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}
}
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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
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
...
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