Mercury's capture into the 3/2 spin–orbit resonance including the effect of core–mantle friction

@article{Correia2009MercurysCI,
  title={Mercury's capture into the 3/2 spin–orbit resonance including the effect of core–mantle friction},
  author={A. C. M. Correia and Jacques Laskar},
  journal={Icarus},
  year={2009},
  volume={201},
  pages={1-11}
}
The rotation of Mercury is presently captured in a 3/2 spin-orbit resonance with the orbital mean motion. The capture mechanism is well understood as the result of tidal interactions with the Sun combined with planetary perturbations. However, it is now almost certain that Mercury has a liquid core, which should induce a contribution of viscous friction at the core-mantle boundary to the spin evolution. This last effect greatly increases the chances of capture in all spin-orbit resonances… Expand
Long-term evolution of the spin of Mercury: I. Effect of the obliquity and core–mantle friction
Abstract The present obliquity of Mercury is very low (less than 0.1°), which led previous studies to always adopt a nearly zero obliquity during the planet’s past evolution. However, the initialExpand
Mercury’s spin–orbit resonance explained by initial retrograde and subsequent synchronous rotation
The planet Mercury rotates three times about its spin axis for every two orbits around the Sun. Numerical modelling suggests that this unusual pattern could result from initial retrograde rotationExpand
Revisiting the capture of Mercury into its 3:2 spin-orbit resonance
Abstract We simulate the despinning of Mercury, with or without a fluid core, and with a frequency-dependent tidal model employed. The tidal model incorporates the viscoelastic (Maxwell) rebound atExpand
Spin–orbit evolution of Mercury revisited
Abstract Although it is accepted that the significant eccentricity of Mercury (0.206) favours entrapment into the 3:2 spin–orbit resonance, open are the questions of how and when the capture tookExpand
CONDITIONS OF PASSAGE AND ENTRAPMENT OF TERRESTRIAL PLANETS IN SPIN-ORBIT RESONANCES
The dynamical evolution of terrestrial planets resembling Mercury in the vicinity of spin-orbit resonances is investigated using comprehensive harmonic expansions of the tidal torque taking intoExpand
Spin-orbit Coupling for Tidally Evolving Super-Earths
We investigate the spin behaviour of close-in rocky planets and the implications for their orbital evolution. Considering that the planet rotation evolves under simultaneous actions of the torque dueExpand
On Mercury's past rotation, in light of its large craters
Abstract We have simulated in-orbit variations of the impact flux and spatial distributions of >100 km diameter (D) crater production for Mercury in its current 3:2 and hypothetical 2:1 and 1:1Expand
Effect of core–mantle and tidal torques on Mercury’s spin axis orientation
Abstract The rotational evolution of Mercury’s mantle plus crust and its core under conservative and dissipative torques is important for understanding the planet’s spin state. Dissipation resultsExpand
Tidal evolution of the Pluto–Charon binary
A giant collision is believed to be at the origin of the Pluto-Charon system. As a result, the initial orbit and spins after impact may have substantially differed from those observed today. MoreExpand
Spin-Spin Coupling in the Solar System
The richness of dynamical behavior exhibited by the rotational states of various solar system objects has driven significant advances in the theoretical understanding of their evolutionary histories.Expand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 66 REFERENCES
Mercury's capture into the 3/2 spin-orbit resonance as a result of its chaotic dynamics
TLDR
It is shown that the chaotic evolution of Mercury's orbit can drive its eccentricity beyond 0.325 during the planet's history, which very efficiently leads to its capture into the 3/2 resonance. Expand
The core–mantle friction effect on the secular spin evolution of terrestrial planets
For planets having a liquid core, friction with the mantle results in an additional source of dissipating energy alternative to tides. As a consequence, the spin of the planet will slowly change: theExpand
A spin-orbit constraint on the viscosity of a Mercurian liquid core
The escape of Mercury from the stable spin-orbit resonance in which the spin angular velocity is twice the orbital mean motion (2n) requires that the kinematic viscosity of a molten core with aExpand
The Free Precession and Libration of Mercury
Abstract An analysis based on the direct torque equations including tidal dissipation and a viscous core–mantle coupling is used to determine the damping time scales of O ( 10 5 ) years for freeExpand
Rotational Period of the Planet Mercury
IN a recent communication by S. J. Peale and T. Gold1 the rotational period of Mercury, determined from radar Doppler-spread measurements to be 59 ± 5 days2, has been explained in terms of a solarExpand
The evolution of the lunar orbit revisited, II
We present here a model for the tidal evolution of an isolated two-body system. Equations are derived, including the dissipation in the planet as in the satellite, in a frequency dependent lag model.Expand
Tidal dissipation by solid friction and the resulting orbital evolution
Dissipation of tidal energy in the earth's mantle and the moon was calculated assuming a dissipation factor 1/Q constant throughout both bodies. In the mantle the dissipation varies from about 2 ×Expand
The evolution of the lunar orbit revisited. I
After recalling the contribution of Halley, J. Kepler, and G. Darwin to our understanding of the secular acceleration of the Moon, we establish a set of differential equations for the variation ofExpand
Q in the solar system
Abstract Secular changes brought about by tidal friction in the solar system are reviewed. The presence or absence of specific changes is used to bound the values of Q (the specific dissipationExpand
Long-term evolution of the spin of Venus: I. theory
Abstract Due to planetary perturbations, there exists a large chaotic zone for the spin of the terrestrial planets (Laskar and Robutel, 1993 , Nature 361, 608–612). The crossing of this zone in theExpand
...
1
2
3
4
5
...