Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology
arXiv:1411.1860 · doi:10.1051/0004-6361/201424211
Abstract
In this paper we present a new approach to tidal theory. Assuming a Maxwell viscoelastic rheology, we compute the instantaneous deformation of celestial bodies using a differential equation for the gravity field coefficients. This method allows large eccentricities and it is not limited to quasi-periodic perturbations. It can take into account an extended class of perturbations, including chaotic motions and transient events. We apply our model to some already detected eccentric hot Jupiters and super-Earths in planar configurations. We show that when the relaxation time of the deformation is larger than the orbital period, spin-orbit equilibria arise naturally at half-integers of the mean motion, even for gaseous planets. In the case of super-Earths, these equilibria can be maintained for very low values of eccentricity. Our method can also be used to study planets with complex internal structures and other rheologies.
16 pages, 13 figures, 2 tables
References in corpus (4)
Cited by in corpus (30)
- Obliquity-Driven Sculpting of Exoplanetary Systems
- Tidally-Induced Radius Inflation of Sub-Neptunes
- Formation of Ultra-Short-Period Planets by Obliquity-Driven Tidal Runaway
- Why do warm Neptunes present nonzero eccentricity?
- Tidal Inflation Reconciles Low-Density Sub-Saturns with Core Accretion
- Complete spin and orbital evolution of close-in bodies using a Maxwell viscoelastic rheology
- Secular and tidal evolution of circumbinary systems
- Post-main-sequence debris from rotation-induced YORP break-up of small bodies II: multiple fissions, internal strengths and binary production
- Self-Consistent Spin, Tidal and Dynamical Equations of Motion in the REBOUNDx Framework
- Detectability of shape deformation in short-period exoplanets
- Spin-orbit coupling for close-in planets
- The small and large lags of the elastic and anelastic tides. The virtual identity of two rheophysical theories
- Tidal excitation of the obliquity of Earth-like planets in the habitable zone of M-dwarf stars
- Atmospheric stability and collapse on tidally locked rocky planets
- A generic frequency dependence for the atmospheric tidal torque of terrestrial planets
- Thermal and orbital evolution of low-mass exoplanets
- The tidal parameters of TRAPPIST-1 b and c
- Spin dynamics of close-in planets exhibiting large TTVs
- Tidal evolution for any rheological model using a vectorial approach expressed in Hansen coefficients
- Tidal synchronization of an anelastic multi-layered body: Titan's synchronous rotation
- Is the orbital distribution of multiplanet systems influenced by pure three-planet resonances?
- An Empirical Fit for Viscoelastic Simulations of Tertiary Tides
- Tidal evolution of exoplanetary systems hosting Potentially Habitable Exoplanets. The cases of LHS-1140 b-c and K2-18 b-c
- Coupled orbital and spin evolution of the CoRoT-7 two-planet system using a Maxwell viscoelastic rheology
- Tidal evolution of the Pluto-Charon binary
- Rotation and figure evolution in the creep tide theory. A new approach and application to Mercury
- Tidal evolution of Earth-like planets in the habitable zone of low-mass stars
- Ellipsoidal equilibrium figure and Cassini states of rotating planets and satellites deformed by a tidal potential in the spatial case
- Exoplanets synchronization in the habitable zone: Learning from Venus' retrograde rotation
- The Resonant Tidal Evolution of the Earth-Moon Distance