Spin–orbit evolution of Mercury revisited

@article{Noyelles2014SpinorbitEO,
  title={Spin–orbit evolution of Mercury revisited},
  author={B. Noyelles and J. Frouard and V. Makarov and M. Efroimsky},
  journal={Icarus},
  year={2014},
  volume={241},
  pages={26-44}
}
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 took place. A recent work by Makarov (Makarov, V.V. [2012]. Astrophys. J., 752, 73) has proven that trapping into this state is certain for eccentricities larger than 0.2 , provided we use a realistic tidal model based on the Darwin–Kaula expansion of the tidal torque. While in Ibid. a Mercury-like planet… Expand
View PDF on arXiv
53 Citations
Highly Influential Citations
2
Background Citations
22
Methods Citations
7
Results Citations
1

53 Citations

Citation Type

Citation Type

Effective resonant stability of Mercury
Mercury is the unique known planet that is situated in a 3:2 spin-orbit resonance nowadays. Observations and models converge to the same conclusion: the planet is presently deeply trapped in the… Expand
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 at… Expand
Periodic and quasi-periodic attractors for the spin-orbit evolution of Mercury with a realistic tidal torque
In this paper, we make a detailed study of the spin-orbit dynamics of Mercury, as predicted by the realistic model which has been recently introduced in a series of papers mainly by Efroimsky and… Expand
Spin-orbital Tidal Dynamics and Tidal Heating in the TRAPPIST-1 Multiplanet System
We perform numerical simulations of the TRAPPIST-1 system of seven exoplanets orbiting a nearby M dwarf, starting with a previously suggested stable configuration. The long-term stability of this… Expand
Steady state obliquity of a rigid body in the spin–orbit resonant problem: application to Mercury
We investigate the stable Cassini state 1 in the p : q spin–orbit resonant problem. Our study includes the effect of the gravitational potential up to degree and order 4 and p : q spin–orbit… Expand
Averaged model to study long-term dynamics of a probe about Mercury
This paper provides a method for finding initial conditions of frozen orbits for a probe around Mercury. Frozen orbits are those whose orbital elements remain constant on average. Thus, at the same… Expand
TIDAL EVOLUTION OF ASTEROIDAL BINARIES. RULED BY VISCOSITY. IGNORANT OF RIGIDITY
This is a pilot paper serving as a launching pad for study of orbital and spin evolution of binary asteroids. The rate of tidal evolution of asteroidal binaries is defined by the dynamical Love… Expand
Rotation and figure evolution in the creep tide theory: a new approach and application to Mercury
This paper deals with the rotation and figure evolution of a planet near the 3/2 spin-orbit resonance and the exploration of a new formulation of the creep tide theory (Folonier et al. 2018). This… Expand
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 1:1… Expand
Final spin states of eccentric ocean planets
Eccentricity tides generate a torque that can drive an ocean planet towards asynchronous rotation states of equilibrium when enhanced by resonances associated with the oceanic tidal modes. We… Expand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 124 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
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 initial… Expand
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 into… Expand
Mercury's capture into the 3/2 spin–orbit resonance including the effect of core–mantle friction
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… Expand
A pre-Caloris synchronous rotation for Mercury
The planet Mercury is locked in a spin-orbit resonance where it rotates three times about its spin axis for every two orbits about the Sun. The current explanation for this unique state assumes that… Expand
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 free… Expand
Mercury's core - The effect of obliquity on the spin-orbit constraints
In an earlier paper by the authors (Peale and Boss, 1977), rather severe constraints were placed on the properties of a Mercurian liquid core and certain other dynamical characteristics of the planet… Expand
A simple model of the chaotic eccentricity of Mercury
Mercury’s eccentricity is chaotic and can increase so much that collisions with Venus or the Sun become possible. This chaotic behavior results from an intricate network of secular resonances, but in… Expand
DYNAMICAL EVOLUTION AND SPIN-ORBIT RESONANCES OF POTENTIALLY HABITABLE EXOPLANETS. THE CASE OF GJ 667C
GJ 581d is a potentially habitable super-Earth in the multiple system of exoplanets orbiting a nearby M dwarf. We investigate this planet's long-term dynamics with an emphasis on its probable final… Expand
Existence of collisional trajectories of Mercury, Mars and Venus with the Earth
TLDR
Numerical simulations of the evolution of the Solar System over 5 Gyr, including contributions from the Moon and general relativity find that one per cent of the solutions lead to a large increase in Mercury’s eccentricity—an increase large enough to allow collisions with Venus or the Sun. Expand
...
1
2
3
4
5
...