Question: How long is the Moon's rotation around its axis?

Tidal locking



Tidal locking (also called gravitational locking or captured rotation) occurs when the long-term interaction between a pair of co-orbiting astronomical bodies drives the rotation rate of at least one of them into the state where there is no more net transfer of angular momentum between this body (e.g. a planet) and its orbit around the second body (e.g. a star); this condition of "no net transfer" must be satisfied over the course of one orbit around the second body.[1][2] This does not mean that the rotation and spin rates are always perfectly synchronized throughout an orbit, as there can be some back and forth transfer over the course of an orbit. This effect arises from the gravitational gradient (tidal force) between the co-orbiting bodies, acting over a sufficiently long period of time.
In the special case where the orbital eccentricity and obliquity are nearly zero, tidal locking results in one hemisphere of the revolving object constantly facing its partner, an effect known as synchronous rotation.[1][2][3] For example, the same side of the Moon always faces the Earth, although there is some libration because the Moon's orbit is not perfectly circular. A tidally locked body in synchronous rotation takes just as long to rotate around its own axis as it does to revolve around its partner.
Usually, only the satellite is tidally locked to the larger body.[4] However, if both the mass difference between the two bodies and the distance between them are relatively small, each may be tidally locked to the other; this is the case for Pluto and Charon.
Mechanism

Consider a pair of co-orbiting objects, A and B. The change in rotation rate necessary to tidally lock body B to the larger body A is caused by the torque applied by A's gravity on bulges it has induced on B by tidal forces.[5]
The gravitational force from object A upon B will vary with distance, being greatest at the nearest surface to A and least at the most distant. This creates a gravitational gradient across object B that will distort its equilibrium shape slightly. The body of object B will become elongated along the axis oriented toward A, and conversely, slightly reduced in dimension in directions orthogonal to this axis. The elongated distortions are known as tidal bulges. (For the solid Earth, these bulges can reach displacements of up to around 0.4 metres (1.3ft).[6]) When B is not yet tidally locked, the bulges travel over its surface due to orbital motions, with one of the two "high" tidal bulges traveling close to the point where body A is overhead. For large astronomical bodies that are nearly spherical due to self-gravitation, the tidal distortion produces a slightly prolate spheroid, i.e. an axially symmetric ellipsoid that is elongated along its major axis. Smaller bodies also experience distortion, but this distortion is less regular.
The material of B exerts resistance to this periodic reshaping caused by the tidal force. In effect, some time is required to reshape B to the gravitational equilibrium shape, by which time the forming bulges have already been carried some distance away from the A–B axis by B's rotation. Seen from a vantage point in space, the points of maximum bulge extension are displaced from the axis oriented toward A. If B's rotation period is shorter than its orbital period, the bulges are carried forward of the axis oriented toward A in the direction of rotation, whereas if B's rotation period is longer, the bulges instead lag behind.
Because the bulges are now displaced from the A–B axis, A's gravitational pull on the mass in them exerts a torque on B. The torque on the A-facing bulge acts to bring B's rotation in line with its orbital period, whereas the "back" bulge, which faces away from A, acts in the opposite sense. However, the bulge on the A-facing side is closer to A than the back bulge by a distance of approximately B's diameter, and so experiences a slightly stronger gravitational force and torque. The net resulting torque from both bulges, then, is always in the direction that acts to synchronize B's rotation with its orbital period, leading eventually to tidal locking.
Orbital changes

The angular momentum of the whole A–B system is conserved in this process, so that when B slows down and loses rotational angular momentum, its orbital angular momentum is boosted by a similar amount (there are also some smaller effects on A's rotation). This results in a raising of B's orbit about A in tandem with its rotational slowdown. For the other case where B starts off rotating too slowly, tidal locking both speeds up its rotation, and lowers its orbit.
Locking of the larger body

The tidal locking effect is also experienced by the larger body A, but at a slower rate because B's gravitational effect is weaker due to B's smaller mass. For example, Earth's rotation is gradually being slowed by the Moon, by an amount that becomes noticeable over geological time as revealed in the fossil record.[7] Current estimations are that this (together with the tidal influence of the Sun) has helped lengthen the Earth day from about 6 hours to the current 24 hours (over ≈ ⁠4½ billion years). Currently, atomic clocks show that Earth's day lengthens by about 15 microseconds every year.[8] Given enough time, this would create a mutual tidal locking between Earth and the Moon, where the length of a day has increased and the length of a lunar month has shortened until the two are the same. However, Earth is not expected to become tidally locked to the Moon before the Sun becomes a red giant and engulfs Earth and the Moon.[9][10]
For bodies of similar size the effect may be of comparable size for both, and both may become tidally locked to each other on a much shorter timescale. An example is the dwarf planet Pluto and its satellite Charon. They have already reached a state where Charon is visible from only one hemisphere of Pluto and vice versa.[11]
Eccentric orbits
For orbits that do not have an eccentricity close to zero, the rotation rate tends to become locked with the orbital speed when the body is at periapsis, which is the point of strongest tidal interaction between the two objects. If the orbiting object has a companion, this third body can cause the rotation rate of the parent object to vary in an oscillatory manner. This interaction can also drive an increase in orbital eccentricity of the orbiting object around the primary – an effect known as eccentricity pumping.[12]
In some cases where the orbit is eccentric and the tidal effect is relatively weak, the smaller body may end up in a so-called spin–orbit resonance, rather than being tidally locked. Here, the ratio of the rotation period of a body to its own orbital period is some simple fraction different from 1:1. A well known case is the rotation of Mercury, which is locked to its own orbit around the Sun in a 3:2 resonance.
Many exoplanets (especially the close-in ones) are expected to be in spin–orbit resonances higher than 1:1. A Mercury-like terrestrial planet can, for example, become captured in a 3:2, 2:1, or 5:2 spin–orbit resonance, with the probability of each being dependent on the orbital eccentricity.[13]
Occurrence
Moons

Most major moons in the Solar System − the gravitationally rounded satellites − are tidally locked with their primaries, because they orbit very closely and tidal force increases rapidly (as a cubic function) with decreasing distance.[14] Notable exceptions are the irregular outer satellites of the gas giants, which orbit much farther away than the large well-known moons.
Pluto and Charon are an extreme example of a tidal lock. Charon is a relatively large moon in comparison to its primary and also has a very close orbit. This results in Pluto and Charon being mutually tidally locked. Pluto's other moons are not tidally locked; Styx, Nix, Kerberos, and Hydra all rotate chaotically due to the influence of Charon.
The tidal locking situation for asteroid moons is largely unknown, but closely orbiting binaries are expected to be tidally locked, as well as contact binaries.
The Moon

The Moon's rotation and orbital periods are tidally locked with each other, so no matter when the Moon is observed from Earth the same hemisphere of the Moon is always seen. The far side of the Moon was not seen until 1959, when photographs of most of the far side were transmitted from the Soviet spacecraft Luna 3.[15]
When the Earth is observed from the moon, the Earth does not appear to translate across the sky but appears to remain in the same place, rotating on its own axis.
Despite the Moon's rotational and orbital periods being exactly locked, about 59% of the Moon's total surface may be seen with repeated observations from Earth due to the phenomena of libration and parallax. Librations are primarily caused by the Moon's varying orbital speed due to the eccentricity of its orbit: this allows up to about 6° more along its perimeter to be seen from Earth. Parallax is a geometric effect: at the surface of Earth we are offset from the line through the centers of Earth and Moon, and because of this we can observe a bit (about 1°) more around the side of the Moon when it is on our local horizon.
Planets
It was thought for some time that Mercury was in synchronous rotation with the Sun. This was because whenever Mercury was best placed for observation, the same side faced inward. Radar observations in 1965 demonstrated instead that Mercury has a 3:2 spin–orbit resonance, rotating three times for every two revolutions around the Sun, which results in the same positioning at those observation points. Modeling has demonstrated that Mercury was captured into the 3:2 spin–orbit state very early in its history, within 20 (and more likely even 10) million years after its formation.[16]
Venus's 583.92-day interval between successive close approaches to Earth is equal to 5.001444 Venusian solar days, making approximately the same face visible from Earth at each close approach. Whether this relationship arose by chance or is the result of some kind of tidal locking with Earth is unknown.[17]
Proxima Centauri b, the "Earth-like planet" discovered in 2016 that orbits around the star Proxima Centauri is tidally locked, either in synchronized rotation,[18] or otherwise expresses a 3:2 spin–orbit resonance like that of Mercury.[19]
One form of hypothetical tidal locked exoplanets are eyeball planets, that in turn are divided into "hot" and "cold" eyeball planets.[20]
Stars
Close binary stars throughout the universe are expected to be tidally locked with each other, and extrasolar planets that have been found to orbit their primaries extremely closely are also thought to be tidally locked to them. An unusual example, confirmed by MOST, may be Tau Boötis, a star that is probably tidally locked by its planet Tau Boötis b.[21] If so, the tidal locking is almost certainly mutual. However, since stars are gaseous bodies that can rotate with a different rate at different latitudes, the tidal lock is with Tau Boötis's magnetic field.
Timescale
An estimate of the time for a body to become tidally locked can be obtained using the following formula:[22]





t

lock


≈



ω

a

6


I
Q


3
G

m

p


2



k

2



R

5







{\displaystyle t_{\text{lock}}\approx {\frac {\omega a^{6}IQ}{3Gm_{p}^{2}k_{2}R^{5}}}}


where




ω



{\displaystyle \omega \,}

 is the initial spin rate expressed in radians per second,




a



{\displaystyle a\,}

 is the semi-major axis of the motion of the satellite around the planet (given by the average of the periapsis and apoapsis distances),




I



{\displaystyle I\,}

 



≈
0.4

m

s



R

2




{\displaystyle \approx 0.4m_{s}R^{2}}

 is the moment of inertia of the satellite, where 




m

s





{\displaystyle m_{s}\,}

 is the mass of the satellite and 



R



{\displaystyle R\,}

 is the mean radius of the satellite,




Q



{\displaystyle Q\,}

 is the dissipation function of the satellite,




G



{\displaystyle G\,}

 is the gravitational constant,





m

p





{\displaystyle m_{p}\,}

 is the mass of the planet, and





k

2





{\displaystyle k_{2}\,}

 is the tidal Love number of the satellite.




Q


{\displaystyle Q}

 and 




k

2




{\displaystyle k_{2}}

 are generally very poorly known except for the Moon, which has 




k

2



/

Q
=
0.0011


{\displaystyle k_{2}/Q=0.0011}

. For a really rough estimate it is common to take 



Q
≈
100


{\displaystyle Q\approx 100}

 (perhaps conservatively, giving overestimated locking times), and





k

2


≈


1.5

1
+



19
μ


2
ρ
g
R






,


{\displaystyle k_{2}\approx {\frac {1.5}{1+{\frac {19\mu }{2\rho gR}}}},}


where




ρ



{\displaystyle \rho \,}

 is the density of the satellite




g
≈
G

m

s



/


R

2




{\displaystyle g\approx Gm_{s}/R^{2}}

 is the surface gravity of the satellite




μ



{\displaystyle \mu \,}

 is the rigidity of the satellite. This can be roughly taken as 3×1010N·m−2 for rocky objects and 4×109N·m−2 for icy ones.
Even knowing the size and density of the satellite leaves many parameters that must be estimated (especially ω, Q, and μ), so that any calculated locking times obtained are expected to be inaccurate, even to factors of ten. Further, during the tidal locking phase the semi-major axis 



a


{\displaystyle a}

 may have been significantly different from that observed nowadays due to subsequent tidal acceleration, and the locking time is extremely sensitive to this value.
Because the uncertainty is so high, the above formulas can be simplified to give a somewhat less cumbersome one. By assuming that the satellite is spherical, 




k

2


≪
1

,
Q
=
100


{\displaystyle k_{2}\ll 1\,,Q=100}

, and it is sensible to guess one revolution every 12 hours in the initial non-locked state (most asteroids have rotational periods between about 2 hours and about 2 days)





t

lock


≈
6





a

6


R
μ



m

s



m

p


2





×

10

10




years

,


{\displaystyle t_{\text{lock}}\approx 6\ {\frac {a^{6}R\mu }{m_{s}m_{p}^{2}}}\times 10^{10}\ {\text{years}},}


with masses in kilograms, distances in meters, and 



μ


{\displaystyle \mu }

 in newtons per meter squared; 



μ


{\displaystyle \mu }

 can be roughly taken as 3×1010N·m−2 for rocky objects and 4×109N·m−2 for icy ones.
There is an extremely strong dependence on semi-major axis 



a


{\displaystyle a}

.
For the locking of a primary body to its satellite as in the case of Pluto, the satellite and primary body parameters can be swapped.
One conclusion is that, other things being equal (such as 



Q


{\displaystyle Q}

 and 



μ


{\displaystyle \mu }

), a large moon will lock faster than a smaller moon at the same orbital distance from the planet because 




m

s





{\displaystyle m_{s}\,}

 grows as the cube of the satellite radius 



R


{\displaystyle R}

. A possible example of this is in the Saturn system, where Hyperion is not tidally locked, whereas the larger Iapetus, which orbits at a greater distance, is. However, this is not clear cut because Hyperion also experiences strong driving from the nearby Titan, which forces its rotation to be chaotic.
The above formulae for the timescale of locking may be off by orders of magnitude, because they ignore the frequency dependence of 




k

2



/

Q


{\displaystyle k_{2}/Q}

. More importantly, they may be inapplicable to viscous binaries (double stars, or double asteroids that are rubble), because the spin–orbit dynamics of such bodies is defined mainly by their viscosity, not rigidity.[23]
List of known tidally locked bodies
Solar System

Extra-solar
Tau Boötis is known to be locked to the close-orbiting giant planet Tau Boötis b.[21]
Bodies likely to be locked
Solar System
Based on comparison between the likely time needed to lock a body to its primary, and the time it has been in its present orbit (comparable with the age of the Solar System for most planetary moons), a number of moons are thought to be locked. However their rotations are not known or not known enough. These are:
Probably locked to Saturn

Daphnis
Aegaeon
Methone
Anthe
Pallene
Helene
Polydeuces

Probably locked to Uranus

Cordelia
Ophelia
Bianca
Cressida
Desdemona
Juliet
Portia
Rosalind
Cupid
Belinda
Perdita
Puck
Mab

Probably locked to Neptune

Naiad
Thalassa
Despina
Galatea
Larissa

Extrasolar
Gliese 581c,[29] Gliese 581g,[30][31] Gliese 581b, and Gliese 581e may be tidally locked to their parent star Gliese 581. Gliese 581d is almost certainly captured either into the 2:1 or the 3:2 spin–orbit resonance with the same star.[32]
All planets in the TRAPPIST-1 system are likely to be tidally locked.[33][34]
See also
Gravity-gradient stabilization – a method used to stabilize some artificial satellites
Orbital resonance
Planetary habitability
Synchronous orbit
Tidal acceleration
Roche limit