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Further information: Seawater
Surface of the Atlantic Ocean meeting the Earth's planetary boundary layer and troposphere.

Template:Five oceans

An ocean (Template:Etymology, the sea of classical antiquity[1]) is a body of saline water that composes much of a planet's hydrosphere.[2] On Earth, an ocean is one of the major conventional divisions of the World Ocean, which occupies two-thirds of the planet's surface. These are, in descending order by area, the Pacific, Atlantic, Indian, Southern, and Arctic Oceans.[3][4] The word sea is often used interchangeably with "ocean" in American English but, strictly speaking, a sea is a body of saline water (generally a division of the world ocean) partly or fully enclosed by land.[5]

Saline water covers approximately 72% of the planet's surface (~3.6×108 km2) and is customarily divided into several principal oceans and smaller seas, with the ocean covering approximately 71% of the Earth's surface.[6] The ocean contains 97% of the Earth's water, and oceanographers have stated that only 5% of the World Ocean has been explored.[6] The total volume is approximately 1.3 billion cubic kilometers (310 million cu mi)[7] with an average depth of 3,682 meters (12,080 ft).[8]

Because it is the principal component of Earth's hydrosphere, the world ocean is integral to all known life, forms part of the carbon cycle, and influences climate and weather patterns. It is the habitat of 230,000 known species, although much of the oceans depths remain unexplored, and over two million marine species are estimated to exist.[9] The origin of Earth's oceans remains unknown; oceans are believed to have formed in the Hadean period and may have been the impetus for the emergence of life.

Extraterrestrial oceans may be composed of water or other elements and compounds. The only confirmed large stable bodies of extraterrestrial surface liquids are the lakes of Titan, although there is evidence for the existence of oceans elsewhere in the Solar System. Early in their geologic histories, Mars and Venus are theorized to have had large water oceans. The Mars ocean hypothesis suggests that nearly a third of the surface of Mars was once covered by water, and a runaway greenhouse effect may have boiled away the global ocean of Venus. Compounds such as salts and ammonia dissolved in water lower its freezing point, so that water might exist in large quantities in extraterrestrial environments as brine or convecting ice. Unconfirmed oceans are speculated beneath the surface of many dwarf planets and natural satellites; notably, the ocean of Europa is believed to have over twice the water volume of Earth. The Solar System's gas giant planets are also believed to possess liquid atmospheric layers of yet to be confirmed compositions. Oceans may also exist on exoplanets and exomoons, including surface oceans of liquid water within a circumstellar habitable zone. Ocean planets are a hypothetical type of planet with a surface completely covered with liquid.[10][11]

Earth's global ocean

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Global divisions

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Further information: Borders of the oceans
Rotating series of maps showing alternate divisions of the oceans
Various ways to divide the World Ocean

Though generally described as several separate oceans, these waters comprise one global, interconnected body of salt water sometimes referred to as the World Ocean or global ocean.[12][13] This concept of a continuous body of water with relatively free interchange among its parts is of fundamental importance to oceanography.[14]

The major oceanic divisions are defined in part by the continents, various archipelagos, and other criteria. See the table below for more information; note that the table is in descending order in terms of size.[11][15]

Rank Ocean Notes
1 Pacific The peaceful sea west of the Magellan Strait,[16] officially separated into the North and South Pacific (divided by the Equator[17] and containing the waters between the southernmost points of Tasmania and Terra del Fuego (and including the waters of the Magellan Strait) but limited by the borders of the Tasman, Coral, Solomon, and Bismark Seas, the East Indian Archipelago, the Philippine, Japan, Okhotsk, and Bering Seas, the Gulf of Alaska, the coastal waters of southeast Alaska and British Columbia, and the Gulf of California.[18]
2 Atlantic The sea beyond the Atlas Mountains,[19][20] officially separated into the North and South Atlantic (divided by the Equator) and containing the waters between the southernmost points of Tierra del Fuego and Africa but limited by the borders of the Rio de la Plata, the Caribbean Sea, the Gulf of Mexico, the Bay of Fundy, the Gulf of St. Lawrence, the Davis Strait, the Greenland, Norwegian, North, Scottish, and Irish Seas, the Bristol and English Channels, the Bay of Biscay, the Mediterranean Sea, and the Gulf of Guinea,[18] although now often considered to end north of the Antarctic Convergence.
3 Indian The sea south of India, officially containing the waters between the southernmost points of Africa and Tasmania, bounded on the north by the Arabian and Laccadive Seas, the Bay of Bengal, the East Indian Archipelago, and the Great Australian Bight and on the south by Antarctica,[18] although now often considered to end north of the Antarctic Convergence.
4 Southern
or
Antarctic		 Still officially considered an extension of the Pacific, Atlantic and Indian Oceans by the IHO,[11][18] it is distinguished by the convergence which encircles Antarctica.
5 Arctic The sea around the North Pole, officially containing the waters north of the Greenland Sea, then a line east along 80°N to the Barentsz, Kara, Laptev, East Siberian, Chuckchi, and Beaufort Seas.[18] Sometimes[when?] itself considered[by whom?] a sea of the Atlantic.

These adjacent regions—whether seas, gulfs, bays, bights, or straits—are very often included as part of the nearest ocean.

Physical properties

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Further information: Seawater

The total mass of the hydrosphere is about 1,400,000,000,000,000,000 metric tons (1.5×1018 short tons) or 1.4×1021 kg, which is about 0.023 percent of the Earth's total mass. Less than 3 percent is freshwater; the rest is saltwater, mostly in the ocean. The area of the World Ocean is 361 million square kilometers (139 million square miles),[21] and its volume is approximately 1.3 billion cubic kilometers (310 million cu mi).[7] This can be thought of as a cube of water with an edge length of 1,111 kilometers (690 mi). Its average depth is 3,790 meters (12,430 ft), and its maximum depth is 10,923 meters (6.787 mi).[21] Nearly half of the world's marine waters are over 3,000 meters (9,800 ft) deep.[13] The vast expanses of deep ocean (anything below 200 meters (660 ft)) cover about 66% of the Earth's surface.[22] This does not include seas not connected to the World Ocean, such as the Caspian Sea.

The bluish color of water is a composite of several contributing agents. Prominent contributors include dissolved organic matter and chlorophyll.[23]

Sailors and other mariners have reported that the ocean often emits a visible glow, or luminescence, which extends for miles at night. In 2005, scientists announced that for the first time, they had obtained photographic evidence of this glow.[24] It is most likely caused by bioluminescence.[25][26][27]

Zones with depth

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Drawing showing divisions according to depth and distance from shore
The major oceanic divisions

Oceanographers divide the ocean into different zones by physical and biological conditions. The pelagic zone includes all open ocean regions, and can be divided into further regions categorized by depth and light abundance. The photic zone includes the oceans from the surface to a depth of 200 m; it is the region where photosynthesis can occur and is, therefore, the most biodiverse. Since plants require photosynthesis, life found deeper than the photic zone must either rely on material sinking from above (see marine snow) or find another energy source. Hydrothermal vents are the primary source of energy in what is known as the aphotic zone (depths exceeding 200 m). The pelagic part of the photic zone is known as the epipelagic.

The pelagic part of the aphotic zone can be further divided into vertical regions according to temperature. The mesopelagic is the uppermost region. Its lowermost boundary is at a thermocline of 12 °C (54 °F), which, in the tropics generally lies at 700–1,000 meters (2,300–3,300 ft). Next is the bathypelagic lying between 10 and 4 °C (50 and 39 °F), typically between 700–1,000 meters (2,300–3,300 ft) and 2,000–4,000 meters (6,600–13,100 ft) Lying along the top of the abyssal plain is the abyssopelagic, whose lower boundary lies at about 6,000 meters (20,000 ft). The last zone includes the deep oceanic trench, and is known as the hadalpelagic. This lies between 6,000–11,000 meters (20,000–36,000 ft) and is the deepest oceanic zone.

The benthic zones are aphotic and correspond to the three deepest zones of the deep-sea. The bathyal zone covers the continental slope down to about 4,000 meters (13,000 ft). The abyssal zone covers the abyssal plains between 4,000 and 6,000 m. Lastly, the hadal zone corresponds to the hadalpelagic zone, which is found in oceanic trenches.

The pelagic zone can be further subdivided into two subregions: the neritic zone and the oceanic zone. The neritic zone encompasses the water mass directly above the continental shelves whereas the oceanic zone includes all the completely open water.

In contrast, the littoral zone covers the region between low and high tide and represents the transitional area between marine and terrestrial conditions. It is also known as the intertidal zone because it is the area where tide level affects the conditions of the region.

The ocean can be divided into three density zones: the surface zone, the pycnocline, and the deep zone. The surface zone, also called the mixed layer, refers to the uppermost density zone of the ocean. Temperature and salinity are relatively constant with depth in this zone due to currents and wave action. The surface zone contains ocean water that is in contact with the atmosphere and within the photic zone. The surface zone has the ocean's least dense water and represents approximately 2% of the total volume of ocean water. The surface zone usually ranges between depths of 500 feet to 3,300 feet below ocean surface, but this can vary a great deal. In some cases, the surface zone can be entirely non-existent. The surface zone is typically thicker in the tropics than in regions of higher latitude. The transition to colder, denser water is more abrupt in the tropics than in regions of higher latitudes. The pycnocline refers to a zone wherein density substantially increases with depth due primarily to decreases in temperature. The pycnocline effectively separates the lower-density surface zone above from the higher-density deep zone below. The pycnocline represents approximately 18% of the total volume of ocean water. The deep zone refers to the lowermost density zone of the ocean. The deep zone usually begins at depths below 3,300 feet in mid-latitudes. The deep zone undergoes negligible changes in water density with depth. The deep zone represents approximately 80% of the total volume of ocean water. The deep zone contains relatively colder and stable water.

If a zone undergoes dramatic changes in temperature with depth, it contains a thermocline. The tropical thermocline is typically deeper than the thermocline at higher latitudes. Polar waters, which receive relatively little solar energy, are not stratified by temperature and generally lack a thermocline since surface water at polar latitudes are nearly as cold as water at greater depths. Below the thermocline, water is very cold, ranging from −1 °C to 3 °C. Since this deep and cold layer contains the bulk of ocean water, the average temperature of the world ocean is 3.9 °C If a zone undergoes dramatic changes in salinity with depth, it contains a halocline. If a zone undergoes a strong, vertical chemistry gradient with depth, it contains a chemocline.

The halocline often coincides with the thermocline, and the combination produces a pronounced pycnocline.

Exploration

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False color photo
Map of large underwater features (1995, NOAA)

Ocean travel by boat dates back to prehistoric times, but only in modern times has extensive underwater travel become possible.

The deepest point in the ocean is the Mariana Trench, located in the Pacific Ocean near the Northern Mariana Islands. Its maximum depth has been estimated to be 10,971 meters (35,994 ft) (plus or minus 11 meters; see the Mariana Trench article for discussion of the various estimates of the maximum depth.) The British naval vessel Challenger II surveyed the trench in 1951 and named the deepest part of the trench the "Challenger Deep". In 1960, the Trieste successfully reached the bottom of the trench, manned by a crew of two men.

Climate

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World map with colored, directed lines showing how water moves through the oceans. Cold deep water rises and warms in the central Pacific and in the Indian, while warm water sinks and cools near Greenland in the North Atlantic and near Antarctica in the South Atlantic.
A map of the global thermohaline circulation; blue represent deep-water currents, while red represent surface currents

Ocean currents greatly affect the Earth's climate by transferring heat from the tropics to the polar regions. Transferring warm or cold air and precipitation to coastal regions, where winds may carry them inland. Surface heat and freshwater fluxes create global density gradients that drive the thermohaline circulation part of large-scale ocean circulation. It plays an important role in supplying heat to the polar regions, and thus in sea ice regulation. Changes in the thermohaline circulation are thought to have significant impacts on the Earth's radiation budget. In so far as the thermohaline circulation governs the rate at which deep waters reach the surface, it may also significantly influence atmospheric carbon dioxide concentrations.

For a discussion of the possibilities of changes to the thermohaline circulation under global warming, see shutdown of thermohaline circulation.

It is often stated that the thermohaline circulation is the primary reason that the climate of Western Europe is so temperate. An alternate hypothesis claims that this is largely incorrect, and that Europe is warm mostly because it lies downwind of an ocean basin, and because atmospheric waves bring warm air north from the subtropics.[28][29]

The Antarctic Circumpolar Current encircles that continent, influencing the area's climate and connecting currents in several oceans.

One of the most dramatic forms of weather occurs over the oceans: tropical cyclones (also called "typhoons" and "hurricanes" depending upon where the system forms).

Biology

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Further information: Marine biology

The ocean has a significant effect on the biosphere. Oceanic evaporation, as a phase of the water cycle, is the source of most rainfall, and ocean temperatures determine climate and wind patterns that affect life on land. Life within the ocean evolved 3 billion years prior to life on land. Both the depth and the distance from shore strongly influence the biodiversity of the plants and animals present in each region.[30]

Lifeforms native to the ocean include:

In addition, many land animals have adapted to living a major part of their life on the oceans. For instance, seabirds are a diverse group of birds that have adapted to a life mainly on the oceans. They feed on marine animals and spend most of their lifetime on water, many only going on land for breeding. Other birds that have adapted to oceans as their living space are penguins, seagulls and pelicans. Seven species of turtles, the sea turtles, also spend most of their time in the oceans.

Gases

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Characteristics of Oceanic Gases [31][32][33]
Gas Concentration of Seawater, by Mass (in parts per million), for whole Ocean % Dissolved Gas, by Volume, in Seawater at Ocean Surface
Carbon dioxide (CO2) 64 to 107 15%
Nitrogen (N2) 10 to 18 48%
Oxygen (O2) 0 to 13 36%
Solubility of Oceanic Gases (in terms of mL/L) with Temperature at salinity of 33‰ and atmospheric pressure[34]
Temperature O2 CO2 N2
0 °C 8.14 8,700 14.47
10 °C 6.42 8,030 11.59
20 °C 5.26 7,350 9.65
30 °C 4.41 6,600 8.26

Ocean Surface

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Generalized Characteristics of Ocean Surface by Latitude [35][36][37][38][39][40][41]
Characteristic Oceanic Waters in Polar regions Oceanic Waters in Temperate regions Oceanic Waters in Tropical regions
Precipitation vs. evaporation P > E P > E E > P
Sea Surface Temperature in Winter −2 °C 5 to 20 °C 20 to 25 °C
Average Salinity 28‰ to 32‰ 35‰ 35‰ to 37‰
Annual Variation of Air Temperature ≤ 40ªC 10 °C < 5 °C
Annual Variation of Water Temperature < 5ªC 10 °C < 5 °C

Mixing Time

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Residence Time=The amount of the element in the ocean ÷ The rate at which that element is added to (or removed from) the ocean

The mean oceanic mixing time (residence time) is thought to be approximately 1,600 years. If a given element in the ocean stays in the ocean, on average, longer than the oceanic mixing time, then that element is assumed to be homogeneously spread throughout the ocean. As a result, since the major salts have a residence time that is longer than 1,600 years, the ratio of major salts is thought to be unchanging across the ocean. This constant ratio is often referred to as Forchhammer's principle or the principle of constant proportions.

Mean Oceanic Residence Times for specific Constituents [42][43]
Constituent Residence Time (in years)
Iron (Fe) 200
Aluminum (Al) 600
Manganese (Mn) 1,300
Water (H2O) 4,100
Silicon (Si) 20,000
Carbonate (CO32−) 110,000
Calcium (Ca2+) 1,000,000
Sulfate (SO42−) 11,000,000
Potassium (K+) 12,000,000
Magnesium (Mg2+) 13,000,000
Sodium (Na+) 68,000,000
Chloride (Cl−) 100,000,000

Salinity

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A zone of rapid salinity increase with depth is called a halocline. The temperature of maximum density of seawater decreases as its salt content increases. Freezing temperature of water decreases with salinity, and boiling temperature of water increases with salinity. Typical seawater freezes at around −1.9 °C at atmospheric pressure. If precipitation exceeds evaporation, as is the case in polar and temperate regions, salinity will be lower. If evaporation exceeds precipitation, as is the case in tropical regions, salinity will be higher. Thus, oceanic waters in polar regions have lower salinity content than oceanic waters in temperate and tropical regions.[44]

Salinity can be calculated using the chlorinity, which is a measure of the total mass of halogen ions (includes fluorine, chlorine, bromine, and iodine) in seawater. By international agreement, the following formula is used to determine salinity:

Salinity (in ‰)=1.80655 x Chlorinity (in ‰)

The average chlorinity is about 19.2‰, and, thus, the average salinity is around 34.7‰ [44]

Absorption of light

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Absorption of Light in Different Wavelengths by Ocean [44]
Color: Wavelength (nm) Depth wherein 99 percent of wavelength is absorbed (in meters) Percent absorbed in 1 meter of water
Ultraviolet (UV): 310 31 14.0
Violet (V): 400 107 4.2
Blue (B): 475 254 1.8
Green (G): 525 113 4.0
Yellow (Y): 575 51 8.7
Orange (O): 600 25 16.7
Red (R): 725 4 71.0
Infrared (IR): 800 3 82.0

Economic value

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The oceans are essential to transportation. This is because most of the world's goods move by ship between the world's seaports. Oceans are also the major supply source for the fishing industry. Some of the more major ones are shrimp, fish, crabs, and lobster.[6]

Waves

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Further information: Wind wave

The motions of the ocean surface, known as undulations or waves, are the partial and alternate rising and falling of the ocean surface.

Extraterrestrial oceans

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Further information: Extraterrestrial liquid water
Artist's conception of subsurface ocean of Enceladus confirmed April 3, 2014.[45][46]
Two models for the composition of Europa predict a large subsurface ocean of liquid water. Similar models have been proposed for other celestial bodies in the Solar System

Although Earth is the only known planet with large stable bodies of liquid water on its surface and the only one in the Solar System, other celestial bodies are believed to possess large oceans.

Planets

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The gas giants, Jupiter and Saturn, are thought to lack surfaces and instead have a stratum of liquid hydrogen, however their planetary geology is not well understood. The possibility of Uranus and Neptune possessing hot, highly compressed, supercritical water under their thick atmospheres has been hypothesised. Although their composition is still not fully understood, a 2006 study by Wiktorowicz et al. ruled out the possibility of such a water "ocean" existing on Neptune,[47] though some studies have suggested that exotic oceans of liquid diamond are possible.[48]

The Mars ocean hypothesis suggests that nearly a third of the surface of Mars was once covered by water, though the water on Mars is no longer oceanic. The possibility continues to be studied along with reasons for their apparent disappearance. Astronomers believe that Venus had liquid water and perhaps oceans in its very early history. If they existed, all later vanished via resurfacing.

Natural satellites

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A global layer of liquid water thick enough to decouple the crust from the mantle is believed to be present on Titan, Europa and, with less certainty, Callisto, Ganymede[49][50] and Triton.[51][52] A magma ocean is thought to be present on Io. Geysers have been found on Saturn's moon Enceladus, possibly originating from about 10 kilometers (6.2 mi) deep ocean beneath an ice shell.[45] Other icy moons may also have internal oceans, or may once have had internal oceans that have now frozen.[53]

Large bodies of liquid hydrocarbons are thought to be present on the surface of Titan, although they are not large enough to be considered oceans and are sometimes referred to as lakes or seas. The Cassini–Huygens space mission initially discovered only what appeared to be dry lakebeds and empty river channels, suggesting that Titan had lost what surface liquids it might have had. Cassini's more recent fly-by of Titan offers radar images that strongly suggest hydrocarbon lakes exist near the colder polar regions. Titan is thought to have a subsurface liquid-water ocean under the ice and hydrocarbon mix that forms its outer crust.

Dwarf planets and trans-Neptunian objects

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Diagram showing a possible internal structure of Ceres

Ceres appears to be differentiated into a rocky core and icy mantle and may harbour a liquid-water ocean under its surface.[54][55]

Not enough is known of the larger Trans-Neptunian objects to determine whether they are differentiated bodies capable of possessing oceans, although models of radioactive decay suggest that Pluto,[56] Eris, Sedna, and Orcus have oceans beneath solid icy crusts at the core-boundary approximately 100 to 180 km thick.[53]

Extrasolar

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Rendering of a hypothetical large extrasolar moon with surface liquid-water oceans

Some planets and natural satellites beyond the Solar System are likely to possess oceans, including possible water ocean planets similar to Earth in the habitable zone or "liquid-water belt". The detection of oceans, even through the spectroscopy method, however is likely to prove extremely difficult and inconclusive.

Theoretical models have been used to predict with high probability that GJ 1214 b, detected by transit, is composed of exotic form of ice VII, making up 75% of its mass,[57] making it an ocean planet.

Other possible candidates are merely speculated based on their mass and position in the habitable zone include planet though little is actually known of their composition. Some scientists speculate Kepler-22b may be an "ocean-like" planet.[58] Models have been proposed for Gliese 581 d that could include surface oceans. Gliese 436 b is speculated to have an ocean of "hot ice".[59] Extrasolar moons orbiting planets, particularly gas giants within their parent star's habitable zone may theoretically possess surface oceans.

Terrestrial planets will acquire water during their accretion, some of which will be buried in the magma ocean but most of it will go into a steam atmosphere, and when the atmosphere cools it will collapse on to the surface forming an ocean. There will also be outgassing of water from the mantle as the magma solidifies—this will happen even for planets with a low percentage of their mass composed of water, so "super-Earth exoplanets may be expected to commonly produce water oceans within tens to hundreds of millions of years of their last major accretionary impact."[60]

Non-water surface liquids

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Oceans, seas, lakes, etc., can be composed of liquids other than water: e.g. the hydrocarbon lakes on Titan. The possibility of seas of nitrogen on Triton was also considered but ruled out.[61] Underneath the thick atmospheres of the planets Uranus and Neptune, it is expected that these planets are composed of oceans of hot high-density fluid mixtures of water, ammonia and other volatiles.[62] The gaseous outer layers of Jupiter and Saturn transition smoothly into oceans of supercritical hydrogen.[63][64] There is evidence that the icy surfaces of the moons Ganymede, Callisto, Europa, Titan and Enceladus are shells floating on oceans of very dense liquid water or water–ammonia.[65][66][67][68][69] Earth is often called the ocean planet because it is 70% covered in water.[70][71] The atmosphere of Venus is 96.5% carbon dioxide and at the surface the pressure makes the CO2 a supercritical fluid. Extrasolar terrestrial planets that are extremely close to their parent star will be tidally locked and so one half of the planet will be a magma ocean.[72] It is also possible that terrestrial planets had magma oceans at some point during their formation as a result of giant impacts.[73] Where there are suitable temperatures and pressures, volatile chemicals that might exist as liquids in abundant quantities on planets include ammonia, argon, carbon disulfide, ethane, hydrazine, hydrogen, hydrogen cyanide, hydrogen sulfide, methane, neon, nitrogen, nitric oxide, phosphine, silane, sulfuric acid, and water.[74] Hot Neptunes close to their star could lose their atmospheres via hydrodynamic escape, leaving behind their cores with various liquids on the surface.[75]

See also

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  • [[Archivo:
  1. REDIRECCIÓN Plantilla:Iconos|20px|Ver el portal sobre Ecology]] Portal:Ecology. Contenido relacionado con Environment.

Template:Colbegin

On other bodies:

Template:Colend

References

[edit]
  1. ^ "Ὠκεανός". Perseus Digital Library. Retrieved May 17, 2012.
  2. ^ "WordNet Search — ocean". Princeton University. Retrieved February 21, 2012.
  3. ^ "ocean, n". Oxford English Dictionary. Retrieved February 5, 2012.
  4. ^ "ocean". Merriam-Webster. Retrieved February 6, 2012.
  5. ^ "WordNet Search — sea". Princeton University. Retrieved February 21, 2012.
  6. ^ a b c "NOAA – National Oceanic and Atmospheric Administration – Ocean". Noaa.gov. Retrieved 8-11-2012. {{cite web}}: Check date values in: |accessdate= (help)
  7. ^ a b Qadri, Syed (2003). "Volume of Earth's Oceans". The Physics Factbook. Retrieved 2007-06-07.
  8. ^ Charette, Matthew; Smith, Walter H. F. (2010). "The volume of Earth's ocean". Oceanography. 23 (2): 112–114. doi:10.5670/oceanog.2010.51. Retrieved 27 September 2012.
  9. ^ Drogin, Bob (August 2, 2009). "Mapping an ocean of species". Los Angeles Times. Retrieved August 18, 2009.
  10. ^ "Titan Likely To Have Huge Underground Ocean | Mind Blowing Science". Mindblowingscience.com. Retrieved 8-11-2012. {{cite web}}: Check date values in: |accessdate= (help)
  11. ^ a b c "Ocean-bearing Planets: Looking For Extraterrestrial Life In All The Right Places". Sciencedaily.com. Retrieved 8-11-2012. {{cite web}}: Check date values in: |accessdate= (help)
  12. ^ "Ocean". Sciencedaily.com. Retrieved 8-11-2012. {{cite web}}: Check date values in: |accessdate= (help)
  13. ^ a b ""Distribution of land and water on the planet". UN Atlas of the Oceans. {{cite web}}: External link in |work= (help)
  14. ^ Spilhaus, Athelstan F. (July 1942). "Maps of the whole world ocean". 32 (3). American Geographical Society: 431–5. {{cite journal}}: Cite journal requires |journal= (help)
  15. ^ "Pacific Ocean – University of Delaware". Ceoe.udel.edu. Retrieved 8-11-2012. {{cite web}}: Check date values in: |accessdate= (help)
  16. ^ Oxford English Dictionary, 3rd ed. "Pacific, adj.2 and n.2" Oxford University Press (Oxford), 2005.
  17. ^ Apart from the Galapagos and Gilbert Islands, whose surroundings waters are formally included in the South Pacific, even where they lie north of the Equator.
  18. ^ a b c d e "Limits of Oceans and Seas" (PDF) (3rd ed.). International Hydrographic Organization. 1953. Retrieved 7 February 2010.
  19. ^ Oxford English Dictionary, 1st ed. "Atlantic, adj. and n." Oxford University Press (Oxford), 1885.
  20. ^ Herodotus. Ἱστορίαι [The Histories], I.202. c. 420 BC. (in Ancient Greek)
  21. ^ a b The World's Oceans and Seas. Encarta.
  22. ^ Drazen, Jeffrey C. "Deep-Sea Fishes". School of Ocean and Earth Science and Technology, the University of Hawaiʻi at Mānoa. Retrieved 2007-06-07.
  23. ^ Coble, Paula G. (2007). "Marine Optical Biogeochemistry:  The Chemistry of Ocean Color". Chemical Reviews. 107: 402–418. doi:10.1021/cr050350.
  24. ^ Britt, Robert Roy (October 4, 2005). "Mystery Ocean Glow Confirmed in Satellite Photos".
  25. ^ Holladay, April (November 21, 2005). "A glowing sea, courtesy of algae". USA Today.
  26. ^ "Sea's eerie glow seen from space". New Scientist. October 5, 2005.
  27. ^ Casey, Amy (August 8, 2003). "The Incredible Glowing Algae". NASA Earth Observatory. NASA.
  28. ^ doi:10.1511/2006.60.999
    This citation will be automatically completed in the next few minutes. You can jump the queue or expand by hand
  29. ^ Rhines; Hakkinen (2003). "Is the Oceanic Heat Transport in the North Atlantic Irrelevant to the Climate in Europe?" (PDF). ASOF Newsletter.
  30. ^ "Chapter 34: The Biosphere: An Introduction to Earth's Diverse Environment". Biology: Concepts & Connections. section 34.7.
  31. ^ "Dissolved Gases other than Carbon Dioxide in Seawater" (PPT). soest.hawaii.edu. Retrieved 2014-05-05.
  32. ^ "Dissolved Oxygen and Carbon Dioxide" (PDF). chem.uiuc.edu.
  33. ^ Anthoni, Floor. "Composition of seawater". Seafriends.org.nz. Retrieved 2014-05-05.
  34. ^ "12.742. Marine Chemistry. Lecture 8. Dissolved Gases and Air-sea exchange" (PDF). Retrieved 2014-05-05.
  35. ^ "5.6 Synthesis – AR4 WGI Chapter 5: Observations: Oceanic Climate Change and Sea Level". Ipcc.ch. Retrieved 2014-05-05.
  36. ^ Lua error in package.lua at line 80: module 'Module:Citation/CS1/Suggestions' not found.
  37. ^ Barry, Roger Graham; Chorley, Richard J. (2003). "Atmosphere, Weather, and Climate". [Routledge]. p. 68. {{cite web}}: Missing or empty |url= (help)
  38. ^ "Ocean Stratification". Eesc.columbia.edu. Retrieved 2014-05-05.
  39. ^ Huang, Rui Xin (2010). "Ocean Circulation: Wind-Driven and Thermohaline Processes". [Cambridge University Press]. {{cite web}}: Missing or empty |url= (help)
  40. ^ doi:10.1146/annurev-marine-120408-151453
    This citation will be automatically completed in the next few minutes. You can jump the queue or expand by hand
  41. ^ "Chapter 6 – Temperature, Salinity, and Density – Geographical Distribution of Surface Temperature and Salinity". Introduction to Physical Oceanography :. Oceanworld.tamu.edu. 2009-03-23. Retrieved 2014-05-05.{{cite web}}: CS1 maint: extra punctuation (link)
  42. ^ "Calculation of residence times in seawater of some important solutes" (PDF). gly.uga.edu.
  43. ^ Chester, Roy; Jickells, Tim (2012). Marine Geochemistry. Blackwell Publishing. pp. 225–230. ISBN 978-1-118-34907-6.
  44. ^ a b c Chester, Roy; Jickells, Tim (2012). Marine Geochemistry. Blackwell Publishing. ISBN 978-1-118-34907-6.
  45. ^ a b Platt, Jane; Bell, Brian (2014-04-03). "NASA Space Assets Detect Ocean inside Saturn Moon". NASA. Retrieved 2014-04-03.
  46. ^ Iess, L.; Stevenson, D.J.; Parisi, M.; Hemingway, D.; et al. (4 April 2014). "The Gravity Field and Interior Structure of Enceladus". Science. 344 (6179): 78–80. doi:10.1126/science.1250551. Retrieved 3 April 2014.
  47. ^ Wiktorowicz, Sloane J.; Ingersoll, Andrew P. (2007). "Liquid water oceans in ice giants". Icarus. 186 (2): 436–447. arXiv:astro-ph/0609723. Bibcode:2007Icar..186..436W. doi:10.1016/j.icarus.2006.09.003. ISSN 0019-1035.
  48. ^ Silvera, Isaac (2010). "Diamond: Molten under pressure". Nature Physics. 6 (1): 9–10. Bibcode:2010NatPh...6....9S. doi:10.1038/nphys1491. ISSN 1745-2473.
  49. ^ Clavin, Whitney (May 1, 2014). "Ganymede May Harbor 'Club Sandwich' of Oceans and Ice". NASA. Jet Propulsion Laboratory. Retrieved 2014-05-01.
  50. ^ Vance, Steve; Bouffard, Mathieu; Choukroun, Mathieu; Sotina, Christophe (12 April 2014). "Ganymede's internal structure including thermodynamics of magnesium sulfate oceans in contact with ice". Planetary and Space Science. Bibcode:2014P&SS...96...62V. doi:10.1016/j.pss.2014.03.011. Retrieved 2014-05-02.
  51. ^ McKinnon, William B.; Kirk, Randolph L. (2007). "Triton". In Lucy Ann Adams McFadden; Lucy-Ann Adams; Paul Robert Weissman; Torrence V. Johnson (eds.). Encyclopedia of the Solar System (2nd ed.). Amsterdam; Boston: Academic Press. pp. 483–502. ISBN 978-0-12-088589-3. {{cite encyclopedia}}: Invalid |display-editors=4 (help)
  52. ^ Ruiz, Javier (December 2003). "Heat flow and depth to a possible internal ocean on Triton". Icarus. 166 (2): 436–439. Bibcode:2003Icar..166..436R. doi:10.1016/j.icarus.2003.09.009.
  53. ^ a b doi: 10.1016/j.icarus.2006.06.005
    This citation will be automatically completed in the next few minutes. You can jump the queue or expand by hand
  54. ^ McCord, Thomas B. (2005). "Ceres: Evolution and current state". Journal of Geophysical Research. 110 (E5): E05009. Bibcode:2005JGRE..11005009M. doi:10.1029/2004JE002244.
  55. ^ Castillo-Rogez, J. C.; McCord, T. B.; Davis, A. G. (2007). "Ceres: evolution and present state" (PDF). Lunar and Planetary Science. XXXVIII: 2006–2007. Retrieved 2009-06-25.
  56. ^ "The Inside Story". pluto.jhuapl.edu — NASA New Horizons mission site. Johns Hopkins University Applied Physics Laboratory. 2013. Retrieved 2 August 2013.
  57. ^ Aguilar, David A. (2009-12-16). "Astronomers Find Super-Earth Using Amateur, Off-the-Shelf Technology". Harvard-Smithsonian Center for Astrophysics. Retrieved January 23, 2010.
  58. ^ Mendez Torres, Abel (2011-12-08). "Updates on Exoplanets during the First Kepler Science Conference". Planetary Habitability Laboratory at UPR Arecibo.
  59. ^ Fox, Maggie (May 16, 2007). "Hot "ice" may cover recently discovered planet". Reuters. Retrieved May 18, 2012.
  60. ^ Elkins-Tanton (2010). "Formation of Early Water Oceans on Rocky Planets". Astrophysics and Space Science. 332 (2): 359–364. arXiv:1011.2710. Bibcode:2011Ap&SS.332..359E. doi:10.1007/s10509-010-0535-3.
  61. ^ McKinnon, William B.; Kirk, Randolph L. (2007). "Triton". In Lucy Ann Adams McFadden; Lucy-Ann Adams; Paul Robert Weissman; Torrence V. Johnson (eds.). Encyclopedia of the Solar System (2nd ed.). Amsterdam; Boston: Academic Press. p. 485. ISBN 978-0-12-088589-3. {{cite encyclopedia}}: Invalid |display-editors=4 (help)
  62. ^ Atreya, S.; Egeler, P.; Baines, K. (2006). "Water-ammonia ionic ocean on Uranus and Neptune?" (PDF). Geophysical Research Abstracts. 8: 05179. Bibcode:2005AGUFM.P11A0088A.
  63. ^ Guillot, T. (1999). "A comparison of the interiors of Jupiter and Saturn". Planetary and Space Science. 47 (10–11): 1183–200. arXiv:astro-ph/9907402. Bibcode:1999P&SS...47.1183G. doi:10.1016/S0032-0633(99)00043-4.
  64. ^ Lang, Kenneth R. (2003). "Jupiter: a giant primitive planet". NASA. Retrieved 2007-01-10.
  65. ^ Coustenis, A.; Lunine, J.; Lebreton, J.; Matson, D.; et al. (2008). "American Geophysical Union, Fall Meeting 2008, abstract #P21A-1346". American Geophysical Union. 21: 1346. Bibcode:2008AGUFM.P21A1346C. the Titan system, rich in organics, containing a vast subsurface ocean of liquid water {{cite journal}}: |contribution= ignored (help)
  66. ^ Nimmo, F.; Bills, B. G. (2010). "Shell thickness variations and the long-wavelength topography of Titan". Icarus. 208 (2): 896–904. Bibcode:2010Icar..208..896N. doi:10.1016/j.icarus.2010.02.020. observations can be explained if Titan has a floating, isostatically-compensated ice shell
  67. ^ Goldreich, Peter M.; Mitchell, Jonathan L. (2010). "Elastic ice shells of synchronous moons: Implications for cracks on Europa and non-synchronous rotation of Titan". Icarus. 209 (2): 631–638. arXiv:0910.0032. Bibcode:2010Icar..209..631G. doi:10.1016/j.icarus.2010.04.013. A number of synchronous moons are thought to harbor water oceans beneath their outer ice shells. A subsurface ocean frictionally decouples the shell from the interior
  68. ^ "Study of the ice shells and possible subsurface oceans of the Galilean satellites using laser altimeters on board the Europa and Ganymede orbiters JEO and JGO" (PDF). Retrieved 2011-10-14.
  69. ^ "Tidal heating and the long-term stability of a subsurface ocean on Enceladus" (PDF). Retrieved 2011-10-14.
  70. ^ "The ocean planet". Ncbi.nlm.nih.gov. 2011-10-03. Retrieved 2011-10-14.
  71. ^ "Irrigating Crops with Seawater". Scientific American. August 1998.
  72. ^ Schaefer, Laura; Fegley, Bruce, Jr. (2009). "Chemistry of Silicate Atmospheres of Evaporating Super-Earths". The Astrophysical Journal Letters. 703 (2): L113–L117. arXiv:0906.1204. Bibcode:2009ApJ...703L.113S. doi:10.1088/0004-637X/703/2/L113.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  73. ^ Solomatov, V. S. (2000). "Fluid Dynamics of a Terrestrial Magma Ocean" (PDF).
  74. ^ Tables 3 and 4 in Bains, William (2004). "Many Chemistries Could Be Used to Build Living Systems" (PDF). Astrobiology.
  75. ^ Lua error in package.lua at line 80: module 'Module:Citation/CS1/Suggestions' not found.

Further reading

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  • Matthias Tomczak and J. Stuart Godfrey. 2003. Regional Oceanography: an Introduction. (see the site)
  • Pope, F. 2009. From eternal darkness springs cast of angels and jellied jewels. in The Times. November 23. 2009 p. 16–17.
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