Spin–orbit evolution of Mercury revisited

@article{Noyelles2014SpinorbitEO,
  title={Spin–orbit evolution of Mercury revisited},
  author={B Noyelles and Julie Frouard and Valeri V. Makarov and Michael Efroimsky},
  journal={Icarus},
  year={2014},
  volume={241},
  pages={26-44}
}
View PDF on arXiv
56 Citations
Highly Influential Citations
2
Background Citations
22
Methods Citations
6
Results Citations
1

56 Citations

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…
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…
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…
Thermal and Orbital Evolution of Low-mass Exoplanets
The thermal, orbital, and rotational dynamics of tidally loaded exoplanets are interconnected by intricate feedback. The rheological structure of the planet determines its susceptibility to tidal…
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…
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…
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…
Final spin states of eccentric ocean planets
Context. 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.…
Could the Migration of Jupiter Have Accelerated the Atmospheric Evolution of Venus?
In the study of planetary habitability and terrestrial atmospheric evolution, the divergence of surface conditions for Venus and Earth remains an area of active research. Among the intrinsic and…
On Mercury's past rotation, in light of its large craters
...
...

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.
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…
Mercury's capture into the 3/2 spin–orbit resonance including the effect of core–mantle friction
DYNAMICAL EVOLUTION AND SPIN-ORBIT RESONANCES OF POTENTIALLY HABITABLE EXOPLANETS. THE CASE OF GJ 667C
We investigate the spin-orbital evolution of the potentially habitable super-Earth GJ 667Cc in the multiple system of at least two exoplanets orbiting a nearby M dwarf. The published radial…
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…
The Free Precession and Libration of Mercury
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…
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…
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.
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 rotation…
...
...