Tidal locking

Tidal locking (or captured rotation) is when one side of an astronomical body always faces another. It is also called synchronous rotation. The classic example is the Moon: the same side of the Moon always faces the Earth.

Because the Moon is tidally locked, only one side is visible from Earth

A tidally locked body takes just as long to rotate around its own axis as it does to revolve around its partner. This makes one hemisphere constantly face the partner body. Usually, at any given time only the satellite is tidally locked around the larger body. If the two bodies are similar in mass, and their distance apart is small, the tidal force will lock each to the other. This is the case between Pluto and Charon.

If the Moon were not spinning at all, it would alternately show its near and far sides to Earth, while moving around Earth in orbit.

It is possible to work out how long it takes for a particular case of tidal locking to occur. It is just a rough estimate, because some factors are poorly known. An example is the rigidity of a planetary body and its change in shape under tidal force.^[1]^[2] Tidal locking is an aspect of orbital resonance.

List of known tidally locked bodies

Solar System

Locked to the Sun

Mercury

Locked to the Earth

Moon

Locked to Mars

Locked to Jupiter

Locked to Saturn

Ymir

Locked to Uranus

Locked to Neptune

Locked to Pluto

Charon (Pluto is itself locked to Charon)

Other

Dysnomia (Eris is locked to Dysnomia)

Extra-solar

Hot Jupiters are usually tidally locked to their star.

The close-orbiting giant planet Tau Boötis b is known to be locked to the star Tau Boötis A.^[3]

Libration

Simulated views of the Moon over one month, demonstrating librations in latitude and longitude

Libration is an oscillating motion of orbiting bodies relative to each other. Examples include the motion of the Moon relative to Earth, or of Trojan asteroids relative to planets.

The Moon generally has one hemisphere facing the Earth, due to tidal locking. Therefore, our first view of the far side of the Moon resulted from lunar exploration in the 1960s.

However, this simple picture is only approximately true: over time, slightly more than half (about 59%) of the Moon's surface is seen from Earth due to libration.^[4]

Libration is a slow rocking back and forth of the Moon as viewed from Earth, permitting an observer to see slightly different halves of the surface at different times.

References

↑ S.J. Peale, Rotation histories of the natural satellites, in J.A. Burns, ed. 1977. Planetary satellites. Tucson: University of Arizona Press, pp. 87–112.
↑ B. Gladman; et al. (1996). "Synchronous locking of tidally evolving satellites". Icarus. 122 (1): 166–192. Bibcode:1996Icar..122..166G. doi:10.1006/icar.1996.0117. See pages 169/170 of this article.
↑ SPACE.com - Role reversal: Planet controls a star. [1]
↑ Spudis, Paul D. (2004). "Moon". World Book at NASA. Archived from the original on April 17, 2007. Retrieved May 27, 2010.

[1] S.J. Peale, Rotation histories of the natural satellites, in J.A. Burns, ed. 1977. Planetary satellites. Tucson: University of Arizona Press, pp. 87–112.

[2] B. Gladman; et al. (1996). "Synchronous locking of tidally evolving satellites". Icarus. 122 (1): 166–192. Bibcode:1996Icar..122..166G. doi:10.1006/icar.1996.0117. See pages 169/170 of this article.

[3] SPACE.com - Role reversal: Planet controls a star. [1]

[4] Spudis, Paul D. (2004). "Moon". World Book at NASA. Archived from the original on April 17, 2007. Retrieved May 27, 2010.

[1]

[2]

[3]

[4]