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Template:Pp-semi {{#invoke:Hatnote|hatnote}}{{ safesubst:#invoke:Unsubst||$N=Use dmy dates |date=__DATE__ |$B= }} {{#invoke:Infobox|infobox}}

Earth, also called the world Template:Refn and, less frequently, Terra (especially in science fiction)[1] or Gaia,Template:Refn is the third planet from the Sun, the densest planet in the Solar System, the largest of the Solar System's four terrestrial planets, and the only astronomical object known to accommodate life. Earth's biodiversity has evolved over hundreds of millions of years, expanding continually except when interrupted by mass extinctions.[2] Although scholars estimate that over 99 percent of all species that ever lived on the planet are extinct,[3][4] Earth is currently home to 10–14 million species of life,[5][6] including over 7.2 billion humans,[7] who depend upon its biosphere and minerals. Earth's human population is divided among about two hundred sovereign states which interact through diplomacy, conflict, travel, trade, and communication media.

According to evidence from radiometric dating and other sources, Earth was formed around four and a half billion years ago. Within its first billion years,[8] life appeared in its oceans and began to affect its atmosphere and surface, promoting the proliferation of aerobic as well as anaerobic organisms and causing the formation of the atmosphere's ozone layer. This layer and the geomagnetic field block the most life-threatening parts of the Sun's radiation, so life was able to flourish on land as well as in water.[9] Since then, the combination of Earth's distance from the Sun, its physical properties, and its geological history have allowed life to persist.

Earth's lithosphere is divided into several rigid tectonic plates that migrate across the surface over periods of many millions of years. Seventy-one percent of Earth's surface is covered with water,[10] with the remainder consisting of continents and islands that together have many lakes and other sources of water that contribute to the hydrosphere. Earth's poles are mostly covered with ice that includes the solid ice of the Antarctic ice sheet and the sea ice of the polar ice packs. Earth's interior remains active, with a solid iron inner core, a liquid outer core that generates the magnetic field, and a thick layer of relatively solid mantle.

Earth gravitationally interacts with other objects in space, especially the Sun and the Moon. During one orbit around the Sun, Earth rotates about its own axis 366.26 times, creating 365.26 solar days, or one sidereal year.[n 1] Earth's axis of rotation is tilted 23.4° away from the perpendicular of its orbital plane, producing seasonal variations on the planet's surface with a period of one tropical year (365.24 solar days).[11] The Moon is Earth's only natural satellite. It began orbiting Earth about 4.53 billion years ago (bya). The Moon's gravitational interaction with Earth stimulates ocean tides, stabilizes the axial tilt, and gradually slows the planet's rotation.

Name and etymology

The modern English {{safesubst:#invoke:anchor|main}} Earth developed from a wide variety of Middle English forms,Template:Refn which derived from an Old English noun most often spelled Template:Linktext.[12] It has cognates in every Germanic language, and their proto-Germanic root has been reconstructed as *erþō. In its earliest appearances, eorðe was already being used to translate the many senses of Latin Template:Linktext and Greek Template:Linktext (): the ground,Template:Refn its soil,Template:Refn dry land,Template:Refn the human world,Template:Refn the surface of the world (including the sea),Template:Refn and the globe itself.Template:Refn As with Terra and Gaia, Earth was a personified goddess in Germanic paganism: the Angles were listed by Tacitus as among the devotees of Nerthus,[13] and later Norse mythology included Jörð, a giantess often given as the mother of Thor.[14]

Originally, earth was written in lowercase and, from early Middle English, its definite sense as "the globe" was expressed as the earth. By early Modern English, many nouns were capitalized and the earth became (and often remained) the Earth, particularly when referenced along with other heavenly bodies. More recently, the name is sometimes simply given as Earth, by analogy with the names of the other planets.[12] House styles now vary: Oxford spelling recognizes the lowercase form as the most common, with the capitalized form an acceptable variant. Another convention capitalizes Earth when appearing as a name (e.g. "Earth's atmosphere") but writes it in lowercase when preceded by the (e.g. "the atmosphere of the earth"). It almost always appears in lowercase in colloquial expressions such as "what on earth are you doing?"[15]

Composition and structure


{{#invoke:main|main}} {{#invoke:Multiple image|render}} The shape of Earth approximates an oblate spheroid, a sphere flattened along the axis from pole to pole such that there is a bulge around the equator.[16] This bulge results from the rotation of Earth, and causes the diameter at the equator to be Template:Convert larger than the pole-to-pole diameter.[17] Thus the point on the surface farthest from Earth's center of mass is the Chimborazo volcano in Ecuador.[18] The average diameter of the reference spheroid is about Template:Convert, which is approximately 40,000 km/π, because the meter was originally defined as 1/10,000,000 of the distance from the equator to the North Pole through Paris, France.[19]

Local topography deviates from this idealized spheroid, although on a global scale these deviations are small compared to Earth's radius: The maximum deviation of only 0.17% is at the Mariana Trench (Template:Val below local sea level), whereas Mount Everest (8,848 m above local sea level) represents a deviation of 0.14%. If Earth were shrunk to the size of a cue ball, some areas of Earth such as mountain ranges and oceanic trenches would feel like small imperfections, whereas much of the planet, including the Great Plains and the Abyssal plains, would actually feel smoother than a cue ball.[20] Due to the equatorial bulge, the surface locations farthest from Earth's center are the summits of Mount Chimborazo in Ecuador and Huascarán in Peru.[21][22][23][24]

Chemical composition of the crust[25]
Compound Formula Composition
Continental Oceanic
silica SiO2 60.2% 48.6%
alumina Al2O3 15.2% 16.5%
lime CaO 5.5% 12.3%
magnesia MgO 3.1% 6.8%
iron(II) oxide FeO 3.8% 6.2%
sodium oxide Na2O 3.0% 2.6%
potassium oxide K2O 2.8% 0.4%
iron(III) oxide Fe2O3 2.5% 2.3%
water H2O 1.4% 1.1%
carbon dioxide CO2 1.2% 1.4%
titanium dioxide TiO2 0.7% 1.4%
phosphorus pentoxide P2O5 0.2% 0.3%
Total 99.6% 99.9%
Chimborazo, Ecuador. The point on Earth's surface farthest from its center.[21]

Chemical composition

{{#invoke:see also|seealso}} Earth's mass is approximately Template:Val. It is composed mostly of iron (32.1%), oxygen (30.1%), silicon (15.1%), magnesium (13.9%), sulfur (2.9%), nickel (1.8%), calcium (1.5%), and aluminium (1.4%), with the remaining 1.2% consisting of trace amounts of other elements. Due to mass segregation, the core region is believed to be primarily composed of iron (88.8%), with smaller amounts of nickel (5.8%), sulfur (4.5%), and less than 1% trace elements.[26]

The geochemist F. W. Clarke calculated that a little more than 47% of Earth's crust consists of oxygen. The more common rock constituents of the crust are nearly all oxides; chlorine, sulfur and fluorine are the important exceptions to this and their total amount in any rock is usually much less than 1%. The principal oxides are silica, alumina, iron oxides, lime, magnesia, potash and soda. The silica functions principally as an acid, forming silicates, and all the commonest minerals of igneous rocks are of this nature. From a computation based on 1,672 analyses of all kinds of rocks, Clarke deduced that 99.22% were composed of 11 oxides (see the table at right), with the other constituents occurring in minute quantities.[27]

Internal structure

{{#invoke:main|main}} Earth's interior, like that of the other terrestrial planets, is divided into layers by their chemical or physical (rheological) properties, but unlike the other terrestrial planets, it has a distinct outer and inner core. The outer layer is a chemically distinct silicate solid crust, which is underlain by a highly viscous solid mantle. The crust is separated from the mantle by the Mohorovičić discontinuity, and the thickness of the crust varies: averaging Template:Val (kilometers) under the oceans and 30-Template:Val on the continents. The crust and the cold, rigid, top of the upper mantle are collectively known as the lithosphere, and it is of the lithosphere that the tectonic plates are composed. Beneath the lithosphere is the asthenosphere, a relatively low-viscosity layer on which the lithosphere rides. Important changes in crystal structure within the mantle occur at 410 and Template:Val below the surface, spanning a transition zone that separates the upper and lower mantle. Beneath the mantle, an extremely low viscosity liquid outer core lies above a solid inner core.[28] The inner core may rotate at a slightly higher angular velocity than the remainder of the planet, advancing by 0.1–0.5° per year.[29] The radius of the inner core is about one fifth of Earth's.

Geologic layers of Earth[30]

Earth cutaway from core to exosphere. Not to scale.
Component Layer Density
0–60 Lithosphere[n 2]
0–35 Crust[n 3] 2.2–2.9
35–60 Upper mantle 3.4–4.4
  35–2890 Mantle 3.4–5.6
100–700 Asthenosphere
2890–5100 Outer core 9.9–12.2
5100–6378 Inner core 12.8–13.1


Earth's internal heat comes from a combination of residual heat from planetary accretion (about 20%) and heat produced through radioactive decay (80%).[32] The major heat-producing isotopes within Earth are potassium-40, uranium-238, uranium-235, and thorium-232.[33] At the center, the temperature may be up to Template:Convert,[34] and the pressure could reach 360 GPa.[35] Because much of the heat is provided by radioactive decay, scientists postulate that early in Earth's history, before isotopes with short half-lives had been depleted, Earth's heat production would have been much higher. This extra heat production, twice present-day at approximately Template:Val,[32] would have increased temperature gradients with radius, increasing the rates of mantle convection and plate tectonics, and allowing the production of uncommon igneous rocks such as komatiites that are rarely formed today.[36]

Present-day major heat-producing isotopes[37]
Isotope Heat release
{{ safesubst:#invoke:Unsubst
$B=W/kg isotope}} Half-life
Mean mantle concentration
{{ safesubst:#invoke:Unsubst
$B=kg isotope/kg mantle}} Heat release
{{ safesubst:#invoke:Unsubst
$B=W/kg mantle}}
238U 94.6 × 10−6 4.47 × 109 30.8 × 10−9 2.91 × 10−12
235U 569 × 10−6 0.704 × 109 0.22 × 10−9 0.125 × 10−12
232Th 26.4 × 10−6 14.0 × 109 124 × 10−9 3.27 × 10−12
40K 29.2 × 10−6 1.25 × 109 36.9 × 10−9 1.08 × 10−12

The mean heat loss from Earth is 87 mW m−2, for a global heat loss of 4.42 × 1013 W.[38] A portion of the core's thermal energy is transported toward the crust by mantle plumes; a form of convection consisting of upwellings of higher-temperature rock. These plumes can produce hotspots and flood basalts.[39] More of the heat in Earth is lost through plate tectonics, by mantle upwelling associated with mid-ocean ridges. The final major mode of heat loss is through conduction through the lithosphere, the majority of which occurs under the oceans because the crust there is much thinner than that of the continents.[40]

Tectonic plates

Earth's major plates[41]
Shows the extent and boundaries of tectonic plates, with superimposed outlines of the continents they support
Plate name Area
106 km2
Template:Legend 103.3
Template:Legend 78.0
Template:Legend 75.9
Template:Legend 67.8
Template:Legend 60.9
Template:Legend 47.2
Template:Legend 43.6

{{#invoke:main|main}} The mechanically rigid outer layer of Earth, the lithosphere, is broken into pieces called tectonic plates. These plates are rigid segments that move in relation to one another at one of three types of plate boundaries: convergent boundaries, at which two plates come together, divergent boundaries, at which two plates are pulled apart, and transform boundaries, in which two plates slide past one another laterally. Earthquakes, volcanic activity, mountain-building, and oceanic trench formation can occur along these plate boundaries.[42] The tectonic plates ride on top of the asthenosphere, the solid but less-viscous part of the upper mantle that can flow and move along with the plates,[43] and their motion is strongly coupled with convection patterns inside mantle.

As the tectonic plates migrate across the planet, the ocean floor is subducted under the leading edges of the plates at convergent boundaries. At the same time, the upwelling of mantle material at divergent boundaries creates mid-ocean ridges. The combination of these processes continually recycles the oceanic crust back into the mantle. Due to this recycling, most of the ocean floor is less than Template:Val old in age. The oldest oceanic crust is located in the Western Pacific, and has an estimated age of about Template:Val.[44][45] By comparison, the oldest dated continental crust is Template:Val.[46]

The seven major plates are the Pacific, North American, Eurasian, African, Antarctic, Indo-Australian, and South American. Other notable plates include the Arabian Plate, the Caribbean Plate, the Nazca Plate off the west coast of South America and the Scotia Plate in the southern Atlantic Ocean. The Australian Plate fused with the Indian Plate between 50 and Template:Val. The fastest-moving plates are the oceanic plates, with the Cocos Plate advancing at a rate of 75 mm/year[47] and the Pacific Plate moving 52–69 mm/year. At the other extreme, the slowest-moving plate is the Eurasian Plate, progressing at a typical rate of about 21 mm/year.[48]


{{#invoke:main|main}} Template:Pie chart Earth's terrain varies greatly from place to place. About 70.8%[49] of the surface is covered by water, with much of the continental shelf below sea level. This equates to Template:Val (139.43 million sq mi).[50] The submerged surface has mountainous features, including a globe-spanning mid-ocean ridge system, as well as undersea volcanoes,[17] oceanic trenches, submarine canyons, oceanic plateaus and abyssal plains. The remaining 29.2% (Template:Val, or 57.51 million sq mi) not covered by water consists of mountains, deserts, plains, plateaus, and other landforms.

The planetary surface undergoes reshaping over geological time periods due to tectonics and erosion. The surface features built up or deformed through plate tectonics are subject to steady weathering and erosion from precipitation, thermal cycles, and chemical effects. Glaciation, coastal erosion, the build-up of coral reefs, and large meteorite impacts[51] also act to reshape the landscape.

The continental crust consists of lower density material such as the igneous rocks granite and andesite. Less common is basalt, a denser volcanic rock that is the primary constituent of the ocean floors.[52] Sedimentary rock is formed from the accumulation of sediment that becomes buried and compacted together. Nearly 75% of the continental surfaces are covered by sedimentary rocks, although they form about 5% of the crust.[53] The third form of rock material found on Earth is metamorphic rock, which is created from the transformation of pre-existing rock types through high pressures, high temperatures, or both. The most abundant silicate minerals on Earth's surface include quartz, feldspars, amphibole, mica, pyroxene and olivine.[54] Common carbonate minerals include calcite (found in limestone) and dolomite.[55]

The pedosphere is the outermost layer of Earth's continental surface and is composed of soil and subject to soil formation processes. It exists at the interface of the lithosphere, atmosphere, hydrosphere and biosphere. The total arable land is 13.31% of the land surface, with 4.71% supporting permanent crops.[56] Close to 40% of Earth's land surface is used for cropland and pasture, or an estimated 1.3Template:E km2 of cropland and 3.4Template:E km2 of pastureland.[57]

The elevation of the land surface varies from the low point of −418 m at the Dead Sea, to a 2005-estimated maximum altitude of 8,848 m at the top of Mount Everest. The mean height of land above sea level is 840 m.[58]

Besides being divided logically into Northern and Southern hemispheres centered on the poles, Earth has been divided arbitrarily into Eastern and Western hemispheres. The surface of Earth is traditionally divided into seven continents and various seas. As people settled and organized the planet, nearly all the land was divided into nations.



Elevation histogram of Earth's surface

The abundance of water on Earth's surface is a unique feature that distinguishes the "Blue Planet" from other planets in the Solar System. Earth's hydrosphere consists chiefly of the oceans, but technically includes all water surfaces in the world, including inland seas, lakes, rivers, and underground waters down to a depth of 2,000 m. The deepest underwater location is Challenger Deep of the Mariana Trench in the Pacific Ocean with a depth of 10,911.4 m.[n 4][59]

The mass of the oceans is approximately 1.35Template:E metric tons, or about 1/4400 of Earth's total mass. The oceans cover an area of Template:Val with a mean depth of Template:Val, resulting in an estimated volume of Template:Val.[60] If all of Earth's crustal surface was at the same elevation as a smooth sphere, the depth of the resulting world ocean would be 2.7 to 2.8 km.[61][62]

About 97.5% of the water is saline; the remaining 2.5% is fresh water. Most fresh water, about 68.7%, is present as ice in ice caps and glaciers.[63]

The average salinity of Earth's oceans is about 35 grams of salt per kilogram of sea water (3.5% salt).[64] Most of this salt was released from volcanic activity or extracted from cool igneous rocks.[65] The oceans are also a reservoir of dissolved atmospheric gases, which are essential for the survival of many aquatic life forms.[66] Sea water has an important influence on the world's climate, with the oceans acting as a large heat reservoir.[67] Shifts in the oceanic temperature distribution can cause significant weather shifts, such as the El Niño-Southern Oscillation.[68]



A Typhoon as seen from low Earth orbit

The atmospheric pressure on Earth's surface averages 101.325 kPa, with a scale height of about 8.5 km.[69] It has a composition of 78% nitrogen and 21% oxygen, with trace amounts of water vapor, carbon dioxide and other gaseous molecules. The height of the troposphere varies with latitude, ranging between 8 km at the poles to 17 km at the equator, with some variation resulting from weather and seasonal factors.[70]

Earth's biosphere has significantly altered its atmosphere. Oxygenic photosynthesis evolved Template:Val, forming the primarily nitrogen–oxygen atmosphere of today.[71] This change enabled the proliferation of aerobic organisms as well as the formation of the ozone layer, which blocks ultraviolet solar radiation, permitting life on land. Other atmospheric functions important to life include transporting water vapor, providing useful gases, causing small meteors to burn up before they strike the surface, and moderating temperature.[72] This last phenomenon is known as the greenhouse effect: trace molecules within the atmosphere serve to capture thermal energy emitted from the ground, thereby raising the average temperature. Water vapor, carbon dioxide, methane and ozone are the primary greenhouse gases in the atmosphere. Without this heat-retention effect, the average surface would be −18 °C, in contrast to the current +15 °C, and life would likely not exist.[73]

Weather and climate


Earth's atmosphere has no definite boundary, slowly becoming thinner and fading into outer space. Three-quarters of the atmosphere's mass is contained within the first 11 km of the surface. This lowest layer is called the troposphere. Energy from the Sun heats this layer, and the surface below, causing expansion of the air. This lower-density air then rises, and is replaced by cooler, higher-density air. The result is atmospheric circulation that drives the weather and climate through redistribution of thermal energy.[74]

The primary atmospheric circulation bands consist of the trade winds in the equatorial region below 30° latitude and the westerlies in the mid-latitudes between 30° and 60°.[75] Ocean currents are also important factors in determining climate, particularly the thermohaline circulation that distributes thermal energy from the equatorial oceans to the polar regions.[76]

Water vapor generated through surface evaporation is transported by circulatory patterns in the atmosphere. When atmospheric conditions permit an uplift of warm, humid air, this water condenses and falls to the surface as precipitation.[74] Most of the water is then transported to lower elevations by river systems and usually returned to the oceans or deposited into lakes. This water cycle is a vital mechanism for supporting life on land, and is a primary factor in the erosion of surface features over geological periods. Precipitation patterns vary widely, ranging from several meters of water per year to less than a millimeter. Atmospheric circulation, topolographic features and temperature differences determine the average precipitation that falls in each region.[77]

The amount of solar energy reaching Earth's surface decreases with increasing latitude. At higher latitudes the sunlight reaches the surface at lower angles and it must pass through thicker columns of the atmosphere. As a result, the mean annual air temperature at sea level decreases by about 0.4 °C per degree of latitude away from the equator.[78] Earth's surface can be subdivided into specific latitudinal belts of approximately homogeneous climate. Ranging from the equator to the polar regions, these are the tropical (or equatorial), subtropical, temperate and polar climates.[79] Climate can also be classified based on the temperature and precipitation, with the climate regions characterized by fairly uniform air masses. The commonly used Köppen climate classification system (as modified by Wladimir Köppen's student Rudolph Geiger) has five broad groups (humid tropics, arid, humid middle latitudes, continental and cold polar), which are further divided into more specific subtypes.[75]

Upper atmosphere

This view from orbit shows the full Moon partially obscured by Earth's atmosphere. NASA image

Above the troposphere, the atmosphere is usually divided into the stratosphere, mesosphere, and thermosphere.[72] Each layer has a different lapse rate, defining the rate of change in temperature with height. Beyond these, the exosphere thins out into the magnetosphere, where the geomagnetic fields interact with the solar wind.[80] Within the stratosphere is the ozone layer, a component that partially shields the surface from ultraviolet light and thus is important for life on Earth. The Kármán line, defined as 100 km above Earth's surface, is a working definition for the boundary between the atmosphere and outer space.[81]

Thermal energy causes some of the molecules at the outer edge of the atmosphere to increase their velocity to the point where they can escape from Earth's gravity. This causes a slow but steady leakage of the atmosphere into space. Because unfixed hydrogen has a low molecular mass, it can achieve escape velocity more readily and it leaks into outer space at a greater rate than other gases.[82] The leakage of hydrogen into space contributes to the shifting of Earth's atmosphere and surface from an initially reducing state to its current oxidizing one. Photosynthesis provided a source of free oxygen, but the loss of reducing agents such as hydrogen is believed to have been a necessary precondition for the widespread accumulation of oxygen in the atmosphere.[83] Hence the ability of hydrogen to escape from the atmosphere may have influenced the nature of life that developed on Earth.[84] In the current, oxygen-rich atmosphere most hydrogen is converted into water before it has an opportunity to escape. Instead, most of the hydrogen loss comes from the destruction of methane in the upper atmosphere.[85]

Magnetic field

Diagram showing the magnetic field lines of Earth's magnetosphere. The lines are swept back in the anti-solar direction under the influence of the solar wind.
Schematic of Earth's magnetosphere. The solar wind flows from left to right

{{#invoke:main|main}} The main part of the Earth's magnetic field is generated in the core, the site of a dynamo process that converts kinetic energy of fluid convective motion into electrical and magnetic field energy. The field extends outwards from the core, through the mantle, and up to Earth's surface, where it is, to rough approximation, a dipole. The poles of the dipole are located close to Earth's geographic poles. At the equator of the magnetic field, the magnetic field strength at the surface is 3.05 × 10−5 T, with global magnetic dipole moment of 7.91 × 1015 T m3.[86] The convection movements in the core are chaotic; the magnetic poles drift and periodically change alignment. This causes field reversals at irregular intervals averaging a few times every million years. The most recent reversal occurred approximately 700,000 years ago.[87][88]


The extent of Earth's magnetic field in space defines the magnetosphere. Ions and electrons of the solar wind are deflected by the magnetosphere; solar wind pressure compresses the dayside of the magnetosphere, to about 10 earth radii, and extends the nightside magnetosphere into a long tail. Since the velocity of the solar wind is greater than the speed at which wave propagate through the solar wind, a supersonic bowshock precedes the dayside magnetosphere within the solar wind. Charged particles are contained within the magnetosphere; the plasmasphere is defined by low-energy particles that essentially follow magnetic field lines as Earth rotates; the ring current is defined by medium-energy particles that drift relative to the geomagnetic field, but with paths that are still dominated by the magnetic field, and the Van Allen radiation belt are formed by high-energy particles whose motion is essentially random, but otherwise contained by the magnetosphere.

During a magnetic storm, charged particles can be deflected from the outer magnetosphere, directed along field lines into Earth's ionosphere, where atmospheric atoms can be excited and ionized, causing the aurora.[89]

Orbit and rotation



Earth's axial tilt (or obliquity) and its relation to the rotation axis and plane of orbit

Earth's rotation period relative to the Sun—its mean solar day—is 86,400 seconds of mean solar time (86,400.0025 SI seconds).[90] Because Earth's solar day is now slightly longer than it was during the 19th century due to tidal acceleration, each day varies between 0 and 2 SI ms longer.[91][92]

Earth's rotation period relative to the fixed stars, called its stellar day by the International Earth Rotation and Reference Systems Service (IERS), is 86,164.098903691 seconds of mean solar time (UT1), or 23Template:Smallsup 56Template:Smallsup 4.098903691Template:Smallsup.[93][n 5] Earth's rotation period relative to the precessing or moving mean vernal equinox, misnamed its sidereal day, is 86,164.09053083288 seconds of mean solar time (UT1) (23Template:Smallsup 56Template:Smallsup 4.09053083288Template:Smallsup) Template:As of.[93] Thus the sidereal day is shorter than the stellar day by about 8.4 ms.[94] The length of the mean solar day in SI seconds is available from the IERS for the periods 1623–2005[95] and 1962–2005.[96]

Apart from meteors within the atmosphere and low-orbiting satellites, the main apparent motion of celestial bodies in Earth's sky is to the west at a rate of 15°/h = 15'/min. For bodies near the celestial equator, this is equivalent to an apparent diameter of the Sun or the Moon every two minutes; from Earth's surface, the apparent sizes of the Sun and the Moon are approximately the same.[97][98]


{{#invoke:main|main}} Earth orbits the Sun at an average distance of about 150 million kilometers every 365.2564 mean solar days, or one sidereal year. This gives an apparent movement of the Sun eastward with respect to the stars at a rate of about 1°/day, which is one apparent Sun or Moon diameter every 12 hours. Due to this motion, on average it takes 24 hours—a solar day—for Earth to complete a full rotation about its axis so that the Sun returns to the meridian. The orbital speed of Earth averages about 29.8 km/s (107,000 km/h), which is fast enough to travel a distance equal to Earth's diameter, about 12,742 km, in seven minutes, and the distance to the Moon, 384,000 km, in about 3.5 hours.[99]

The Moon and Earth orbit a common barycenter every 27.32 days relative to the background stars. When combined with Earth–Moon system's common orbit around the Sun, the period of the synodic month, from new moon to new moon, is 29.53 days. Viewed from the celestial north pole, the motion of Earth, the Moon, and their axial rotations are all counterclockwise. Viewed from a vantage point above the north poles of both the Sun and Earth, Earth orbits in a counterclockwise direction about the Sun. The orbital and axial planes are not precisely aligned: Earth's axis is tilted some 23.4 degrees from the perpendicular to the Earth–Sun plane (the ecliptic), and the Earth–Moon plane is tilted up to ±5.1 degrees against the Earth–Sun plane. Without this tilt, there would be an eclipse every two weeks, alternating between lunar eclipses and solar eclipses.[69][100]

The Hill sphere, or gravitational sphere of influence, of Earth is about 1.5 Gm or 1,500,000 km in radius.[101][n 6] This is the maximum distance at which the Earth's gravitational influence is stronger than the more distant Sun and planets. Objects must orbit Earth within this radius, or they can become unbound by the gravitational perturbation of the Sun.

Earth, along with the Solar System, is situated in the Milky Way galaxy and orbits about 28,000 light years from the center of the galaxy. It is about 20 light years above the galactic plane in the Orion spiral arm.[102]

Axial tilt and seasons

{{#invoke:main|main}} Due to Earth's axial tilt, the amount of sunlight reaching any given point on the surface varies over the course of the year. This causes seasonal change in climate, with summer in the northern hemisphere occurring when the North Pole is pointing toward the Sun, and winter taking place when the pole is pointed away. During the summer, the day lasts longer and the Sun climbs higher in the sky. In winter, the climate becomes generally cooler and the days shorter. In North temperate latitudes, the sun rises north of true East during the Summer Solstice, and sets north of true west, reversing in the winter. The sun rises south of true east in the summer for the Southern Temperate Zone, and sets south of true west.

Above the Arctic Circle, an extreme case is reached where there is no daylight at all for part of the year, up to six months at the North Pole itself, a polar night. In the southern hemisphere the situation is exactly reversed, with the South Pole oriented opposite the direction of the North Pole. Six months later, this pole will experience a midnight sun, a day of 24 hours, again reversing with the South Pole.

By astronomical convention, the four seasons are determined by the solstices—the point in the orbit of maximum axial tilt toward or away from the Sun—and the equinoxes, when the direction of the tilt and the direction to the Sun are perpendicular. In the northern hemisphere, Winter Solstice occurs on about December 21, Summer Solstice is near June 21, Spring Equinox is around March 20 and Autumnal Equinox is about September 23. In the Southern hemisphere, the situation is reversed, with the Summer and Winter Solstices exchanged and the Spring and Autumnal Equinox dates switched.[103]

NASA's Cassini spacecraft photographs Earth and the Moon (visible bottom-right) from Saturn (July 19, 2013).

The angle of Earth's axial tilt is relatively stable over long periods of time. Its axials tilt does undergo nutation; a slight, irregular motion with a main period of 18.6 years.[104] The orientation (rather than the angle) of Earth's axis also changes over time, precessing around in a complete circle over each 25,800 year cycle; this precession is the reason for the difference between a sidereal year and a tropical year. Both of these motions are caused by the varying attraction of the Sun and the Moon on Earth's equatorial bulge. The poles also migrate a few meters across Earth's surface. This polar motion has multiple, cyclical components, which collectively are termed quasiperiodic motion. In addition to an annual component to this motion, there is a 14-month cycle called the Chandler wobble. Earth's rotational velocity also varies in a phenomenon known as length-of-day variation.[105]

In modern times, Earth's perihelion occurs around January 3, and its aphelion around July 4. These dates change over time due to precession and other orbital factors, which follow cyclical patterns known as Milankovitch cycles. The changing Earth–Sun distance causes an increase of about 6.9%[n 7] in solar energy reaching Earth at perihelion relative to aphelion. Because the southern hemisphere is tilted toward the Sun at about the same time that Earth reaches the closest approach to the Sun, the southern hemisphere receives slightly more energy from the Sun than does the northern over the course of a year. This effect is much less significant than the total energy change due to the axial tilt, and most of the excess energy is absorbed by the higher proportion of water in the southern hemisphere.[106]


{{#invoke:see also|seealso}}

This ancient impact crater, now filled with water, marks Earth's surface

A planet that can sustain life is termed habitable, even if life did not originate there. Earth provides liquid water—an environment where complex organic molecules can assemble and interact, and sufficient energy to sustain metabolism.[107] The distance of Earth from the Sun, as well as its orbital eccentricity, rate of rotation, axial tilt, geological history, sustaining atmosphere and protective magnetic field all contribute to the current climatic conditions at the surface.[108]



Coral reef and beach

A planet's life forms are sometimes said to form a "biosphere". Earth's biosphere is generally believed to have begun evolving about Template:Val.[71] The biosphere is divided into a number of biomes, inhabited by broadly similar plants and animals. On land, biomes are separated primarily by differences in latitude, height above sea level and humidity. Terrestrial biomes lying within the Arctic or Antarctic Circles, at high altitudes or in extremely arid areas are relatively barren of plant and animal life; species diversity reaches a peak in humid lowlands at equatorial latitudes.[109]

Evolution of life


Speculative phylogenetic tree of life on Earth based on rRNA analysis

Highly energetic chemical reactions are thought to have produced self–replicating molecules around four billion years ago. This was followed a half billion years later by the last common ancestor of all life.[110] The development of photosynthesis allowed the Sun's energy to be harvested directly by life forms; the resultant molecular oxygen (O2) accumulated in the atmosphere and due to interaction with high energy solar radiation, formed a layer of protective ozone (O3) in the upper atmosphere.[71] The incorporation of smaller cells within larger ones resulted in the development of complex cells called eukaryotes.[111] True multicellular organisms formed as cells within colonies became increasingly specialized. Aided by the absorption of harmful ultraviolet radiation by the ozone layer, life colonized Earth's surface.[112] The earliest fossil evidences for life are graphite found to be biogenic in 3.7 billion-year-old metasedimentary rocks discovered in Western Greenland[113] and microbial mat fossils found in 3.48 billion-year-old sandstone discovered in Western Australia.[114][115]

Since the 1960s, it has been hypothesized that severe glacial action between 750 and Template:Val, during the Neoproterozoic, covered much of the planet in a sheet of ice. This hypothesis has been termed "Snowball Earth", and is of particular interest because it preceded the Cambrian explosion, when multicellular life forms began to proliferate.[116]

Following the Cambrian explosion, about Template:Val, there have been five major mass extinctions.[117] The most recent such event was Template:Val, when an asteroid impact triggered the extinction of the (non-avian) dinosaurs and other large reptiles, but spared some small animals such as mammals, which then resembled shrews. Over the past Template:Val, mammalian life has diversified, and several million years ago an African ape-like animal such as Orrorin tugenensis gained the ability to stand upright.[118] This enabled tool use and encouraged communication that provided the nutrition and stimulation needed for a larger brain, which allowed the evolution of the human race. The development of agriculture, and then civilization, allowed humans to influence Earth in a short time span as no other life form had,[119] affecting both the nature and quantity of other life forms.

Natural resources and land use


Estimated human land use, 2000[120]
Land use Mha
Cropland 1,510–1,611
Pastures 2,500–3,410
Natural forests 3,143–3,871
Planted forests 126–215
Urban areas 66–351
Unused, productive land 356–445

Earth provides resources that are exploitable by humans for useful purposes. Some of these are non-renewable resources, such as fossil fuels, that are difficult to replenish on a short time scale.

Large deposits of fossil fuels are obtained from Earth's crust, consisting of coal, petroleum and natural gas. These deposits are used by humans both for energy production and as feedstock for chemical production. Mineral ore bodies have also been formed within the crust through a process of ore genesis, resulting from actions of magmatism, erosion and plate tectonics.[121] These bodies form concentrated sources for many metals and other useful elements.

Earth's biosphere produces many useful biological products for humans, including food, wood, pharmaceuticals, oxygen, and the recycling of many organic wastes. The land-based ecosystem depends upon topsoil and fresh water, and the oceanic ecosystem depends upon dissolved nutrients washed down from the land.[122] In 1980, 5,053 Mha (50.53 million km2) of Earth's land surface consisted of forest and woodlands, 6,788 Mha (67.88 million km2) was grasslands and pasture, and 1,501 Mha (15.01 million km2) was cultivated as croplands.[123] The estimated amount of irrigated land in 1993 was Template:Convert.[56] Humans also live on the land by using building materials to construct shelters.

Natural and environmental hazards

Earth's volcanoes can inject gas and ash into the atmosphere.

Large areas of Earth's surface are subject to extreme weather such as tropical cyclones, hurricanes, or typhoons that dominate life in those areas. From 1980 to 2000, these events caused an average of 11,800 deaths per year.[124] Many places are subject to earthquakes, landslides, tsunamis, volcanic eruptions, tornadoes, sinkholes, blizzards, floods, droughts, wildfires, and other calamities and disasters.

Many localized areas are subject to human-made pollution of the air and water, acid rain and toxic substances, loss of vegetation (overgrazing, deforestation, desertification), loss of wildlife, species extinction, soil degradation, soil depletion, erosion, and introduction of invasive species.

According to the United Nations, a scientific consensus exists linking human activities to global warming due to industrial carbon dioxide emissions. This is predicted to produce changes such as the melting of glaciers and ice sheets, more extreme temperature ranges, significant changes in weather and a global rise in average sea levels.[125]

Human geography

{{#invoke:main|main}} Template:World map indicating continents

A composite picture consisting of DMSP/OLS ground-illumination data for 2000 placed on a simulated night-time image of Earth.

Cartography, the study and practice of map-making, and geography, the study of the lands, features, inhabitants and phenomena on Earth, have historically been the disciplines devoted to depicting Earth. Surveying, the determination of locations and distances, and to a lesser extent navigation, the determination of position and direction, have developed alongside cartography and geography, providing and suitably quantifying the requisite information.

Earth's human population reached approximately seven billion on October 31, 2011.[126] Projections indicate that the world's human population will reach 9.2 billion in 2050.[127] Most of the growth is expected to take place in developing nations. Human population density varies widely around the world, but a majority live in Asia. By 2020, 60% of the world's population is expected to be living in urban, rather than rural, areas.[128]

It is estimated that one-eighth of Earth's surface is suitable for humans to live on – three-quarters of Earth's surface is covered by oceans, leaving one quarter as land. Half of that land area is desert (14%),[129] high mountains (27%),[130] or other unsuitable terrain. The northernmost permanent settlement in the world is Alert, on Ellesmere Island in Nunavut, Canada.[131] (82°28′N) The southernmost is the Amundsen–Scott South Pole Station, in Antarctica, almost exactly at the South Pole. (90°S)

In 2000, 90% of all humans lived in the Northern Hemisphere. Half lived north of 27° N latitude.[132] An estimated 86% of all people live in the Eastern Hemisphere.[133]

Independent sovereign nations claim the planet's entire land surface, except for some parts of Antarctica, a few land parcels along the Danube river's western bank, and the odd unclaimed area of Bir Tawil between Egypt and Sudan. Template:As of, there are 205 de facto sovereign states, including the 193 United Nations member states. In addition, there are 59 dependent territories, and a number of autonomous areas, territories under dispute and other entities.[56] Historically, Earth has never had a sovereign government with authority over the entire globe although a number of nation-states have striven for world domination and failed.[134]

The United Nations is a worldwide intergovernmental organization that was created with the goal of intervening in the disputes between nations, thereby avoiding armed conflict.[135] The U.N. serves primarily as a forum for international diplomacy and international law. When the consensus of the membership permits, it provides a mechanism for armed intervention.[136]

The first human to orbit Earth was Yuri Gagarin on April 12, 1961.[137] In total, about 487 people have visited outer space and reached orbit Template:As of, and, of these, twelve have walked on the Moon.[138][139][140] Normally, the only humans in space are those on the International Space Station. The station's crew, made up of six people, is usually replaced every six months.[141] The farthest that humans have travelled from Earth is 400,171 km, achieved during the Apollo 13 mission in 1970.[142]

Cultural and historical viewpoint


The first "earthrise" ever seen directly by humans, photographed by astronauts on board Apollo 8.

The standard astronomical symbol of Earth consists of a cross circumscribed by a circle, Earth symbol.svg.[143]

Unlike other planets in the Solar System, humankind did not begin to view Earth as a moving object until the 16th century.[144] Earth has often been personified as a deity, in particular a goddess. In many cultures a mother goddess is also portrayed as a fertility deity. Creation myths in many religions recall a story involving the creation of Earth by a supernatural deity or deities. A variety of religious groups, often associated with fundamentalist branches of Protestantism[145] or Islam,[146] assert that their interpretations of these creation myths in sacred texts are literal truth and should be considered alongside or replace conventional scientific accounts of the formation of Earth and the origin and development of life.[147] Such assertions are opposed by the scientific community[148][149] and by other religious groups.[150][151][152] A prominent example is the creation–evolution controversy.

In the past, there were varying levels of belief in a flat Earth,[153] but this was displaced by spherical Earth, a concept that has been credited to Pythagoras (6th century BC).[154] Human cultures have developed many views of the planet, including its personification as a planetary deity, its shape as flat, its position as the center of the universe, and in the modern Gaia Principle, as a single, self-regulating organism in its own right.




Artist's impression of the birth of the Solar System

The earliest material found in the Solar System is dated to Template:Val (bya);[155] therefore, it is inferred that Earth must have been formed by accretion around this time. By Template:Val[8] the primordial Earth had formed. The formation and evolution of the Solar System bodies occurred in tandem with the Sun. In theory a solar nebula partitions a volume out of a molecular cloud by gravitational collapse, which begins to spin and flatten into a circumstellar disk, and then the planets grow out of that in tandem with the star. A nebula contains gas, ice grains and dust (including primordial nuclides). In nebular theory planetesimals commence forming as particulate accrues by cohesive clumping and then by gravity. The assembly of the primordial Earth proceeded for 10–Template:Val.[156] The Moon formed shortly thereafter, about Template:Val.[157]

The formation of the Moon remains a topic of debate. The working hypothesis is that it formed by accretion from material loosed from Earth after a Mars-sized object, named Theia, impacted with Earth.[158] This model, however, is not self-consistent. In this scenario, the mass of Theia is 10% of that of Earth,[159] it impacted Earth with a glancing blow,[160] and some of its mass merges with Earth. Between approximately 3.8 and Template:Val, numerous asteroid impacts during the Late Heavy Bombardment caused significant changes to the greater surface environment of the Moon, and by inference, to Earth.

Geological history

{{#invoke:main|main}} Earth's atmosphere and oceans formed by volcanic activity and outgassing that included water vapor. The origin of the world's oceans was condensation augmented by water and ice delivered by asteroids, proto-planets, and comets.[161] In this model, atmospheric "greenhouse gases" kept the oceans from freezing when the newly forming Sun had only 70% of its current luminosity.[162] By Template:Val, the Earth's magnetic field was established, which helped prevent the atmosphere from being stripped away by the solar wind.[163] A crust formed when the molten outer layer of Earth cooled to form a solid as the accumulated water vapor began to act in the atmosphere. The two models[164] that explain land mass propose either a steady growth to the present-day forms[165] or, more likely, a rapid growth[166] early in Earth history[167] followed by a long-term steady continental area.[168][169][170] Continents formed by plate tectonics, a process ultimately driven by the continuous loss of heat from Earth's interior. On time scales lasting hundreds of millions of years, the supercontinents have formed and broken up three times. Roughly Template:Val (million years ago), one of the earliest known supercontinents, Rodinia, began to break apart. The continents later recombined to form Pannotia, 600–Template:Val, then finally Pangaea, which also broke apart Template:Val.[171]

The present pattern of ice ages began about Template:Val and then intensified during the Pleistocene about Template:Val. High-latitude regions have since undergone repeated cycles of glaciation and thaw, repeating every 40–Template:Val. The last continental glaciation ended 10,000 years ago.[172]

Predicted future

{{#invoke:main|main}} Estimates on how much longer the planet will be able to continue to support life range from 500 million years (myr), to as long as 2.3 billion years (byr).[173][174][175] The future of the planet is closely tied to that of the Sun. As a result of the steady accumulation of helium at the Sun's core, the star's total luminosity will slowly increase. The luminosity of the Sun will grow by 10% over the next Template:Val and by 40% over the next Template:Val.[176] Climate models indicate that the rise in radiation reaching Earth is likely to have dire consequences, including the loss of the planet's oceans.[177]

Earth's increasing surface temperature will accelerate the inorganic CO2 cycle, reducing its concentration to levels lethally low for plants (Template:Val for C4 photosynthesis) in approximately 500-Template:Val.[173] The lack of vegetation will result in the loss of oxygen in the atmosphere, so animal life will become extinct within several million more years.[178] After another billion years all surface water will have disappeared[174] and the mean global temperature will reach Template:Val[178] (Template:Val). Earth is expected to be effectively habitable for about another Template:Val from that point,[173] although this may be extended up to Template:Val if the nitrogen is removed from the atmosphere.[175] Even if the Sun were eternal and stable, 27% of the water in the modern oceans will descend to the mantle in one billion years, due to reduced steam venting from mid-ocean ridges.[179]

14 billion year timeline showing Sun's present age at Template:Val; from Template:Val Sun gradually warming, becoming a red dwarf at Template:Val, "soon" followed by its transformation into a white dwarf star
Life cycle of the Sun

The Sun, as part of its evolution, will become a red giant in about Template:Val. Models predict that the Sun will expand to roughly Template:Convert, which is about 250 times its present radius.[176][180] Earth's fate is less clear. As a red giant, the Sun will lose roughly 30% of its mass, so, without tidal effects, Earth will move to an orbit Template:Convert from the Sun, when the star reaches its maximum radius. The planet was, therefore, initially expected to escape envelopment by the expanded Sun's sparse outer atmosphere, though most, if not all, remaining life would have been destroyed by the Sun's increased luminosity (peaking at about 5,000 times its present level).[176] A 2008 simulation indicates that Earth's orbit will decay due to tidal effects and drag, causing it to enter the red giant Sun's atmosphere and be vaporized.[180] After that, the Sun's core will collapse into a white dwarf, as its outer layers are ejected into space as a planetary nebula. The matter that once made up Earth will be released into interstellar space, where it may one day become incorporated into a new generation of planets and other celestial bodies. {{#invoke:see also|seealso}}


Diameter 3,474.8 km
Mass 7.349Template:E kg
Semi-major axis 384,400 km
Orbital period 27 d 7 h 43.7 m
Details of the Earth–Moon system. Besides the radius of each object, the radius to the Earth–Moon barycenter is shown. Photos from NASA. Data from NASA. The Moon's axis is located by Cassini's third law.
Full moon as seen from Earth's northern hemisphere

{{#invoke:main|main}} The Moon is a relatively large, terrestrial, planet-like satellite, with a diameter about one-quarter of Earth's. It is the largest moon in the Solar System relative to the size of its planet, although Charon is larger relative to the dwarf planet Pluto. The natural satellites orbiting other planets are called "moons" after Earth's Moon.

The gravitational attraction between Earth and the Moon causes tides on Earth. The same effect on the Moon has led to its tidal locking: its rotation period is the same as the time it takes to orbit Earth. As a result, it always presents the same face to the planet. As the Moon orbits Earth, different parts of its face are illuminated by the Sun, leading to the lunar phases; the dark part of the face is separated from the light part by the solar terminator.

Due to their tidal interaction, the Moon recedes from Earth at the rate of approximately 38 mm a year. Over millions of years, these tiny modifications—and the lengthening of Earth's day by about 23 µs a year—add up to significant changes.[181] During the Devonian period, for example, (approximately Template:Val) there were 400 days in a year, with each day lasting 21.8 hours.[182]

The Moon may have dramatically affected the development of life by moderating the planet's climate. Paleontological evidence and computer simulations show that Earth's axial tilt is stabilized by tidal interactions with the Moon.[183] Some theorists believe that without this stabilization against the torques applied by the Sun and planets to Earth's equatorial bulge, the rotational axis might be chaotically unstable, exhibiting chaotic changes over millions of years, as appears to be the case for Mars.[184]

Viewed from Earth, the Moon is just far enough away to have almost the same apparent-sized disk as the Sun. The angular size (or solid angle) of these two bodies match because, although the Sun's diameter is about 400 times as large as the Moon's, it is also 400 times more distant.[98] This allows total and annular solar eclipses to occur on Earth.

The most widely accepted theory of the Moon's origin, the giant impact theory, states that it formed from the collision of a Mars-size protoplanet called Theia with the early Earth. This hypothesis explains (among other things) the Moon's relative lack of iron and volatile elements, and the fact that its composition is nearly identical to that of Earth's crust.[185]

Scale representation of the relative sizes of, and average distance between, Earth and the Moon

Asteroids and artificial satellites

The International Space Station is an artificial satellite in orbit around Earth.

Earth has at least five co-orbital asteroids, including 3753 Cruithne and 2002 AA29.[186][187] A trojan asteroid companion, 2010 TK7, is librating around the leading Lagrange triangular point, L4, in the Earth's orbit around the Sun.[188][189]

Template:As of, there were 931 operational, man-made satellites orbiting Earth.[190] There are also inoperative satellites and over 300,000 pieces of space debris. Earth's largest artificial satellite is the International Space Station.


  1. The number of solar days is one less than the number of sidereal days because the orbital motion of Earth around the Sun causes one additional revolution of the planet about its axis.
  2. Locally varies between 5 and 200 km.
  3. Locally varies between 5 and 70 km.
  4. This is the measurement taken by the vessel Kaikō in March 1995 and is believed to be the most accurate measurement to date. See the Challenger Deep article for more details.
  5. Aoki, the ultimate source of these figures, uses the term "seconds of UT1" instead of "seconds of mean solar time".—{{#invoke:Citation/CS1|citation |CitationClass=journal }}
  6. For Earth, the Hill radius is , where m is the mass of Earth, a is an astronomical unit, and M is the mass of the Sun. So the radius in A.U. is about .
  7. Aphelion is 103.4% of the distance to perihelion. Due to the inverse square law, the radiation at perihelion is about 106.9% the energy at aphelion.

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See also


  1. Oxford English Dictionary, 1st ed. "terra, n." Oxford University Press (Oxford), 1911.
  2. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  3. {{#invoke:citation/CS1|citation |CitationClass=book }}
  4. Template:Cite news
  5. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  6. {{#invoke:citation/CS1|citation |CitationClass=book }}
  7. Template:Cite web
  8. 8.0 8.1 See:
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    |CitationClass=book }} |CitationClass=journal }}
  9. {{#invoke:citation/CS1|citation |CitationClass=book }}
  10. Template:Cite web
  11. {{#invoke:citation/CS1|citation |CitationClass=book }}
  12. 12.0 12.1 Oxford English Dictionary, 3rd ed. "earth, n.¹" Oxford University Press (Oxford), 2010.
  13. Tacitus. Germania, Ch. 40.
  14. Simek, Rudolf. Trans. Angela Hall as Dictionary of Northern Mythology, p. 179. D.S. Brewer, 2007. ISBN 0-85991-513-1.
  15. The New Oxford Dictionary of English, 1st ed. "earth". Oxford University Press (Oxford), 1998. ISBN 0-19-861263-X.
  16. Template:Cite web
  17. 17.0 17.1 Template:Cite web
  18. The 'Highest' Spot on Earth? Consultado el 25-07-2010
  19. Template:Cite web
  20. Template:Cite web
  21. 21.0 21.1 Template:Cite web
  22. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  23. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  24. Template:Cite web
  25. {{#invoke:citation/CS1|citation |CitationClass=book }} Note: After Ronov and Yaroshevsky (1969).
  26. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  27. Template:Hide in printOne or more of the preceding sentences incorporates text from a publication now in the public domainTemplate:Cite EB1911
  28. {{#invoke:citation/CS1|citation |CitationClass=book }}
  29. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  30. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  31. Template:Cite web
  32. 32.0 32.1 {{#invoke:citation/CS1|citation |CitationClass=book }}
  33. Template:Cite news
  35. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  36. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  37. {{#invoke:citation/CS1|citation |CitationClass=book }}
  38. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  39. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  40. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  41. Template:Cite web
  42. Template:Cite web
  43. Template:Cite web
  44. Template:Cite web
  45. Template:Cite web
  46. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  47. Template:Cite web
  48. Template:Cite web
  49. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  50. Template:Cite web
  51. Template:Cite web
  52. Template:Cite web
  53. Template:Cite web
  54. {{#invoke:citation/CS1|citation |CitationClass=book }}
  55. {{#invoke:citation/CS1|citation |CitationClass=book }}
  56. 56.0 56.1 56.2 Template:Cite web
  57. {{#invoke:citation/CS1|citation |CitationClass=book }}
  58. {{#invoke:citation/CS1|citation |CitationClass=book }}
  59. Template:Cite web
  60. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  61. Sphere depth of the ocean, Encyclopædia Britannica
  62. Third rock from the Sun - restless Earth, NASA's Cosmos
  63. "The World of Water", USGS
  64. {{#invoke:citation/CS1|citation |CitationClass=book }}
  65. Template:Cite web
  66. Template:Cite web
  67. Template:Cite web
  68. Template:Cite web
  69. 69.0 69.1 Template:Cite web
  70. Template:Cite web
  71. 71.0 71.1 71.2 Template:Cite news
  72. 72.0 72.1 Template:Cite web
  73. Template:Cite web
  74. 74.0 74.1 Template:Cite web
  75. 75.0 75.1 Template:Cite web
  76. Template:Cite web
  77. Template:Cite web
  78. {{#invoke:citation/CS1|citation |CitationClass=book }}
  79. Template:Cite web
  80. Template:Cite web
  81. Template:Cite web
  82. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  83. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  84. Template:Cite web
  85. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  86. {{#invoke:citation/CS1|citation |CitationClass=book }}
  87. Template:Cite web
  88. {{#invoke:citation/CS1|citation |CitationClass=book }}
  89. Template:Cite web
  90. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  91. Template:Cite web
  93. 93.0 93.1 Template:Cite web
  94. {{#invoke:citation/CS1|citation |CitationClass=book }}
  95. Template:Cite web—Graph at end.
  96. Template:Cite web
  97. {{#invoke:citation/CS1|citation |CitationClass=book }}
  98. 98.0 98.1 Template:Cite web—See the apparent diameters on the Sun and Moon pages.
  99. Cite error: Invalid <ref> tag; no text was provided for refs named earth fact sheet
  100. Template:Cite web
  101. Template:Cite web
  102. Template:Cite web
  103. Template:Cite web
  104. Template:Cite web
  105. Template:Cite web
  106. Template:Cite web
  107. Template:Cite web
  108. {{#invoke:citation/CS1|citation |CitationClass=book }}
  109. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  110. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  111. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  112. Template:Cite web
  113. Template:Cite web
  114. Template:Cite news
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  117. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
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  119. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  120. {{#invoke:Citation/CS1|citation |CitationClass=journal }} See Table 1.
  121. Template:Cite web
  122. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  123. {{#invoke:citation/CS1|citation |CitationClass=book }}
  124. {{#invoke:citation/CS1|citation |CitationClass=book }}
  125. Template:Cite web
  126. Template:Cite web
  127. Template:Cite web
  128. Template:Cite web
  129. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  130. Template:Cite web
  131. Template:Cite web
  132. [1]
  133. [2]
  134. {{#invoke:citation/CS1|citation |CitationClass=book }}
  135. Template:Cite web
  136. Template:Cite web
  137. {{#invoke:citation/CS1|citation |CitationClass=book }}
  138. {{#invoke:citation/CS1|citation |CitationClass=book }}
  139. {{#invoke:citation/CS1|citation |CitationClass=book }}
  140. Template:Cite web
  141. Template:Cite web
  142. Template:Cite news
  143. {{#invoke:citation/CS1|citation |CitationClass=book }}
  144. Template:Cite web
  145. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
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  147. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
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  151. {{#invoke:citation/CS1|citation |CitationClass=book }}
  152. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  153. Template:Cite web; but see also Cosmas Indicopleustes.
  154. Template:Cite web
  155. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  156. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
  157. {{#invoke:Citation/CS1|citation |CitationClass=journal }}
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  172. Template:Cite web
  173. 173.0 173.1 173.2 Template:Cite web
  174. 174.0 174.1 Template:Cite news
  175. 175.0 175.1 {{#invoke:Citation/CS1|citation |CitationClass=journal }}
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  181. Template:Cite web
  182. Template:Cite web
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Further reading

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External links