Kyrie

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| talk = | other | #default = }} | #default =}}|}} Template:Infobox Planet

Earth (or the Earth) is the third planet from the Sun and the densest and fifth-largest of the eight planets in the Solar System. It is also the largest of the Solar System's four terrestrial planets. It is sometimes referred to as the World, the Blue Planet, or by its Latin name, Terra.<ref group=note name="blue planet" /><ref group=note name="Terra" />

Home to millions of species including humans, Earth is currently the only astronomical body where life is known to exist.<ref name=science_241_4872_1441 /> The planet formed 4.54 billion years ago, and life appeared on its surface within a billion years.<ref name="age_earth1" /> Earth's biosphere has significantly altered the atmosphere and other abiotic conditions on the planet, enabling the proliferation of aerobic organisms as well as the formation of the ozone layer which, together with Earth's magnetic field, blocks harmful solar radiation, permitting life on land.<ref name="Harrison 2002" /> The physical properties of the Earth, as well as its geological history and orbit, have allowed life to persist during this period. The planet is expected to continue supporting life for at least another Template:Nowrap years.<ref name="britt2000" /><ref name=carrington />

Earth's outer surface is divided into several rigid segments, or tectonic plates, that migrate across the surface over periods of many millions of years. About 71% of the surface is covered with salt water oceans, the remainder consisting of continents and islands which together have many lakes and other sources of water contributing to the hydrosphere. Liquid water, necessary for all known life, is not known to exist in equilibrium on any other planet's surface.<ref group=note name="water vapor"/> Earth's poles are mostly covered with solid ice (Antarctic ice sheet) or sea ice (Arctic ice cap). The planet's interior remains active, with a thick layer of relatively solid mantle, a liquid outer core that generates a magnetic field, and a solid iron inner core.

Earth interacts with other objects in space, especially the Sun and the Moon. At present, Earth orbits the Sun once for every roughly 366.26 times it rotates about its axis, which is equal to 365.26 solar days, or one sidereal year.<ref group=note name=sidereal_solar/> The Earth's axis of rotation is tilted 23.4° away from the perpendicular to its orbital plane, producing seasonal variations on the planet's surface with a period of one tropical year (365.24 solar days).<ref name=yoder1995/> Earth's only known natural satellite, the Moon, which began orbiting it about Template:Nowrap years ago, provides ocean tides, stabilizes the axial tilt and gradually slows the planet's rotation. Between approximately Template:Nowrap and Template:Nowrap years ago, numerous asteroid impacts during the Late Heavy Bombardment caused significant changes to the greater surface environment.

Both the mineral resources of the planet, as well as the products of the biosphere, contribute resources that are used to support a global human population. These inhabitants are grouped into about 200 independent sovereign states, which interact through diplomacy, travel, trade, and military action. Human cultures have developed many views of the planet, including personification as a deity, a belief in a flat Earth or in the Earth as the center of the universe, and a modern perspective of the world as an integrated environment that requires stewardship.

Chronology

Template:Main Template:See also Scientists have been able to reconstruct detailed information about the planet's past. The earliest dated Solar System material was formed Template:Nowrap ago,<ref name=bowring_housch1995/> and by 4.54 billion years ago (within an uncertainty of 1%)<ref name="age_earth1" /> the Earth and the other planets in the Solar System had formed out of the solar nebula—a disk-shaped mass of dust and gas left over from the formation of the Sun. This assembly of the Earth through accretion was thus largely completed within 10–20 million years.<ref name=nature418_6901_949/> Initially molten, the outer layer of the planet Earth cooled to form a solid crust when water began accumulating in the atmosphere. The Moon formed shortly thereafter, Template:Nowrap ago.<ref name=science310_5754_1671/>

The current consensus model<ref name=reilly20091022/> for the formation of the Moon is the giant impact hypothesis, in which the Moon was created when a Mars-sized object (sometimes called Theia) with about 10% of the Earth's mass<ref name=canup_asphaug2001a/> impacted the Earth in a glancing blow.<ref name=canup_asphaug2001b/> In this model, some of this object's mass would have merged with the Earth and a portion would have been ejected into space, but enough material would have been sent into orbit to coalesce into the Moon.

Outgassing and volcanic activity produced the primordial atmosphere of the Earth. Condensing water vapor, augmented by ice and liquid water delivered by asteroids and the larger proto-planets, comets, and trans-Neptunian objects produced the oceans.<ref name="watersource"/> The newly formed Sun was only 70% of its present luminosity, yet evidence shows that the early oceans remained liquid—a contradiction dubbed the faint young Sun paradox. A combination of greenhouse gases and higher levels of solar activity served to raise the Earth's surface temperature, preventing the oceans from freezing over.<ref name=asp2002/> By Template:Nowrap years ago, the Earth's magnetic field was established, which helped prevent the atmosphere from being stripped away by the solar wind.<ref name=physorg20100304/>

Two major models have been proposed for the rate of continental growth:<ref name=williams_santosh2004/> steady growth to the present-day<ref name=science164_1229/> and rapid growth early in Earth history.<ref name=rg6_175/> Current research shows that the second option is most likely, with rapid initial growth of continental crust<ref name=tp322_19/> followed by a long-term steady continental area.<ref name=science310_5756_1947/><ref name=jaes23_799/><ref name=ajes38_613/> On time scales lasting hundreds of millions of years, the surface continually reshaped as continents formed and broke up. The continents migrated across the surface, occasionally combining to form a supercontinent. Roughly Template:Nowrap ago (Ma), one of the earliest known supercontinents, Rodinia, began to break apart. The continents later recombined to form Pannotia, 600–540 Ma, then finally Pangaea, which broke apart 180 Ma.<ref name=as92_324/>

Evolution of life

Template:Main

At present, Earth provides the only example of an environment that has given rise to the evolution of life.<ref name=purves_et_al2001/> Highly energetic chemistry is believed to have produced a self-replicating molecule around Template:Nowrap ago and half a billion years later the last common ancestor of all life existed.<ref name=sa282_6_90/> The development of photosynthesis allowed the Sun's energy to be harvested directly by life forms; the resultant oxygen accumulated in the atmosphere and formed a layer of ozone (a form of molecular oxygen [O₃]) in the upper atmosphere. The incorporation of smaller cells within larger ones resulted in the development of complex cells called eukaryotes.<ref name=jas22_3_225/> 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 the surface of Earth.<ref name=burton20021129/>

Since the 1960s, it has been hypothesized that severe glacial action between 750 and 580 Ma, 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.<ref name=kirschvink1992/>

Following the Cambrian explosion, about 535 Ma, there have been five major mass extinctions.<ref name=sci215_4539_1501/> The most recent such event was 65 Ma, 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 65 million years, mammalian life has diversified, and several million years ago an African ape-like animal such as Orrorin tugenensis gained the ability to stand upright.<ref name=gould1994/> 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 the Earth in a short time span as no other life form had,<ref name=bgsa119_1_140/> affecting both the nature and quantity of other life forms.

The present pattern of ice ages began about 40 Ma and then intensified during the Pleistocene about 3 Ma. High-latitude regions have since undergone repeated cycles of glaciation and thaw, repeating every 40–100,000 years. The last continental glaciation ended 10,000 years ago.<ref name=psc/>

Future

Template:Main Template:See also

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 1.1 Gyr (1.1 billion years) and by 40% over the next 3.5 Gyr.<ref name="sun_future"/> Climate models indicate that the rise in radiation reaching the Earth is likely to have dire consequences, including the loss of the planet's oceans.<ref name=icarus74_472/>

The Earth's increasing surface temperature will accelerate the inorganic CO₂ cycle, reducing its concentration to levels lethally low for plants (10 ppm for C4 photosynthesis) in approximately Template:Nowrap<ref name="britt2000" /> to Template:Nowrap years. 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.<ref name=ward_brownlee2002/> After another billion years all surface water will have disappeared<ref name=carrington/> and the mean global temperature will reach 70 °C<ref name=ward_brownlee2002/> (158 °F). The Earth is expected to be effectively habitable for about another Template:Nowrap years from that point,<ref name="britt2000"/> although this may be extended up to Template:Nowrap if the nitrogen is removed from the atmosphere.<ref name=pnas1_24_9576/> Even if the Sun were eternal and stable, the continued internal cooling of the Earth would result in a loss of much of its CO₂ due to reduced volcanism,<ref name=sec1014/> and 35% of the water in the oceans would descend to the mantle due to reduced steam venting from mid-ocean ridges.<ref name=hess5_4_569/>

The Sun, as part of its evolution, will become a red giant in about 5 Gyr. Models predict that the Sun will expand out to about 250 times its present radius, roughly {{#ifeq:|on|Template:Ntsh}}{{convert/{{#if:1|AU}}|1|{{#ifeq:{{#expr:km*0}}|0|0}}|km||||||r={{#ifeq:{{{sp}}}|us|er|re}}|d=LoffA{{#switch:on|off=none|def=off|on}}D{{#switch:{{{disp}}}|/|slash=s|b}}Soff|s=}}{{#switch:{{{disp}}}|br=|/=}}.<ref name="sun_future" /><ref name="sun_future_schroder"/> Earth's fate is less clear. As a red giant, the Sun will lose roughly 30% of its mass, so, without tidal effects, the Earth will move to an orbit {{#ifeq:|on|Template:Ntsh}}{{convert/{{#if:1|AU}}|1.7|{{#ifeq:{{#expr:km*0}}|0|0}}|km||||||r={{#ifeq:{{{sp}}}|us|er|re}}|d=LoffA{{#switch:on|off=none|def=off|on}}D{{#switch:{{{disp}}}|/|slash=s|b}}Soff|s=}}{{#switch:{{{disp}}}|br=|/=}} from the Sun when the star reaches it 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 5000 times its present level).<ref name="sun_future" /> However, 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.<ref name="sun_future_schroder" />

Composition and structure

Template:Main Template:See Earth is a terrestrial planet, meaning that it is a rocky body, rather than a gas giant like Jupiter. It is the largest of the four solar terrestrial planets in size and mass. Of these four planets, Earth also has the highest density, the highest surface gravity, the strongest magnetic field, and fastest rotation.<ref name=stern20011125/> It also is the only terrestrial planet with active plate tectonics.<ref name=science288_5473_2002/>

Shape

Template:Main

The shape of the Earth is very close to that of an oblate spheroid, a sphere flattened along the axis from pole to pole such that there is a bulge around the equator.<ref name=milbert_smith96/> This bulge results from the rotation of the Earth, and causes the diameter at the equator to be 43 km larger than the pole to pole diameter.<ref name="ngdc2006"/> The average diameter of the reference spheroid is about 12,742 km, which is approximately 40,000 km/π, as the meter was originally defined as 1/10,000,000 of the distance from the equator to the North Pole through Paris, France.<ref name=nist_length2000/>

Local topography deviates from this idealized spheroid, though on a global scale, these deviations are very small: Earth has a tolerance of about one part in about 584, or 0.17%, from the reference spheroid, which is less than the 0.22% tolerance allowed in billiard balls.<ref name=wpba2001/> The largest local deviations in the rocky surface of the Earth are Mount Everest (8848 m above local sea level) and the Mariana Trench (10,911 m below local sea level). Because of the equatorial bulge, the surface locations farthest from the center of the Earth are the summits of Mount Chimborazo in Ecuador and Huascarán in Peru.<ref name=ps20_5_16/><ref name=lancet365_9462_831/><ref name=tall_tales/>

Chemical composition

Template:See also The mass of the Earth is approximately 5.98{{#if:24

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| main = | other | #default = }} }} kg. 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.<ref name=pnas71_12_6973/>

The geochemist F. W. Clarke calculated that a little more than 47% of the Earth's crust consists of oxygen. The more common rock constituents of the Earth's crust are nearly all oxides; chlorine, sulfur and fluorine are the only 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). All the other constituents occur only in very small quantities.<ref>Template:1911</ref>

Internal structure

Template:Main The interior of the Earth, 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 of the Earth 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 6 km under the oceans and 30–50 km 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 comprised. 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 660 kilometers 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.<ref name=tanimoto_ahrens1995/> 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.<ref name=science309_5739_1313/>

Heat

Earth's internal heat comes from a combination of residual heat from planetary accretion (about 20%) and heat produced through radioactive decay (80%).<ref name="turcotte"/> The major heat-producing isotopes in the Earth are potassium-40, uranium-238, uranium-235, and thorium-232.<ref name=sanders20031210/> At the center of the planet, the temperature may be up to 7,000 K and the pressure could reach 360 GPa.<ref name=ptrsl360_1795_1227/> Because much of the heat is provided by radioactive decay, scientists believe that early in Earth 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 3 billion years ago,<ref name="turcotte" /> would have increased temperature gradients within the Earth, increasing the rates of mantle convection and plate tectonics, and allowing the production of igneous rocks such as komatiites that are not formed today.<ref name=epsl121_1/>

The mean heat loss from the Earth is Template:Nowrap, for a global heat loss of Template:Nowrap.<ref name=jg31_3_267/> 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.<ref name=science246_4926_103/> More of the heat in the 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 in the oceans because the crust there is much thinner than that of the continents.<ref name="heat loss" />

Tectonic plates

Template:Main The mechanically rigid outer layer of the 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.<ref name=kious_tilling1999/> 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,<ref name=seligman2008/> and their motion is strongly coupled with convection patterns inside the Earth's 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. Because of this recycling, most of the ocean floor is less than Template:Nowrap years in age. The oldest oceanic crust is located in the Western Pacific, and has an estimated age of about Template:Nowrap years.<ref name=duennebier1999/><ref name=noaa20070307/> By comparison, the oldest dated continental crust is Template:Nowrap years old.<ref name=cmp134_3/>

Other notable plates include the Indian Plate, 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:Nowrap years ago. The fastest-moving plates are the oceanic plates, with the Cocos Plate advancing at a rate of 75 mm/yr<ref name=podp2000/> and the Pacific Plate moving 52–69 mm/yr. At the other extreme, the slowest-moving plate is the Eurasian Plate, progressing at a typical rate of about 21 mm/yr.<ref name=gps_time_series/>

Surface

Template:Main The Earth's terrain varies greatly from place to place. About 70.8%<ref name="Pidwirny2006"/> of the surface is covered by water, with much of the continental shelf below sea level. The submerged surface has mountainous features, including a globe-spanning mid-ocean ridge system, as well as undersea volcanoes,<ref name="ngdc2006" /> oceanic trenches, submarine canyons, oceanic plateaus and abyssal plains. The remaining 29.2% not covered by water consists of mountains, deserts, plains, plateaus, and other geomorphologies.

The planetary surface undergoes reshaping over geological time periods because of tectonics and erosion. The surface features built up or deformed through plate tectonics are subject to steady weathering from precipitation, thermal cycles, and chemical effects. Glaciation, coastal erosion, the build-up of coral reefs, and large meteorite impacts<ref name=kring/> 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.<ref name=layers_earth/> Sedimentary rock is formed from the accumulation of sediment that becomes compacted together. Nearly 75% of the continental surfaces are covered by sedimentary rocks, although they form only about 5% of the crust.<ref name=jessey/> 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 the Earth's surface include quartz, the feldspars, amphibole, mica, pyroxene and olivine.<ref name=de_pater_lissauer2010/> Common carbonate minerals include calcite (found in limestone) and dolomite.<ref name=wekn_bulakh2004/>

The pedosphere is the outermost layer of the Earth that is composed of soil and subject to soil formation processes. It exists at the interface of the lithosphere, atmosphere, hydrosphere and biosphere. Currently the total arable land is 13.31% of the land surface, with only 4.71% supporting permanent crops.<ref name=cia/> Close to 40% of the Earth's land surface is presently used for cropland and pasture, or an estimated 1.3{{#if:7

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| main = | other | #default = }} }} km² of cropland and 3.4{{#if:7

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| main = | other | #default = }} }} km² of pastureland.<ref name=fao1994/>

The elevation of the land surface of the Earth 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.<ref name=sverdrup/>

Hydrosphere

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The abundance of water on Earth's surface is a unique feature that distinguishes the "Blue Planet" from others in the Solar System. The 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.<ref group="note" name=trench_depth/><ref name=kaiko7000/>

The mass of the oceans is approximately 1.35{{#if:18

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| main = | other | #default = }} }} metric tons, or about 1/4400 of the total mass of the Earth. The oceans cover an area of 361.8{{#if:6

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| main = | other | #default = }} }} km² with a mean depth of 3,682 m, resulting in an estimated volume of 1.332{{#if:9

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| main = | other | #default = }} }} km³.<ref name=ocean23_2_112/> If all the land on Earth were spread evenly, water would rise to an altitude of more than 2.7 km.<ref group=note>The total surface area of the Earth is 5.1{{#if:8

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| main = | other | #default = }} }} km². To first approximation, the average depth would be the ratio of the two, or 2.7 km.</ref> About 97.5% of the water is saline, while the remaining 2.5% is fresh water. Most fresh water, about 68.7%, is currently ice.<ref name=shiklomanov_et_al_1999/>

The average salinity of the Earth's oceans is about 35 grams of salt per kilogram of sea water (35 ‰).<ref name=kennish2001/> Most of this salt was released from volcanic activity or extracted from cool, igneous rocks.<ref name=mullen2002/> The oceans are also a reservoir of dissolved atmospheric gases, which are essential for the survival of many aquatic life forms.<ref name=natsci_oxy4/> Sea water has an important influence on the world's climate, with the oceans acting as a large heat reservoir.<ref name=michon2006/> Shifts in the oceanic temperature distribution can cause significant weather shifts, such as the El Niño-Southern Oscillation.<ref name=sample2005/>

Atmosphere

Template:Main The atmospheric pressure on the surface of the Earth averages 101.325 kPa, with a scale height of about 8.5 km.<ref name="earth_fact_sheet"/> It is 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.<ref name=geerts_linacre97/>

Earth's biosphere has significantly altered its atmosphere. Oxygenic photosynthesis evolved Template:Nowrap years ago, forming the primarily nitrogen-oxygen atmosphere of today. 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 on Earth include transporting water vapor, providing useful gases, causing small meteors to burn up before they strike the surface, and moderating temperature.<ref name="atmosphere"/> 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. Carbon dioxide, water vapor, methane and ozone are the primary greenhouse gases in the Earth's atmosphere. Without this heat-retention effect, the average surface temperature would be −18 °C and life would likely not exist.<ref name="Pidwirny2006" />

Weather and climate

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The 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 planet's 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 heat energy.<ref name="moran2005"/>

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°.<ref name="berger2002"/> Ocean currents are also important factors in determining climate, particularly the thermohaline circulation that distributes heat energy from the equatorial oceans to the polar regions.<ref name=rahmstorf2003/>

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 settles to the surface as precipitation.<ref name="moran2005" /> 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, topological features and temperature differences determine the average precipitation that falls in each region.<ref name=hydrologic_cycle/>

The amount of solar energy reaching the Earth's decreases with increasing latitude. At higher latitudes the sunlight reaches the surface at a 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 per degree of latitude away from the equator.<ref name=sadava_heller2006/> The Earth can be sub-divided 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.<ref name=climate_zones/> 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.<ref name="berger2002" />

Upper atmosphere

Template:See also Above the troposphere, the atmosphere is usually divided into the stratosphere, mesosphere, and thermosphere.<ref name="atmosphere" /> 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 Earth's magnetic fields interact with the solar wind.<ref name=sciweek2004/> 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 the Earth's surface, is a working definition for the boundary between atmosphere and space.<ref name=cordoba2004/>

Thermal energy causes some of the molecules at the outer edge of the Earth's atmosphere have their velocity increased to the point where they can escape from the planet's gravity. This results in a slow but steady leakage of the atmosphere into space. Because unfixed hydrogen has a low molecular weight, it can achieve escape velocity more readily and it leaks into outer space at a greater rate than other gasses.<ref name=jas31_4_1118/> The leakage of hydrogen into space contributes to the pushing of the Earth 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.<ref name=sci293_5531_839/> Hence the ability of hydrogen to escape from the Earth's atmosphere may have influenced the nature of life that developed on the planet.<ref name=abedon1997/> 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.<ref name=arwps4_265/>

Magnetic field

Template:Main The Earth's magnetic field is shaped roughly as a magnetic dipole, with the poles currently located proximate to the planet's geographic poles. At the equator of the magnetic field, the magnetic field strength at the planet's surface is Template:Nowrap, with global magnetic dipole moment of Template:Nowrap.<ref name=lang2003/> According to dynamo theory, the field is generated within the molten outer core region where heat creates convection motions of conducting materials, generating electric currents. These in turn produce the Earth's magnetic field. The convection movements in the core are chaotic; the magnetic poles drift and periodically change alignment. This results in field reversals at irregular intervals averaging a few times every million years. The most recent reversal occurred approximately 700,000 years ago.<ref name=fitzpatrick2006/><ref name=campbelwh/>

The field forms the magnetosphere, which deflects particles in the solar wind. The sunward edge of the bow shock is located at about 13 times the radius of the Earth. The collision between the magnetic field and the solar wind forms the Van Allen radiation belts, a pair of concentric, torus-shaped regions of energetic charged particles. When the plasma enters the Earth's atmosphere at the magnetic poles, it forms the aurora.<ref name=stern2005/>

Orbit and rotation

Rotation

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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).<ref name=aj136_5_1906/> As the Earth's solar day is now slightly longer than it was during the 19th century because of tidal acceleration, each day varies between 0 and 2 SI ms longer.<ref name=USNO_TSD/><ref>http://maia.usno.navy.mil/ser7/ser7.dat</ref>

Earth's rotation period relative to the fixed stars, called its stellar day by the International Earth Rotation and Reference Systems Service (IERS), is Template:Nowrap of mean solar time (UT1), or Template:Nowrap<ref name=IERS/><ref group=note name=Aoki/> Earth's rotation period relative to the precessing or moving mean vernal equinox, misnamed its sidereal day, is Template:Nowrap of mean solar time (UT1) Template:Nowrap.<ref name=IERS/> Thus the sidereal day is shorter than the stellar day by about 8.4 ms.<ref name=seidelmann1992/> The length of the mean solar day in SI seconds is available from the IERS for the periods 1623–2005<ref name=iers1623/> and 1962–2005.<ref name=iers1962/>

Apart from meteors within the atmosphere and low-orbiting satellites, the main apparent motion of celestial bodies in the 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 Moon every two minutes; from the planet's surface, the apparent sizes of the Sun and the Moon are approximately the same.<ref name=zeilik1998/><ref name=angular/>

Orbit

Template:Main Earth orbits the Sun at an average distance of about 150 million kilometers every 365.2564 mean solar days, or one sidereal year. From Earth, this gives an apparent movement of the Sun eastward with respect to the stars at a rate of about 1°/day, or a Sun or Moon diameter every 12 hours. Because of 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 the Earth averages about 30 km/s (108,000 km/h), which is fast enough to cover the planet's diameter (about 12,600 km) in seven minutes, and the distance to the Moon (384,000 km) in four hours.<ref name="earth_fact_sheet"/>

The Moon revolves with the Earth around a common barycenter every 27.32 days relative to the background stars. When combined with the Earth–Moon system's common revolution 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 counter-clockwise. Viewed from a vantage point above the north poles of both the Sun and the Earth, the Earth appears to revolve in a counterclockwise direction about the Sun. The orbital and axial planes are not precisely aligned: Earth's axis is tilted some 23.5 degrees from the perpendicular to the Earth–Sun plane, and the Earth–Moon plane is tilted about 5 degrees against the Earth-Sun plane. Without this tilt, there would be an eclipse every two weeks, alternating between lunar eclipses and solar eclipses.<ref name="earth_fact_sheet" /><ref name="moon_fact_sheet"/>

The Hill sphere, or gravitational sphere of influence, of the Earth is about 1.5 Gm (or 1,500,000 kilometers) in radius.<ref name=vazquez_etal2006/><ref name=hill_radius group=note/> This is maximum distance at which the Earth's gravitational influence is stronger than the more distant Sun and planets. Objects must orbit the 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, orbiting about 28,000 light years from the center of the galaxy. It is currently about 20 light years above the galaxy's equatorial plane in the Orion spiral arm.<ref name=nasa20051201/>

Axial tilt and seasons

Template:Main Because of the axial tilt of the Earth, the amount of sunlight reaching any given point on the surface varies over the course of the year. This results in 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. Above the Arctic Circle, an extreme case is reached where there is no daylight at all for part of the year—a polar night. In the southern hemisphere the situation is exactly reversed, with the South Pole oriented opposite the direction of the North 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.<ref name=bromberg2008/>

The angle of the Earth's tilt is relatively stable over long periods of time. However, the tilt does undergo nutation; a slight, irregular motion with a main period of 18.6 years.<ref name=lin2006/> The orientation (rather than the angle) of the 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 Moon on the Earth's equatorial bulge. From the perspective of the Earth, the poles also migrate a few meters across the 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. The rotational velocity of the Earth also varies in a phenomenon known as length of day variation.<ref name=fisher19960205/>

In modern times, Earth's perihelion occurs around January 3, and the aphelion around July 4. However, 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 results in an increase of about 6.9%<ref name=solar_energy group=note/> in solar energy reaching the Earth at perihelion relative to aphelion. Since the southern hemisphere is tilted toward the Sun at about the same time that the 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. However, 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.<ref name=williams20051230/>

Moon

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The Moon is a relatively large, terrestrial, planet-like satellite, with a diameter about one-quarter of the 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 the Earth and 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 the 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.

Because of 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.<ref name=espenak_meeus20070207/> During the Devonian period, for example, (approximately Template:Nowrap years ago) there were 400 days in a year, with each day lasting 21.8 hours.<ref name=hannu_poropudas19911216/>

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.<ref name=aaa428_261/> Some theorists believe that without this stabilization against the torques applied by the Sun and planets to the 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.<ref name=nature410_6830_773/>

Viewed from Earth, the Moon is just far enough away to have very nearly 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.<ref name=angular /> 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 the Earth's crust.<ref name=nature412_708/>

Earth has at least two co-orbital asteroids, 3753 Cruithne and 2002 AA₂₉.<ref name=whitehouse20021021/>

Habitability

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A planet that can sustain life is termed habitable, even if life did not originate there. The Earth provides the (currently understood) requisite conditions of liquid water, an environment where complex organic molecules can assemble, and sufficient energy to sustain metabolism.<ref name=ab2003/> The distance of the 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 conditions believed necessary to originate and sustain life on this planet.<ref name=dole1970/>

Biosphere

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The planet's life forms are sometimes said to form a "biosphere". This biosphere is generally believed to have begun evolving about 3.5 billion years ago. Earth is the only place where life is known to exist. 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.<ref name=amnat163_2_192/>

Natural resources and land use

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

Large deposits of fossil fuels are obtained from the Earth's crust, consisting of coal, petroleum, natural gas and methane clathrate. These deposits are used by humans both for energy production and as feedstock for chemical production. Mineral ore bodies have also been formed in Earth's crust through a process of Ore genesis, resulting from actions of erosion and plate tectonics.<ref name=mnpl_utx2006/> These bodies form concentrated sources for many metals and other useful elements.

The Earth's biosphere produces many useful biological products for humans, including (but far from limited to) 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.<ref name=science299_5607_673/> Humans also live on the land by using building materials to construct shelters. In 1993, human use of land is approximately:

The estimated amount of irrigated land in 1993 was 2,481,250 km².<ref name=cia/>

Natural and environmental hazards

Large areas of the Earth's surface are subject to extreme weather such as tropical cyclones, hurricanes, or typhoons that dominate life in those areas. Many places are subject to earthquakes, landslides, tsunamis, volcanic eruptions, tornadoes, sinkholes, blizzards, floods, droughts, 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.<ref name=un20070202/>

Human geography

Template:Main Template:See also Template:Continents navmap

Cartography, the study and practice of map making, and vicariously geography, have historically been the disciplines devoted to depicting the 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 has approximately 6,803,000,000 human inhabitants as of December 12, 2009.<ref name="World Population Clock"/> Projections indicate that the world's human population will reach seven billion in 2013 and 9.2 billion in 2050.<ref name=un2006/> 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.<ref name=prb2007/>

It is estimated that only one-eighth of the surface of the Earth is suitable for humans to live on—three-quarters is covered by oceans, and half of the land area is either desert (14%),<ref name=hessd4_439/> high mountains (27%),<ref name=biodiv/> or other less suitable terrain. The northernmost permanent settlement in the world is Alert, on Ellesmere Island in Nunavut, Canada.<ref name=cfsa2006/> (82°28′N) The southernmost is the Amundsen-Scott South Pole Station, in Antarctica, almost exactly at the South Pole. (90°S)

Independent sovereign nations claim the planet's entire land surface, except for some parts of Antarctica and the odd unclaimed area of Bir Tawil between Egypt and Sudan. As of 2007 there are 201 sovereign states, including the 192 United Nations member states. In addition, there are 59 dependent territories, and a number of autonomous areas, territories under dispute and other entities.<ref name=cia /> 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.<ref name=kennedy1989/>

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.<ref name=uncharter/> It is not, however, a world government. 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.<ref name=un_int_law/>

The first human to orbit the Earth was Yuri Gagarin on April 12, 1961.<ref name=kuhn2006/> In total, about 400 people visited outer space and reached Earth orbit as of 2004, and, of these, twelve have walked on the Moon.<ref name=ellis2004/><ref name=shayler_vis2005/><ref name=wade2008/> Normally the only humans in space are those on the International Space Station. The station's crew, currently six people, is usually replaced every six months.<ref name=nasa_rg_iss2007/> The furthest humans have travelled from Earth is 400,171 km, achieved during the 1970 Apollo 13 mission.<ref name=cramb2007/> Template:-

Cultural viewpoint

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The name "Earth" derives from the Anglo-Saxon word erda, which means ground or soil, and is related to the German word erde. It became eorthe later, and then erthe in Middle English.<ref name=randhouse2005/> The standard astronomical symbol of the Earth consists of a cross circumscribed by a circle.<ref name=liungman2004/>

Unlike the rest of the planets in the Solar System, humankind did not begin to view the Earth as a moving object in orbit around the Sun until the 16th century.<ref name=arnett20060716/> Earth has often been personified as a deity, in particular a goddess. In many cultures the mother goddess is also portrayed as a fertility deity. Creation myths in many religions recall a story involving the creation of the Earth by a supernatural deity or deities. A variety of religious groups, often associated with fundamentalist branches of Protestantism<ref name=Dutch2002/> or Islam,<ref name=edis2003/> 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 the Earth and the origin and development of life.<ref name=jge53_3_319/> Such assertions are opposed by the scientific community<ref name=arghg4_143/><ref name=sec_nap2008/> and by other religious groups.<ref name=jrst43_4_419/><ref name=frye1983/><ref name=nathist106_2_16/> A prominent example is the creation-evolution controversy.

In the past there were varying levels of belief in a flat Earth,<ref name=russell1997/> but this was displaced by the concept of a spherical Earth due to observation and circumnavigation.<ref name=jacobs19980201/> The human perspective regarding the Earth has changed following the advent of spaceflight, and the biosphere is now widely viewed from a globally integrated perspective.<ref name=fuller1963/><ref name=lovelock1979/> This is reflected in a growing environmental movement that is concerned about humankind's effects on the planet.<ref name=mcmichael1993/>

See also

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• Geodesy
• Geology

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Notes

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References

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Further reading

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External links

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• USGS Geomagnetism Program
• NASA Earth Observatory
• Audio—Cain/Gay (2007) Astronomy Cast Earth
• Earth Profile by NASA's Solar System Exploration
• Climate changes cause Earth's shape to change – NASA
• The Gateway to Astronaut Photography of Earth
• Global Measured Extremes of Temperature and Precipitation National Climatic Data Center

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