Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology

Correia, A. C. M.; Boué, G.; Laskar, Jacques; Rodríguez, Adrián

doi:10.1051/0004-6361/201424211

Cited by 109 publications

(205 citation statements)

References 59 publications

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“…In agreement with the early result of Ingersoll & Dobrovolskis (1978) (Eq. (4)), it is of the same form as the result given by the Maxwell model (Correia et al 2014), where we identify the Maxwell time T 0 " σ´1 0 . It also corresponds to the torque computed by Leconte et al (2015) for Venus-like planets with numerical simulations using GCM, which suggests that the slow rotation and convective instability approximations are appropriate for planets of this kind.…”

Section: Comparison With Previous Modelsmentioning

confidence: 96%

“…As a consequence, in both cases the phase shifted elongation of the shell induces a tidal torque which modifies the rotational dynamics of the body. This torque drives the evolution of the spin of planets and determines its possible states of equilibrium (Gold & Soter 1969;Dobrovolskis & Ingersoll 1980;Correia & Laskar 2001;Correia et al , 2014Arras & Socrates 2010).…”

Section: Introductionmentioning

confidence: 99%

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Atmospheric tides in Earth-like planets

Auclair-Desrotour

Laskar

Mathis

2017

A&A

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Context. Atmospheric tides can strongly affect the rotational dynamics of planets. In the family of Earth-like planets, which includes Venus, this physical mechanism coupled with solid tides makes the angular velocity evolve over long timescales and determines the equilibrium configurations of their spin. Aims. Unlike the solid core, the atmosphere of a planet is subject to both tidal gravitational potential and insolation flux coming from the star. The complex response of the gas is intrinsically linked to its physical properties. This dependence has to be characterized and quantified for application to the wide variety of extrasolar planetary systems. Methods. We develop a theoretical global model where radiative losses, which are predominant in slowly rotating atmospheres, are taken into account. We analytically compute the perturbation of pressure, density, temperature, and velocity field caused by a thermogravitational tidal perturbation. From these quantities, we deduce the expressions of atmospheric Love numbers and tidal torque exerted on the fluid shell by the star. The equations are written for the general case of a thick envelope and the simplified one of a thin isothermal atmosphere. Results. The dynamics of atmospheric tides depends on the frequency regime of the tidal perturbation: the thermal regime near synchronization and the dynamical regime characterizing fast-rotating planets. Gravitational and thermal perturbations imply different responses of the fluid, i.e. gravitational tides and thermal tides, which are clearly identified. The dependence of the torque on the tidal frequency is quantified using the analytic expressions of the model for Earth-like and Venus-like exoplanets and is in good agreement with the results given by global climate models (GCM) simulations. Introducing dissipative processes such as radiation regularizes the tidal response of the atmosphere, otherwise it is singular at synchronization. Conclusions. We demonstrate the important role played by the physical and dynamical properties of a super-Earth atmosphere (e.g. Coriolis, stratification, basic pressure, density, temperature, radiative emission) in its response to a tidal perturbation. We point out the key parameters defining tidal regimes (e.g. inertia, Brunt-Väisälä, radiative frequencies, tidal frequency) and characterize the behaviour of the fluid shell in the dissipative regime, which cannot be studied without considering the radiative losses.

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Section: Comparison With Previous Modelsmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

Atmospheric tides in Earth-like planets

Auclair-Desrotour

Laskar

Mathis

2017

A&A

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“…For simplicity, in this paper we consider τ e = 0, since this term does not contribute to the tidal dissipation (for more details, see Correia et al 2014). …”

Section: Numerical Simulations With Tidal Dissipationmentioning

confidence: 99%

Spin dynamics of close-in planets exhibiting large transit timing variations

Delisle

Correia

Leleu

et al. 2017

A&A

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We study the spin evolution of close-in planets in compact multi-planetary systems. The rotation period of these planets is often assumed to be synchronous with the orbital period due to tidal dissipation. Here we show that planet-planet perturbations can drive the spin of these planets into non-synchronous or even chaotic states. In particular, we show that the transit timing variation (TTV) is a very good probe to study the spin dynamics, since both are dominated by the perturbations of the mean longitude of the planet. We apply our model to KOI-227 b and Kepler-88 b, which are both observed undergoing strong TTVs. We also perform numerical simulations of the spin evolution of these two planets. We show that for KOI-227 b non-synchronous rotation is possible, while for Kepler-88 b the rotation can be chaotic.

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“…The final scenario depends on the initial conditions, and also on the tidal model. A constant-Q model would prevent any capture in resonance (Goldreich & Peale 1966), while a visco-elastic model would increase the chances of capture (e.g., Makarov 2012;Correia et al 2014). Strange attractors can also exist in the chaotic zone, which may prevent the spin from stabilizing (e.g., Batygin & Morbidelli 2011).…”

Section: Application To the Pluto-charon Systemmentioning

confidence: 99%

“…Planets orbiting two stars, often called circumbinary planets, have also been reported (e.g., Correia et al 2005;Doyle et al 2011;Welsh et al 2012). Most of these bodies are close enough to the central binary to undergo tidal dissipation, which slowly modifies the rotation rate until it becomes close to the mean motion (e.g., MacDonald 1964; Correia et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Spin-orbit coupling and chaotic rotation for circumbinary bodies

Correia

Leleu

Rambaux

et al. 2015

A&A

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We investigate the resonant rotation of circumbinary bodies in planar quasi-circular orbits. Denoting n b and n the orbital mean motion of the inner binary and of the circumbinary body, respectively, we show that spin-orbit resonances exist at the frequencies n ± kν/2, where ν = n b − n, and k is an integer. Moreover, when the libration at natural frequency has the same magnitude as ν, the resonances overlap and the rotation becomes chaotic. We apply these results to the small satellites in the Pluto-Charon system, and conclude that their rotations are likely chaotic. However, the rotation can also be stable and not synchronous for small axial asymmetries.

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Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology

Cited by 109 publications

References 59 publications

Atmospheric tides in Earth-like planets

Atmospheric tides in Earth-like planets

Spin dynamics of close-in planets exhibiting large transit timing variations

Spin-orbit coupling and chaotic rotation for circumbinary bodies

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