Complete spin and orbital evolution of close-in bodies using a Maxwell viscoelastic rheology
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Publication:333826
DOI10.1007/S10569-016-9708-XzbMath1348.70023arXiv1612.02558OpenAlexW3104719339WikidataQ58436210 ScholiaQ58436210MaRDI QIDQ333826
Alexandre C. M. Correia, Jacques Laskar, Gwenaël Boué
Publication date: 31 October 2016
Published in: Celestial Mechanics and Dynamical Astronomy (Search for Journal in Brave)
Full work available at URL: https://arxiv.org/abs/1612.02558
Related Items (11)
Viscoelastic tides: models for use in Celestial Mechanics ⋮ Tidal evolution for any rheological model using a vectorial approach expressed in Hansen coefficients ⋮ Tidal effects in differentiated viscoelastic bodies: a numerical approach ⋮ A direct numerical verification of tidal locking mechanism using the discrete element method ⋮ Tidal synchronization of close-in satellites and exoplanets. III: Tidal dissipation revisited and application to Enceladus ⋮ Tidal synchronization of an anelastic multi-layered body: Titan's synchronous rotation ⋮ Cassini states of a rigid body with a liquid core ⋮ Tidal evolution of the Keplerian elements ⋮ The two rigid body interaction using angular momentum theory formulae ⋮ The effects of deformation inertia (kinetic energy) in the orbital and spin evolution of close-in bodies ⋮ Ellipsoidal equilibrium figure and Cassini states of rotating planets and satellites deformed by a tidal potential in the spatial case
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