author={Val{\'e}ry Lainey and Ozgur Karatekin and Josselin Desmars and S{\'e}bastien Charnoz and J. -E. Arlot and Nikolay Emelyanov and Christophe Le Poncin-lafitte and S. Mathis and Françoise Remus and Gabriel Tobie and J-P. Zahn},
  journal={The Astrophysical Journal},
Tidal interactions between Saturn and its satellites play a crucial role in both the orbital migration of the satellites and the heating of their interiors. Therefore, constraining the tidal dissipation of Saturn (here the ratio k2/Q) opens the door to the past evolution of the whole system. If Saturn’s tidal ratio can be determined at different frequencies, it may also be possible to constrain the giant planet’s interior structure, which is still uncertain. Here, we try to determine Saturn’s… 
How Cassini can constrain tidal dissipation in Saturn
Tidal dissipation inside giant planets is important for the orbital evolution of their natural satellites. It is conventionally treated by parametrized equilibrium tidal theory, in which the tidal
Frequency-dependent tidal dissipation in a viscoelastic Saturnian core and expansion of Mimas' semi-major axis
Regarding tidal dissipation in Saturn, usually parameterized by Saturn's quality factor Q, there remains a discrepancy between conventional estimates and the latest determination that has been
Strong tidal energy dissipation in Saturn at Titan’s frequency as an explanation for Iapetus orbit
Context. Natural satellite systems present a large variety of orbital configurations in the solar system. While some are clearly the result of known processes, others still have largely unexplained
New constraints on Saturn’s interior from Cassini astrometric data
Orbital evolution of Saturn’s mid-sized moons and the tidal heating of Enceladus
Resonance locking in giant planets indicated by the rapid orbital expansion of Titan
Saturn is orbited by dozens of moons, and the intricate dynamics of this complex system provide clues about its formation and evolution. Tidal friction within Saturn causes its moons to migrate
The equilibrium tide in stars and giant planets: I - the coplanar case
Since 1995, more than 500 extrasolar planets have been discovered orbiting very close to their parent star, where they experience strong tidal interactions. Their orbital evolution depends on the
Orbital evolution and tidal heating of Saturn’s mid-sized moons
The formation and orbital evolution of Saturn’s inner mid-sized moons (Rhea, Dione, Tethys, Enceladus, and Mimas) are still in debate. The most puzzling points are how the moons passed through some
Tidal synchronization of close-in satellites and exoplanets. III. Tidal dissipation revisited and application to Enceladus
This paper deals with a new formulation of the creep tide theory (Ferraz-Mello in Celest Mech Dyn Astron 116:109, 2013—Paper I) and with the tidal dissipation predicted by the theory in the case of
The thermal and orbital evolution of Enceladus : observational constraints and models
Enceladus possesses a global subsurface ocean beneath an ice shell a few tens of km thick, and is observed to be losing heat at a rate of ∼10 GW from its south polar region. Two major puzzles are the


Tidal Dissipation in Rotating Giant Planets
Many extrasolar planets orbit sufficiently close to their host stars that significant tidal interactions can be expected, resulting in an evolution of the spin and orbital properties of the planets.
Dynamical Tides in Rotating Planets and Stars
Tidal dissipation may be important for the internal evolution as well as the orbits of short-period massive planets—hot Jupiters. We revisit a mechanism proposed by Ogilvie and Lin for tidal forcing
Origin of Tidal Dissipation in Jupiter. II. The Value of Q
The process of tidal dissipation inside Jupiter is not yet understood. Its tidal quality factor (Q) is inferred to lie between 105 and 106. Having studied the structure and properties of inertial
Celestial Mechanics and Dynamical Astronomy
1. Dynamics of Extrasolar Planets (C. Beaugé) The orbital fits of multi-planetary systems from radial velocity data has proved to be a complex task. In some cases, different orbital solutions provide
Viscous dissipation by tidally forced inertial modes in a rotating spherical shell
We investigate the properties of forced inertial modes of a rotating fluid inside a spherical shell. Our forcing is tidal like, but its main property is that it is on the large scales. By numerically
Saturn from Cassini-Huygens
This book comprehensively reviews our current knowledge of Saturn featuring the latest results obtained by the Cassini-Huygens mission.
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