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.
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
Locked to the Earth
Locked to Mars
Locked to Jupiter
Locked to Saturn
Locked to Uranus
Locked to Neptune
Locked to Pluto
- Charon (Pluto is itself locked to Charon)
Other
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
.gif)
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.
Tidal Locking Media
A side view of the Pluto–Charon system. Pluto and Charon are tidally locked to each other. Charon is massive enough that the barycenter of Pluto's system lies outside of Pluto; thus, Pluto and Charon are sometimes considered to be a binary system.
If the tidal bulges on a body (green) are misaligned with the major axis (red), the tidal forces (blue) exert a net torque on that body that twists the body toward the direction of realignment.
If rotational frequency is larger than orbital frequency, a small torque counteracting the rotation arises, eventually locking the frequencies (situation depicted in green)
Due to tidal locking, the inhabitants of the central body will never be able to see the satellite's green area.
Libration causes variability in the portion of the Moon visible from Earth. This is an artificial animation of one lunar orbit; in reality, the visible hemisphere would go through phases of dark and light as the Moon rotates with respect to the Sun.
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. Retrieved on 27 May 2010.