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Moon

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Moon
☾
orbit plane[2]
  • 24° to Earth's equator [9]
  • North pole right ascension
    • 17h 47m 26s
    • 266.86°[10]
    North pole declination
    65.64°[10]
    Albedo0.136[11]
    Surface temp. min mean max
    Equator 100 K[12] 250 K 390 K[12]
    85°N  150 K 230 K[13]
    Surface absorbed dose rate13.2 μGy/h[14]
    Surface equivalent dose rate57.0 μSv/h[14]
    29.3 to 34.1 arcminutes[4][d]
    Atmosphere[15]
    Surface pressure
    • 10−7 Pa (1 picobar)  (day)
    • 10−10 Pa (1 femtobar)   
      (night)
      [e]
    Composition by volume

    The Moon is

    satellite planet under the geophysical definitions of the term and larger than all known dwarf planets of the Solar System.[17] It lacks any significant atmosphere, hydrosphere, or magnetic field. Its surface gravity is about one-sixth of Earth's at 0.1654 g, with Jupiter's moon Io
    being the only satellite in the Solar System known to have a higher surface gravity and density.

    Orbiting Earth at an

    synodic period of 29.5 days, the amount of visible surface illuminated by the Sun varies from none up to 100%, resulting in lunar phases that form the basis for the months of a lunar calendar. The Moon is tidally locked to Earth, which means that the length of a full rotation of the Moon on its own axis causes its same side (the near side) to always face Earth, and the somewhat longer lunar day is the same as the synodic period. However, 59% of the total lunar surface can be seen from Earth through shifts in perspective due to libration
    .

    The most widely accepted origin explanation posits that the Moon formed 4.51 billion years ago,

    impact basins and mare surfaces were in place by the end of the Imbrian period, some three billion years ago. The lunar surface is relatively non-reflective, with a reflectance just slightly brighter than that of worn asphalt. However, because it has a large angular diameter, the full moon is the brightest celestial object in the night sky. The Moon's apparent size is nearly the same as that of the Sun, allowing it to cover the Sun almost completely during a total solar eclipse
    .

    Both the Moon's prominence in Earth's sky and its regular cycle of phases have provided cultural references and influences for human societies throughout history. Such influences can be found in language, calendar systems, art, and mythology. The first artificial object to reach the Moon was the Soviet Union's Luna 2 uncrewed spacecraft in 1959; this was followed by the first successful soft landing by Luna 9 in 1966. The only human lunar missions to date have been those of the United States' Apollo program, which landed twelve men on the surface between 1969 and 1972. These and later uncrewed missions returned lunar rocks that have been used to develop a detailed geological understanding of the Moon's origins, internal structure, and subsequent history.

    Names and etymology

    The usual

    Proto-Indo-European *mēnsis "month"[21] (from earlier *mēnōt, genitive *mēneses) which may be related to the verb "measure" (of time).[22]

    Occasionally, the name Luna /ˈlnə/ is used in scientific writing[23] and especially in science fiction to distinguish the Earth's moon from others, while in poetry "Luna" has been used to denote personification of the Moon.[24] Cynthia /ˈsɪnθiə/ is another poetic name, though rare, for the Moon personified as a goddess,[25] while Selene /səˈln/ (literally "Moon") is the Greek goddess of the Moon.

    The usual English adjective pertaining to the Moon is "lunar", derived from the Latin word for the Moon, lūna. The adjective selenian

    selenography, the study of the physical features of the Moon, as well as the element name selenium.[30][31]

    The Greek goddess of the wilderness and the hunt,

    Mount Cynthus.[32] These names – Luna, Cynthia and Selene – are reflected in technical terms for lunar orbits
    such as apolune, pericynthion and selenocentric.

    The

    ☾
    , for example in M 'lunar mass' (also ML).

    Natural history

    Lunar geologic timescale

    Early ImbrianLate ImbrianPre-NectarianNectarianEratosthenianCopernican period
    Millions of years before present
    maria (in blue), KREEP (red) and other special features. Oldest to youngest: Aitkenian (pink), Nectarian (brown), Imbrian (greens/turquoise), Eratosthenian (light orange) and Copernican
    (yellow).

    Formation

    atmosphere of Earth to dissipate the energy of the passing Moon.[37] A co-formation of Earth and the Moon together in the primordial accretion disk does not explain the depletion of metals in the Moon.[37] None of these hypotheses can account for the high angular momentum of the Earth–Moon system.[39]

    The prevailing theory is that the Earth–Moon system formed after a

    proto-Earth. The impact blasted material into orbit about the Earth and the material accreted and formed the Moon[40][41] just beyond the Earth's Roche limit of ~2.56 R🜨.[42]

    Giant impacts are thought to have been common in the early Solar System. Computer simulations of giant impacts have produced results that are consistent with the mass of the lunar core and the angular momentum of the Earth–Moon system. These simulations show that most of the Moon derived from the impactor, rather than the proto-Earth.[43] However, more recent simulations suggest a larger fraction of the Moon derived from the proto-Earth.[44][45][46][47] Other bodies of the inner Solar System such as Mars and Vesta have, according to meteorites from them, very different oxygen and tungsten isotopic compositions compared to Earth. However, Earth and the Moon have nearly identical isotopic compositions. The isotopic equalization of the Earth-Moon system might be explained by the post-impact mixing of the vaporized material that formed the two,[48] although this is debated.[49]

    The impact would have released enough energy to liquefy both the ejecta and the Earth's crust, forming a magma ocean. The liquefied ejecta could have then re-accreted into the Earth–Moon system.[50][51] Similarly, the newly formed Moon would have had its own lunar magma ocean; its depth is estimated from about 500 km (300 miles) to 1,737 km (1,079 miles).[50]

    While the giant-impact theory explains many lines of evidence, some questions are still unresolved, most of which involve the Moon's composition.

    example needed]Above a high resolution threshold for simulations, a study published in 2022 finds that giant impacts can immediately place a satellite with similar mass and iron content to the Moon into orbit far outside Earth's Roche limit. Even satellites that initially pass within the Roche limit can reliably and predictably survive, by being partially stripped and then torqued onto wider, stable orbits.[53]

    Natural development

    Artist's impression of the Moon as it might have appeared in Earth's sky after the Late Heavy Bombardment around 4 billion years ago. At that time the Moon orbited Earth much closer,[54]
    appearing much larger.

    After the Moon's formation the Moon settled in orbit around Earth much closer than today, making both bodies appear much larger in each's sky and causing on both more frequent and stronger

    Since then, due to tidal acceleration, the Moon's orbit around Earth has become significantly larger as well as longer, tidally locking the so-called lunar near side, always facing Earth with this same side.

    The post formation cooled

    lunar highlands on the far side, has been an unresolved issue due to differing explanations. One explanation suggests that large meteorites were hitting the Moon in its early history leaving large craters which then were filled with lava. Other explanations suggest processes of lunar volcanism.[57]

    Physical characteristics

    The Moon

    The Moon is a very slightly

    scalene ellipsoid due to tidal stretching, with its long axis displaced 30° from facing the Earth, due to gravitational anomalies from impact basins. Its shape is more elongated than current tidal forces can account for. This 'fossil bulge' indicates that the Moon solidified when it orbited at half its current distance to the Earth, and that it is now too cold for its shape to adjust to its orbit.[58]

    Size and mass

    subsurface oceans
    and one, Titan, having a considerable atmosphere.

    The Moon is by size and mass the fifth largest natural satellite of the Solar System, categorizeable as one of its

    primary planets.[g]

    The Moon's diameter is about 3,500 km, more than a quarter of Earth's, with the face of the Moon comparable to the width of Australia.[16] The whole surface area of the Moon is about 38 million square kilometers, slightly less than the area of the Americas (North and South America).

    The Moon's mass is 1/81 of Earth's,[60] being the second densest among the planetary moons, and having the second highest surface gravity, after Io, at 0.1654 g and an escape velocity of 2.38 km/s (8600 km/h; 5300 mph).

    Structure

    The Moon is a differentiated body that was initially in hydrostatic equilibrium but has since departed from this condition.[61] It has a geochemically distinct crust, mantle, and core. The Moon has a solid iron-rich inner core with a radius possibly as small as 240 kilometres (150 mi) and a fluid outer core primarily made of liquid iron with a radius of roughly 300 kilometres (190 mi). Around the core is a partially molten boundary layer with a radius of about 500 kilometres (310 mi).[62][63] This structure is thought to have developed through the fractional crystallization of a global magma ocean shortly after the Moon's formation 4.5 billion years ago.[64]

    Crystallization of this magma ocean would have created a

    orthopyroxene; after about three-quarters of the magma ocean had crystallised, lower-density plagioclase minerals could form and float into a crust atop.[65] The final liquids to crystallise would have been initially sandwiched between the crust and mantle, with a high abundance of incompatible and heat-producing elements.[1] Consistent with this perspective, geochemical mapping made from orbit suggests a crust of mostly anorthosite.[15] The Moon rock samples of the flood lavas that erupted onto the surface from partial melting in the mantle confirm the mafic mantle composition, which is more iron-rich than that of Earth.[1] The crust is on average about 50 kilometres (31 mi) thick.[1]

    The Moon is the second-densest satellite in the Solar System, after Io.[66] However, the inner core of the Moon is small, with a radius of about 350 kilometres (220 mi) or less,[1] around 20% of the radius of the Moon. Its composition is not well understood, but is probably metallic iron alloyed with a small amount of sulfur and nickel; analyses of the Moon's time-variable rotation suggest that it is at least partly molten.[67] The pressure at the lunar core is estimated to be 5 GPa (49,000 atm).[68]

    Magnetic and gravitational fields

    The Moon has an external magnetic field of less than 0.2 nanoteslas,[69] or less than one hundred thousandth that of Earth. The Moon does not currently have a global dipolar magnetic field and only has crustal magnetization likely acquired early in its history when a dynamo was still operating.[70][71] However, early in its history, 4 billion years ago, its magnetic field strength was likely close to that of Earth today.[69] This early dynamo field apparently expired by about one billion years ago, after the lunar core had completely crystallized.[69] Theoretically, some of the remnant magnetization may originate from transient magnetic fields generated during large impacts through the expansion of plasma clouds. These clouds are generated during large impacts in an ambient magnetic field. This is supported by the location of the largest crustal magnetizations situated near the antipodes of the giant impact basins.[72]

    The Moon's gravitational field is not uniform. The details of the gravitational field have been measured through tracking the Doppler shift of radio signals emitted by orbiting spacecraft. The main lunar gravity features are mascons, large positive gravitational anomalies associated with some of the giant impact basins, partly caused by the dense mare basaltic lava flows that fill those basins.[73][74] The anomalies greatly influence the orbit of spacecraft about the Moon. There are some puzzles: lava flows by themselves cannot explain all of the gravitational signature, and some mascons exist that are not linked to mare volcanism.[75]

    Surface conditions

    On average the Moon's surface gravity is 1.62 m/s2[4] (0.1654 g; 5.318 ft/s2), about half of the surface gravity of Mars and about a sixth of Earth's. The surface of the Moon, having a surface pressure of 10−10 Pa, lacks any significant atmosphere to moderate the extreme conditions of the surface.

    microsieverts per day, which is about 2-3 times more than on the International Space Station at about 400 km above Earth in orbit,[77] 5-10 times more than during a trans-Atlantic flight,[78] 200 times more than on Earth's surface.[77] For further comparison radiation on a flight to Mars is about 1.84 millisieverts per day and on Mars 0.64 millisieverts per day.[79]

    The Moon's

    peaks of eternal light at the Moon's north pole, at the rim of the crater Peary
    .

    The surface is exposed to drastic temperature differences ranging from 140 °C to −171 °C depending on the solar irradiance. Because of the lack of atmosphere, temperatures of different areas vary particularly upon whether they are in sunlight or shadow,[81] making topographical details play a decisive role on local surface temperatures.[82] Parts of many craters, particularly the bottoms of many polar craters,

    craters of eternal darkness" have extremely low temperatures. The Lunar Reconnaissance Orbiter measured the lowest summer temperatures in craters at the southern pole at 35 K (−238 °C; −397 °F)[84] and just 26 K (−247 °C; −413 °F) close to the winter solstice in the north polar crater Hermite. This is the coldest temperature in the Solar System ever measured by a spacecraft, colder even than the surface of Pluto.[82]

    These extreme conditions for example are considered making it unlikely for spacecrafts to harbor bacterial spores at the Moon longer than just one lunar orbit.[85]

    Atmosphere

    The thin lunar atmosphere is visible on the Moon's surface at sunrise and sunset with the Lunar Horizon Glow[86] and lunar twilight rays, like Earth's crepuscular rays. This Apollo 17 sketch depicts the glow and rays[87] among the general zodiacal light[88][89]
    .

    The Moon has an

    sublimation of water ice in the regolith.[95] These gases either return into the regolith because of the Moon's gravity or are lost to space, either through solar radiation pressure or, if they are ionized, by being swept away by the solar wind's magnetic field.[93]

    Studies of Moon magma samples retrieved by the Apollo missions demonstrate that the Moon had once possessed a relatively thick atmosphere for a period of 70 million years between 3 and 4 billion years ago. This atmosphere, sourced from gases ejected from lunar volcanic eruptions, was twice the thickness of that of present-day Mars. The ancient lunar atmosphere was eventually stripped away by solar winds and dissipated into space.[96]

    A permanent

    LADEE's Lunar Dust EXperiment (LDEX) found particle counts peaked during the Geminid, Quadrantid, Northern Taurid, and Omicron Centaurid meteor showers, when the Earth, and Moon pass through comet debris. The lunar dust cloud is asymmetric, being more dense near the boundary between the Moon's dayside and nightside.[97][98]

    Surface features

    The

    topographic feature is the giant far-side South Pole–Aitken basin, some 2,240 km (1,390 mi) in diameter, the largest crater on the Moon and the second-largest confirmed impact crater in the Solar System.[100][101] At 13 km (8.1 mi) deep, its floor is the lowest point on the surface of the Moon.[100][102] The highest elevations of the Moon's surface are located directly to the northeast, which might have been thickened by the oblique formation impact of the South Pole–Aitken basin.[103] Other large impact basins such as Imbrium, Serenitatis, Crisium, Smythii, and Orientale possess regionally low elevations and elevated rims.[100] The far side of the lunar surface is on average about 1.9 km (1.2 mi) higher than that of the near side.[1]

    The discovery of fault scarp cliffs suggest that the Moon has shrunk by about 90 metres (300 ft) within the past billion years.[104] Similar shrinkage features exist on Mercury. Mare Frigoris, a basin near the north pole long assumed to be geologically dead, has cracked and shifted. Since the Moon doesn't have tectonic plates, its tectonic activity is slow and cracks develop as it loses heat.[105]

    Volcanic features

    The largest mare, the main dark region of the near side, is Oceanus Procellarum, with smaller mare, such as Imbrium and Serenitatis
    , that sit within its ring. Left of the centerline is Procellarum proper.

    The main features visible from Earth by the naked eye are dark and relatively featureless lunar plains called

    Latin for "seas", as they were once believed to be filled with water)[106] are vast solidified pools of ancient basaltic lava. Although similar to terrestrial basalts, lunar basalts have more iron and no minerals altered by water.[107] The majority of these lava deposits erupted or flowed into the depressions associated with impact basins. Several geologic provinces containing shield volcanoes and volcanic domes are found within the near side "maria".[108]

    Almost all maria are on the near side of the Moon, and cover 31% of the surface of the near side[60] compared with 2% of the far side.[109] This is likely due to a concentration of heat-producing elements under the crust on the near side, which would have caused the underlying mantle to heat up, partially melt, rise to the surface and erupt.[65][110][111] Most of the Moon's mare basalts erupted during the Imbrian period, 3.3–3.7 billion years ago, though some being as young as 1.2 billion years[55] and as old as 4.2 billion years.[56]

    In 2006, a study of

    Moonquakes and releases of gas indicate continued lunar activity.[112] Evidence of recent lunar volcanism has been identified at 70 irregular mare patches, some less than 50 million years old. This raises the possibility of a much warmer lunar mantle than previously believed, at least on the near side where the deep crust is substantially warmer because of the greater concentration of radioactive elements.[113][114][115][116] Evidence has been found for 2–10 million years old basaltic volcanism within the crater Lowell,[117][118] inside the Orientale basin. Some combination of an initially hotter mantle and local enrichment of heat-producing elements in the mantle could be responsible for prolonged activities on the far side in the Orientale basin.[119][120]

    The lighter-colored regions of the Moon are called terrae, or more commonly highlands, because they are higher than most maria. They have been radiometrically dated to having formed 4.4 billion years ago, and may represent plagioclase cumulates of the lunar magma ocean.[56][55] In contrast to Earth, no major lunar mountains are believed to have formed as a result of tectonic events.[121]

    The concentration of maria on the near side likely reflects the substantially thicker crust of the highlands of the Far Side, which may have formed in a slow-velocity impact of a second moon of Earth a few tens of millions of years after the Moon's formation.[122][123] Alternatively, it may be a consequence of asymmetrical tidal heating when the Moon was much closer to the Earth.[124]

    Impact craters

    A gray, many-ridged surface from high above. The largest feature is a circular ringed structure with high walled sides and a lower central peak: the entire surface out to the horizon is filled with similar structures that are smaller and overlapping.
    Lunar crater Daedalus on the Moon's far side

    A major geologic process that has affected the Moon's surface is

    Apollo missions cluster between 3.8 and 4.1 billion years old: this has been used to propose a Late Heavy Bombardment period of increased impacts.[128]

    High-resolution images from the Lunar Reconnaissance Orbiter in the 2010s show a contemporary crater-production rate significantly higher than was previously estimated. A secondary cratering process caused by distal ejecta is thought to churn the top two centimeters of regolith on a timescale of 81,000 years.[129][130] This rate is 100 times faster than the rate computed from models based solely on direct micrometeorite impacts.[131]

    Lunar swirls

    Lunar Reconnaissance Orbiter Wide Angle Camera image of the lunar swirl Reiner Gamma

    Lunar swirls are enigmatic features found across the Moon's surface. They are characterized by a high albedo, appear optically immature (i.e. the optical characteristics of a relatively young regolith), and often have a sinuous shape. Their shape is often accentuated by low albedo regions that wind between the bright swirls. They are located in places with enhanced surface magnetic fields and many are located at the antipodal point of major impacts. Well known swirls include the Reiner Gamma feature and Mare Ingenii. They are hypothesized to be areas that have been partially shielded from the solar wind, resulting in slower space weathering.[132]

    Surface composition

    Relative elemental composition of the lunar soil

    Blanketed on top of the Moon's crust is a highly comminuted (broken into ever smaller particles) and impact gardened mostly gray surface layer called regolith, formed by impact processes. The finer regolith, the lunar soil of silicon dioxide glass, has a texture resembling snow and a scent resembling spent gunpowder.[133] The regolith of older surfaces is generally thicker than for younger surfaces: it varies in thickness from 10–15 m (33–49 ft) in the highlands and 4–5 m (13–16 ft) in the maria.[134]

    Beneath the finely comminuted regolith layer is the megaregolith, a layer of highly fractured bedrock many kilometers thick.[135]

    Presence of water

    Liquid water cannot persist on the lunar surface. When exposed to solar radiation, water quickly decomposes through a process known as

    comets or possibly produced by the reaction of oxygen-rich lunar rocks, and hydrogen from solar wind, leaving traces of water which could possibly persist in cold, permanently shadowed craters at either pole on the Moon.[136][137] Computer simulations suggest that up to 14,000 km2 (5,400 sq mi) of the surface may be in permanent shadow.[83] The presence of usable quantities of water on the Moon is an important factor in rendering lunar habitation as a cost-effective plan; the alternative of transporting water from Earth would be prohibitively expensive.[138]

    In years since, signatures of water have been found to exist on the lunar surface.

    bistatic radar experiment located on the Clementine spacecraft, indicated the existence of small, frozen pockets of water close to the surface. However, later radar observations by Arecibo, suggest these findings may rather be rocks ejected from young impact craters.[140] In 1998, the neutron spectrometer on the Lunar Prospector spacecraft showed that high concentrations of hydrogen are present in the first meter of depth in the regolith near the polar regions.[141] Volcanic lava beads, brought back to Earth aboard Apollo 15, showed small amounts of water in their interior.[142]

    The 2008

    permanently shadowed polar crater, and detected at least 100 kg (220 lb) of water in a plume of ejected material.[145][146] Another examination of the LCROSS data showed the amount of detected water to be closer to 155 ± 12 kg (342 ± 26 lb).[147]

    In May 2011, 615–1410 ppm water in

    upper mantle
    . Although of considerable selenological interest, this insight does not mean that water is easily available since the sample originated many kilometers below the surface, and the inclusions are so difficult to access that it took 39 years to find them with a state-of-the-art ion microprobe instrument.

    Analysis of the findings of the Moon Mineralogy Mapper (M3) revealed in August 2018 for the first time "definitive evidence" for water-ice on the lunar surface.[149][150] The data revealed the distinct reflective signatures of water-ice, as opposed to dust and other reflective substances.[151] The ice deposits were found on the North and South poles, although it is more abundant in the South, where water is trapped in permanently shadowed craters and crevices, allowing it to persist as ice on the surface since they are shielded from the sun.[149][151]

    In October 2020, astronomers reported detecting molecular water on the sunlit surface of the Moon by several independent spacecraft, including the Stratospheric Observatory for Infrared Astronomy (SOFIA).[152][153][154][155]

    Earth–Moon system

    Orbit

    DSCOVR satellite
    sees the Moon passing in front of Earth

    The Earth and the Moon form the Earth-Moon

    barycentre
    . This barycentre stays located at all times 1,700 km (1,100 mi) (about a quarter of Earth's radius) beneath the Earth's surface, making the Moon seemingly orbit the Earth.

    The orbital eccentricity, giving ovalness of the orbit, is 0.055.[1] The

    semi-major axis
    of the geocentric lunar orbit, is approximately 400,000 km, which is a quarter of a million miles or 1.28 light-seconds, and a unit of measure in astronomy. This is not to be confused with the instantaneous Earth–Moon distance, or distance to the Moon, the momentanous distance from the center of Earth to the center of the Moon.

    The Moon makes a complete orbit around Earth with respect to the fixed stars, its

    solar day on the Moon.[156]

    Due to tidal locking, the Moon has a 1:1 spin–orbit resonance. This rotationorbit ratio makes the Moon's orbital periods around Earth equal to its corresponding rotation periods. This is the reason for only one side of the Moon, its so-called near side, being visible from Earth. That said, while the movement of the Moon is in resonance, it still is not without nuances such as libration, resulting in slightly changing perspectives, making over time and location on Earth about 59% of the Moon's surface visible from Earth.[157]

    Unlike most satellites of other planets, the Moon's orbital plane is closer to the

    Cassini's laws.[159]

    Tidal effects

    The gravitational attraction that Earth and the Moon (as well as the Sun) exert on each other manifests in a slightly greater attraction on the sides of closest to each other, resulting in

    are the most widely experienced result of this, but tidal forces considerably affect also other mechanics of Earth, as well as the Moon and their system.

    The lunar solid crust experiences tides of around 10 cm (4 in) amplitude over 27 days, with three components: a fixed one due to Earth, because they are in

    synchronous rotation, a variable tide due to orbital eccentricity and inclination, and a small varying component from the Sun.[160] The Earth-induced variable component arises from changing distance and libration, a result of the Moon's orbital eccentricity and inclination (if the Moon's orbit were perfectly circular and un-inclined, there would only be solar tides).[160] According to recent research, scientists suggest that the Moon's influence on the Earth may contribute to maintaining Earth's magnetic field.[161]

    The cumulative effects of stress built up by these tidal forces produces

    moonquakes. Moonquakes are much less common and weaker than are earthquakes, although moonquakes can last for up to an hour – significantly longer than terrestrial quakes – because of scattering of the seismic vibrations in the dry fragmented upper crust. The existence of moonquakes was an unexpected discovery from seismometers placed on the Moon by Apollo astronauts from 1969 through 1972.[162]

    The most commonly known effect of tidal forces are elevated sea levels called ocean tides.

    The tides are two bulges in the Earth's oceans, one on the side facing the Moon and the other on the side opposite. As the Earth rotates on its axis, one of the ocean bulges (high tide) is held in place "under" the Moon, while another such tide is opposite. As a result, there are two high tides, and two low tides in about 24 hours.[163] Since the Moon is orbiting the Earth in the same direction of the Earth's rotation, the high tides occur about every 12 hours and 25 minutes; the 25 minutes is due to the Moon's time to orbit the Earth.

    If the Earth were a water world (one with no continents) it would produce a tide of only one meter, and that tide would be very predictable, but the ocean tides are greatly modified by other effects:

    • the frictional coupling of water to Earth's rotation through the ocean floors
    • the inertia of water's movement
    • ocean basins that grow shallower near land
    • the sloshing of water between different ocean basins[164]

    As a result, the timing of the tides at most points on the Earth is a product of observations that are explained, incidentally, by theory.

    Delays in the tidal peaks of both ocean and solid-body tides cause torque in opposition to the Earth's rotation. This "drains" angular momentum and rotational kinetic energy from Earth's rotation, slowing the Earth's rotation.[163][160] That angular momentum, lost from the Earth, is transferred to the Moon in a process known as tidal acceleration, which lifts the Moon into a higher orbit while lowering orbital speed around the Earth.

    Thus the distance between Earth and Moon is increasing, and the Earth's rotation is slowing in reaction.

    lunar ranging experiments) have found that the Moon's distance increases by 38 mm (1.5 in) per year (roughly the rate at which human fingernails grow).[165][166][167]
    Atomic clocks show that Earth's day lengthens by about 17 microseconds every year,[168][169][170] slowly increasing the rate at which UTC is adjusted by leap seconds.

    This tidal drag makes the rotation of Earth and the orbital period of the Moon very slowly match. This matching first results in

    Pluto-Charon system). However, the Sun will become a red giant engulfing the Earth-Moon system long before the latter occurs.[172][173]

    Position and appearance

    Rotation

    The

    tidally locked synchronous rotation of the Moon as it orbits the Earth results in it always keeping nearly the same face turned towards the planet. The side of the Moon that faces Earth is called the near side, and the opposite the far side. The far side is often inaccurately called the "dark side", but it is in fact illuminated as often as the near side: once every 29.5 Earth days. During dark moon to new moon, the near side is dark.[174]

    The Moon originally rotated at a faster rate, but early in its history its rotation slowed and became tidally locked in this orientation as a result of frictional effects associated with tidal deformations caused by Earth.[175] With time, the energy of rotation of the Moon on its axis was dissipated as heat, until there was no rotation of the Moon relative to Earth. In 2016, planetary scientists using data collected on the 1998-99 NASA Lunar Prospector mission, found two hydrogen-rich areas (most likely former water ice) on opposite sides of the Moon. It is speculated that these patches were the poles of the Moon billions of years ago before it was tidally locked to Earth.[176]

    View from Earth

    apparent size
    and viewing angle over a single lunar month as viewed from Earth's north.