• Corpus ID: 119180439

Tidal Evolution of Exoplanets

  title={Tidal Evolution of Exoplanets},
  author={A. C. M. Correia and Jacques Laskar},
  journal={arXiv: Earth and Planetary Astrophysics},
  • A. Correia, J. Laskar
  • Published 7 September 2010
  • Physics, Geology
  • arXiv: Earth and Planetary Astrophysics
Tidal effects arise from differential and inelastic deformation of a planet by a perturbing body. The continuous action of tides modify the rotation of the planet together with its orbit until an equilibrium situation is reached. It is often believed that synchronous motion is the most probable outcome of the tidal evolution process, since synchronous rotation is observed for the majority of the satellites in the Solar System. However, in the 19th century, Schiaparelli also assumed synchronous… 
Tidal evolution of hierarchical and inclined systems
We investigate the dynamical evolution of hierarchical three-body systems under the effect of tides, when the ratio of the orbital semi-major axes is small and the mutual inclination is relatively
Secular and tidal evolution of circumbinary systems
We investigate the secular dynamics of three-body circumbinary systems under the effect of tides. We use the octupolar non-restricted approximation for the orbital interactions, general relativity
An analytical model for tidal evolution in co-orbital systems. I. Application to exoplanets
Close-in co-orbital planets (in a 1:1 mean motion resonance) can experience strong tidal interactions with the central star. Here, we develop an analytical model adapted to the study of the tidal
Diversity of the Extrasolar Worlds
The solar system consists of three different types of planets located in three distinctly separated areas. Their orbits are mostly circular and confined in a plane perpendicular to the sun’s rotation
Photodynamical analysis of the nearly resonant planetary system WASP-148. Accurate transit-timing variations and mutual orbital inclination
WASP-148 is a recently announced extra-solar system harbouring at least two giant planets. The inner planet transits its host star. The planets travel on eccentric orbits and are near the 4:1
Tidal effects in differentiated viscoelastic bodies: a numerical approach
The majority of confirmed terrestrial exoplanets orbits close to their host stars and their evolution was likely altered by tidal interaction. Nevertheless, due to their viscoelastic properties on
Modelling the secular evolution of migrating planet pairs
The subject of this paper is the secular behaviour of a pair of planets evolving under dissipative forces. In particular, we investigate the case when dissipative forces affect the planetary
The structure of terrestrial bodies: Impact heating, corotation limits, and synestias
During accretion, terrestrial bodies attain a wide range of thermal and rotational states, which are accompanied by significant changes in physical structure (size, shape, pressure and temperature
Why do warm Neptunes present nonzero eccentricity?
Most Neptune-mass planets in close-in orbits (orbital periods less than a few days) present nonzero eccentricity, typically around 0.15. This is somehow unexpected, as these planets undergo strong


Secular Evolution of a Satellite by Tidal Effect: Application to Triton
Some of the satellites in the solar system, including the Moon, appear to have been captured from heliocentric orbits at some point in their past, and then have evolved to the present configurations.
Thermal Tides in Short Period Exoplanets
Time-dependent insolation in a planetary atmosphere induces a mass quadrupole upon which the stellar tidal acceleration can exert a force. This "thermal tide" force can give rise to secular torques
On the equilibrium rotation of Earth-like extra-solar planets
The equilibrium rotation of tidally evolved “Earth-like” extra-solar planets is often assumed to be synchronous with their orbital mean motion. The same assumption persisted for Mercury and Venus
Asynchronous rotation and orbital eccentricity lead to time-dependent irradiation of the close-in gas giant exoplanets—the hot Jupiters. This time-dependent surface heating gives rise to fluid
We investigate the effect of planetary rotation on the transit spectrum of an extrasolar giant planet. During ingress and egress, absorption features arising from the planet's atmosphere are Doppler
Planet Migration and Binary Companions: The Case of HD 80606b
The exosolar planet HD 80606b has a highly eccentric (e = 0.93) and tight (a = 0.47 AU) orbit. We study how it might arrive at such an orbit and how it has avoided being tidally circularized until
Shrinking binary and planetary orbits by Kozai cycles with tidal friction
At least two arguments suggest that the orbits of a large fraction of binary stars and extrasolar planets shrank by 1-2 orders of magnitude after formation: (1) the physical radius of a star shrinks
The four final rotation states of Venus
Here it is shown that independent of uncertainties in the models, terrestrial planets with dense atmosphere like Venus can evolve into one of only four possible rotation states, and that most initial conditions will drive the planet towards the configuration at present seen at Venus, albeit through two very different evolutionary paths.
Tidally Heated Terrestrial Exoplanets: Viscoelastic Response Models
Tidal friction in exoplanet systems, driven by orbits that allow for durable nonzero eccentricities at short heliocentric periods, can generate internal heating far in excess of the conditions
Tidal dissipation within hot Jupiters : a new appraisal
Context. Eccentricity or obliquity tides have been proposed as the missing energy source that may explain the anomalously large radius of some transiting “hot Jupiters”. To maintain a non-zero and