellites, Cressida and Desdemona

DOI10.1007/S10569-014-9550-YzbMath1298.70013OpenAlexW2059826259MaRDI QIDQ468638

Anne Lemaitre, Emilie Verheylewegen

Publication date: 7 November 2014

Published in: Celestial Mechanics and Dynamical Astronomy (Search for Journal in Brave)

Full work available at URL: https://doi.org/10.1007/s10569-014-9550-y

zbMATH Keywords

oblatenessinner Uranian systemMiranda-Cressida-Drestricted 3-body problem

Mathematics Subject Classification ID

Three-body problems (70F07) Celestial mechanics (70F15)

Cites Work

• The origin of chaotic behaviour in the Miranda-Umbriel 3:1 resonances
• Surfaces of section in the Miranda-Umbriel 3:1 inclination problem
• Solving Ordinary Differential Equations I
• High-order resonances in the restricted three-body problem
• Capture into resonance: An extension of the use of adiabatic invariants
• Solar System Dynamics

This page was built for publication: The \(3:1\) mean motion resonance between Miranda and the inner Uranian satellites, Cressida and Desdemona