# Mercury's capture into the 3/2 spin-orbit resonance as a result of its chaotic dynamics

@article{Correia2004MercurysCI, title={Mercury's capture into the 3/2 spin-orbit resonance as a result of its chaotic dynamics}, author={Alexandre C. M. Correia and Jacques Laskar}, journal={Nature}, year={2004}, volume={429}, pages={848-850} }

Mercury is locked into a 3/2 spin-orbit resonance where it rotates three times on its axis for every two orbits around the sun. The stability of this equilibrium state is well established, but our understanding of how this state initially arose remains unsatisfactory. Unless one uses an unrealistic tidal model with constant torques (which cannot account for the observed damping of the libration of the planet) the computed probability of capture into 3/2 resonance is very low (about 7 per cent…

## 148 Citations

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## References

SHOWING 1-10 OF 21 REFERENCES

A spin-orbit constraint on the viscosity of a Mercurian liquid core

- Physics
- 1977

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 a…

Rotational Period of the Planet Mercury

- Physics, GeologyNature
- 1965

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 solar…

The chaotic motion of the solar system: A numerical estimate of the size of the chaotic zones

- Physics, Geology
- 1990

Long term evolution and chaotic diffusion of the insolation quantities of Mars

- Physics, Geology
- 2004

Tidal dissipation by solid friction and the resulting orbital evolution

- Geology, Physics
- 1964

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 ×…

The Chaotic Motion of the Solar System

- Geology
- 1993

In a previous paper (Laskar, Nature, 338,237-238), the chaotic nature of the solar system excluding Pluto was e s t a b lished by the numerical computation of the maximum Lyapunov exponent of i t s…

Solar system dynamics

- Physics
- 1999

The Solar System is a complex and fascinating dynamical system. This is the first textbook to describe comprehensively the dynamical features of the Solar System and to provide students with all the…