Atmosphere of Earth

"Air" redirects here. For other uses, see Air (disambiguation). "Qualities of air" redirects here. Not to be confused with Air quality.

The atmosphere of Earth is composed of a layer of gas mixture that surrounds the Earth's planetary surface (both lands and oceans), known collectively as air, with variable quantities of suspended aerosols and particulates (which create weather features such as clouds and hazes), all retained by Earth's gravity. The atmosphere serves as a protective buffer between the Earth's surface and outer space, shields the surface from most meteoroids and ultraviolet solar radiation, keeps it warm and reduces diurnal temperature variation (temperature extremes between day and night) through heat retention (greenhouse effect), redistributes heat and moisture among different regions via air currents, and provides the chemical and climate conditions allowing life to exist and evolve on Earth.

Blue light is scattered more than other wavelengths by the gases in the atmosphere, surrounding Earth in a visibly blue layer at the stratosphere, above the clouds of the troposphere, when seen from space on board the ISS at an altitude of 335 km (208 mi) (the Moon is visible as a crescent in the far background).^[1]

By mole fraction (i.e., by quantity of molecules), dry air contains 78.08% nitrogen, 20.95% oxygen, 0.93% argon, 0.04% carbon dioxide, and small amounts of other trace gases. Air also contains a variable amount of water vapor, on average around 1% at sea level, and 0.4% over the entire atmosphere. Air composition, temperature and atmospheric pressure vary with altitude. Within the atmosphere, air suitable for use in photosynthesis by terrestrial plants and respiration of terrestrial animals is found only within 12 kilometres (7.5 mi) from the ground.^[2]

Earth's early atmosphere consisted of accreted gases from the solar nebula, but the atmosphere changed significantly over time, affected by many factors such as volcanism, impact events, weathering and the evolution of life (particularly the photoautotrophs). Recently, human activity has also contributed to atmospheric changes, such as climate change (mainly through deforestation and fossil fuel-related global warming), ozone depletion and acid deposition.

The atmosphere has a mass of about 5.15×10¹⁸ kg,^[3] three quarters of which is within about 11 km (6.8 mi; 36,000 ft) of the surface. The atmosphere becomes thinner with increasing altitude, with no definite boundary between the atmosphere and outer space. The Kármán line, at 100 km (62 mi) or 1.57% of Earth's radius, is often used as the border between the atmosphere and outer space. Atmospheric effects become noticeable during atmospheric reentry of spacecraft at an altitude of around 120 km (75 mi). Several layers can be distinguished in the atmosphere based on characteristics such as temperature and composition, namely the troposphere, stratosphere, mesosphere, thermosphere (formally the ionosphere) and exosphere.

The study of Earth's atmosphere and its processes is called atmospheric science (aerology), and includes multiple subfields, such as climatology and atmospheric physics. Early pioneers in the field include Léon Teisserenc de Bort and Richard Assmann.^[4] The study of historic atmosphere is called paleoclimatology.

Composition

Main article: Atmospheric chemistry

Composition of Earth's atmosphere by molecular count, excluding water vapor. Lower pie represents trace gases that together compose about 0.0434% of the atmosphere (0.0442% at August 2021 concentrations^[5][6]). Numbers are mainly from 2000, with CO₂ and methane from 2019, and do not represent any single source.^[7]

The three major constituents of Earth's atmosphere are nitrogen, oxygen, and argon. Water vapor accounts for roughly 0.25% of the atmosphere by mass. The concentration of water vapor (a greenhouse gas) varies significantly from around 10 ppm by mole fraction in the coldest portions of the atmosphere to as much as 5% by mole fraction in hot, humid air masses, and concentrations of other atmospheric gases are typically quoted in terms of dry air (without water vapor).^[8]: 8 The remaining gases are often referred to as trace gases,^[9] among which are other greenhouse gases, principally carbon dioxide, methane, nitrous oxide, and ozone. Besides argon, other noble gases, neon, helium, krypton, and xenon are also present. Filtered air includes trace amounts of many other chemical compounds. Many substances of natural origin may be present in locally and seasonally variable small amounts as aerosols in an unfiltered air sample, including dust of mineral and organic composition, pollen and spores, sea spray, and volcanic ash. Various industrial pollutants also may be present as gases or aerosols, such as chlorine (elemental or in compounds), fluorine compounds and elemental mercury vapor. Sulfur compounds such as hydrogen sulfide and sulfur dioxide (SO₂) may be derived from natural sources or from industrial air pollution.

The volume fraction of the main constituents of the Earth's atmosphere as a function of height, based on the MSIS-E-90 atmospheric model; the model only works above 85 km

Major constituents of air, by mole fraction^[13]

Dry air
Gas		Mole fraction(A)
Name	Formula	in ppm(B)	in %
Nitrogen	N2	780,840	78.084
Oxygen	O2	209,460	20.946
Argon	Ar	9,340	0.9340
Carbon dioxide (April 2022)(C)[14]	CO2	417	0.0417
Neon	Ne	18.18	0.001818
Helium	He	5.24	0.000524
Methane (2022)(C)[15]	CH4	1.91	0.000191
Krypton	Kr	1.14	0.000114
If air is not dry:
Water vapor(D)	H2O	0–30,000(D)	0–3%(E)
Notes (A) Mole fraction is sometimes referred to as volume fraction; these are identical for an ideal gas only. (B) ppm: parts per million by molecular count The total ppm above adds up to more than 1 million (currently 83.43 above it) due to experimental error. (C) The concentration of CO2 has been increasing in recent decades, as has that of CH4. (D) Water vapor is about 0.25% by mass over full atmosphere (E) Water vapor varies significantly locally[8]

The average molecular weight of dry air, which can be used to calculate densities or to convert between mole fraction and mass fraction, is about 28.946^[16] or 28.96^[17][18] g/mol. This is decreased when the air is humid.

The relative concentration of gases remains constant until about 10,000 m (33,000 ft).^[19]

Stratification

Earth's atmosphere. Lower four layers of the atmosphere in three dimensions as seen diagonally from above the exobase. Layers drawn to scale, objects within the layers are not to scale. Aurorae shown at the bottom of the thermosphere can form at any altitude within this layer.

In general, air pressure and density decrease with altitude in the atmosphere. However, temperature has a more complicated profile with altitude and may remain relatively constant or even increase with altitude in some regions (see the temperature section). Because the general pattern of the temperature/altitude profile, or lapse rate, is constant and measurable by means of instrumented balloon soundings, the temperature behavior provides a useful metric to distinguish atmospheric layers. This atmospheric stratification divides the Earth's atmosphere into five main layers:^[20]

• Exosphere: 700–10,000 km (435–6,214 mi)^[21]
• Thermosphere: 80–700 km (50–435 mi)^[22]
• Mesosphere: 50–80 km (31–50 mi)
• Stratosphere: 12–50 km (7–31 mi)
• Troposphere: 0–12 km (0–7 mi)^[23]

Exosphere

Main article: Exosphere

The exosphere is the outermost layer of Earth's atmosphere (though it is so tenuous that some scientists consider it to be part of interplanetary space rather than part of the atmosphere). It extends from the thermopause (also known as the "exobase") at the top of the thermosphere to a poorly defined boundary with the solar wind and interplanetary medium. The altitude of the exobase varies from about 500 kilometres (310 mi; 1,600,000 ft) to about 1,000 kilometres (620 mi) in times of higher incoming solar radiation.^[24]

The upper limit varies depending on the definition. Various authorities consider it to end at about 10,000 kilometres (6,200 mi)^[25] or about 190,000 kilometres (120,000 mi)—about halfway to the moon, where the influence of Earth's gravity is about the same as radiation pressure from sunlight.^[24] The geocorona visible in the far ultraviolet (caused by neutral hydrogen) extends to at least 100,000 kilometres (62,000 mi).^[24]

This layer is mainly composed of extremely low densities of hydrogen, helium and several heavier molecules including nitrogen, oxygen and carbon dioxide closer to the exobase. The atoms and molecules are so far apart that they can travel hundreds of kilometres without colliding with one another. Thus, the exosphere no longer behaves like a gas, and the particles constantly escape into space. These free-moving particles follow ballistic trajectories and may migrate in and out of the magnetosphere or the solar wind. Every second, the Earth loses about 3 kg of hydrogen, 50 g of helium, and much smaller amounts of other constituents.^[26]

The exosphere is too far above Earth for meteorological phenomena to be possible. However, Earth's auroras—the aurora borealis (northern lights) and aurora australis (southern lights)—sometimes occur in the lower part of the exosphere, where they overlap into the thermosphere. The exosphere contains many of the artificial satellites that orbit Earth.

Thermosphere

Main article: Thermosphere

The thermosphere is the second-highest layer of Earth's atmosphere. It extends from the mesopause (which separates it from the mesosphere) at an altitude of about 80 km (50 mi; 260,000 ft) up to the thermopause at an altitude range of 500–1000 km (310–620 mi; 1,600,000–3,300,000 ft). The height of the thermopause varies considerably due to changes in solar activity.^[22] Because the thermopause lies at the lower boundary of the exosphere, it is also referred to as the exobase. The lower part of the thermosphere, from 80 to 550 kilometres (50 to 342 mi) above Earth's surface, contains the ionosphere.

The temperature of the thermosphere gradually increases with height and can rise as high as 1500 °C (2700 °F), though the gas molecules are so far apart that its temperature in the usual sense is not very meaningful. The air is so rarefied that an individual molecule (of oxygen, for example) travels an average of 1 kilometre (0.62 mi; 3300 ft) between collisions with other molecules.^[27] Although the thermosphere has a high proportion of molecules with high energy, it would not feel hot to a human in direct contact, because its density is too low to conduct a significant amount of energy to or from the skin.

This layer is completely cloudless and free of water vapor. However, non-hydrometeorological phenomena such as the aurora borealis and aurora australis are occasionally seen in the thermosphere. The International Space Station orbits in this layer, between 350 and 420 km (220 and 260 mi). It is this layer where many of the satellites orbiting the Earth are present.

Mesosphere

Main article: Mesosphere

Afterglow of the troposphere (orange), the stratosphere (blue) and the mesosphere (dark) at which atmospheric entry begins, leaving smoke trails, such as in this case of a spacecraft reentry

The mesosphere is the third highest layer of Earth's atmosphere, occupying the region above the stratosphere and below the thermosphere. It extends from the stratopause at an altitude of about 50 km (31 mi; 160,000 ft) to the mesopause at 80–85 km (50–53 mi; 260,000–280,000 ft) above sea level.

Temperatures drop with increasing altitude to the mesopause that marks the top of this middle layer of the atmosphere. It is the coldest place on Earth and has an average temperature around −85 °C (−120 °F; 190 K).^[28][29]

Just below the mesopause, the air is so cold that even the very scarce water vapor at this altitude can condense into polar-mesospheric noctilucent clouds of ice particles. These are the highest clouds in the atmosphere and may be visible to the naked eye if sunlight reflects off them about an hour or two after sunset or similarly before sunrise. They are most readily visible when the Sun is around 4 to 16 degrees below the horizon. Lightning-induced discharges known as transient luminous events (TLEs) occasionally form in the mesosphere above tropospheric thunderclouds. The mesosphere is also the layer where most meteors burn up upon atmospheric entrance. It is too high above Earth to be accessible to jet-powered aircraft and balloons, and too low to permit orbital spacecraft. The mesosphere is mainly accessed by sounding rockets and rocket-powered aircraft.

Stratosphere

Main article: Stratosphere

The stratosphere is the second-lowest layer of Earth's atmosphere. It lies above the troposphere and is separated from it by the tropopause. This layer extends from the top of the troposphere at roughly 12 km (7.5 mi; 39,000 ft) above Earth's surface to the stratopause at an altitude of about 50 to 55 km (31 to 34 mi; 164,000 to 180,000 ft).

The atmospheric pressure at the top of the stratosphere is roughly 1/1000 the pressure at sea level. It contains the ozone layer, which is the part of Earth's atmosphere that contains relatively high concentrations of that gas. The stratosphere defines a layer in which temperatures rise with increasing altitude. This rise in temperature is caused by the absorption of ultraviolet radiation (UV) from the Sun by the ozone layer, which restricts turbulence and mixing. Although the temperature may be −60 °C (−76 °F; 210 K) at the tropopause, the top of the stratosphere is much warmer, and may be near 0 °C.^[30]

The stratospheric temperature profile creates very stable atmospheric conditions, so the stratosphere lacks the weather-producing air turbulence that is so prevalent in the troposphere. Consequently, the stratosphere is almost completely free of clouds and other forms of weather. However, polar stratospheric or nacreous clouds are occasionally seen in the lower part of this layer of the atmosphere where the air is coldest. The stratosphere is the highest layer that can be accessed by jet-powered aircraft.

Troposphere

Main article: Troposphere

A picture of Earth's troposphere, with different cloud types at low and high altitudes casting shadows. Sunlight, filtered into a reddish hue by passing through much of the troposphere at sunset, is reflected off the ocean. The above-lying stratosphere can be seen at the horizon as a band of its characteristic glow of blue scattered sunlight.

The troposphere is the lowest layer of Earth's atmosphere. It extends from Earth's surface to an average height of about 12 km (7.5 mi; 39,000 ft), although this altitude varies from about 9 km (5.6 mi; 30,000 ft) at the geographic poles to 17 km (11 mi; 56,000 ft) at the Equator,^[23] with some variation due to weather. The troposphere is bounded above by the tropopause, a boundary marked in most places by a temperature inversion (i.e. a layer of relatively warm air above a colder one), and in others by a zone that is isothermal with height.^[31][32]

Although variations do occur, the temperature usually declines with increasing altitude in the troposphere because the troposphere is mostly heated through energy transfer from the surface. Thus, the lowest part of the troposphere (i.e. Earth's surface) is typically the warmest section of the troposphere. This promotes vertical mixing (hence, the origin of its name in the Greek word τρόπος, tropos, meaning "turn"). The troposphere contains roughly 80% of the mass of Earth's atmosphere.^[33] The troposphere is denser than all its overlying layers because a larger atmospheric weight sits on top of the troposphere and causes it to be most severely compressed. Fifty percent of the total mass of the atmosphere is located in the lower 5.6 km (3.5 mi; 18,000 ft) of the troposphere.

Nearly all atmospheric water vapor or moisture is found in the troposphere, so it is the layer where most of Earth's weather takes place. It has basically all the weather-associated cloud genus types generated by active wind circulation, although very tall cumulonimbus thunder clouds can penetrate the tropopause from below and rise into the lower part of the stratosphere. Most conventional aviation activity takes place in the troposphere, and it is the only layer accessible by propeller-driven aircraft.

Other layers

Within the five principal layers above, which are largely determined by temperature, several secondary layers may be distinguished by other properties:

• The ozone layer is contained within the stratosphere. In this layer ozone concentrations are about 2 to 8 parts per million, which is much higher than in the lower atmosphere but still very small compared to the main components of the atmosphere. It is mainly located in the lower portion of the stratosphere from about 15–35 km (9.3–21.7 mi; 49,000–115,000 ft), though the thickness varies seasonally and geographically. About 90% of the ozone in Earth's atmosphere is contained in the stratosphere.
• The ionosphere is a region of the atmosphere that is ionized by solar radiation. It is responsible for auroras. During daytime hours, it stretches from 50 to 1,000 km (31 to 621 mi; 160,000 to 3,280,000 ft) and includes the mesosphere, thermosphere, and parts of the exosphere. However, ionization in the mesosphere largely ceases during the night, so auroras are normally seen only in the thermosphere and lower exosphere. The ionosphere forms the inner edge of the magnetosphere. It has practical importance because it influences, for example, radio propagation on Earth.
• The homosphere and heterosphere are defined by whether the atmospheric gases are well mixed. The surface-based homosphere includes the troposphere, stratosphere, mesosphere, and the lowest part of the thermosphere, where the chemical composition of the atmosphere does not depend on molecular weight because the gases are mixed by turbulence.^[34] This relatively homogeneous layer ends at the turbopause found at about 100 km (62 mi; 330,000 ft), the very edge of space itself as accepted by the FAI, which places it about 20 km (12 mi; 66,000 ft) above the mesopause.

Above this altitude lies the heterosphere, which includes the exosphere and most of the thermosphere. Here, the chemical composition varies with altitude. This is because the distance that particles can move without colliding with one another is large compared with the size of motions that cause mixing. This allows the gases to stratify by molecular weight, with the heavier ones, such as oxygen and nitrogen, present only near the bottom of the heterosphere. The upper part of the heterosphere is composed almost completely of hydrogen, the lightest element.^[35]

• The planetary boundary layer is the part of the troposphere that is closest to Earth's surface and is directly affected by it, mainly through turbulent diffusion. During the day the planetary boundary layer usually is well-mixed, whereas at night it becomes stably stratified with weak or intermittent mixing. The depth of the planetary boundary layer ranges from as little as about 100 metres (330 ft) on clear, calm nights to 3,000 m (9,800 ft) or more during the afternoon in dry regions.

The average temperature of the atmosphere at Earth's surface is 14 °C (57 °F; 287 K)^[36] or 15 °C (59 °F; 288 K),^[37] depending on the reference.^[38][39][40]

Physical properties

Comparison of the 1962 US Standard Atmosphere graph of geometric altitude against air density, pressure, the speed of sound and temperature with approximate altitudes of various objects.^[41]

Pressure and thickness

Main article: Atmospheric pressure

The average atmospheric pressure at sea level is defined by the International Standard Atmosphere as 101325 pascals (760.00 Torr; 14.6959 psi; 760.00 mmHg). This is sometimes referred to as a unit of standard atmospheres (atm). Total atmospheric mass is 5.1480×10¹⁸ kg (1.13494×10¹⁹ lb),^[42] about 2.5% less than would be inferred from the average sea-level pressure and Earth's area of 51007.2 megahectares, this portion being displaced by Earth's mountainous terrain. Atmospheric pressure is the total weight of the air above unit area at the point where the pressure is measured. Thus air pressure varies with location and weather.

If the entire mass of the atmosphere had a uniform density equal to sea-level density (about 1.2 kg/m³) from sea level upwards, it would terminate abruptly at an altitude of 8.50 km (27,900 ft).

Air pressure actually decreases exponentially with altitude, for altitudes up to around 70 km (43 mi; 230,000 ft), dropping by half every 5.6 km (18,000 ft), or by a factor of 1/e ≈ 0.368 every 7.64 km (25,100 ft), which is called the scale height. However, the atmosphere is more accurately modeled with a customized equation for each layer that takes gradients of temperature, molecular composition, solar radiation and gravity into account. At heights over 100 km, an atmosphere may no longer be well mixed. Then each chemical species has its own scale height.

In summary, the mass of Earth's atmosphere is distributed approximately as follows:^[43]

• 50% is below 5.6 km (18,000 ft),
• 90% is below 16 km (52,000 ft),
• 99.99997% is below 100 km (62 mi; 330,000 ft), the Kármán line. By international convention, this marks the beginning of space where human travelers are considered astronauts.

By comparison, the summit of Mount Everest is at 8,848 m (29,029 ft); commercial airliners typically cruise between 10 and 13 km (33,000 and 43,000 ft), where the lower density and temperature of the air improve fuel economy; weather balloons reach 30.4 km (100,000 ft) and above; and the highest X-15 flight in 1963 reached 108.0 km (354,300 ft).

Even above the Kármán line, significant atmospheric effects such as auroras still occur. Meteors begin to glow in this region, though the larger ones may not burn up until they penetrate more deeply. The various layers of Earth's ionosphere, important to HF radio propagation, begin below 100 km and extend beyond 500 km. By comparison, the International Space Station and Space Shuttle typically orbit at 350–400 km, within the F-layer of the ionosphere, where they encounter enough atmospheric drag to require reboosts every few months, otherwise orbital decay will occur, resulting in a return to Earth. Depending on solar activity, satellites can experience noticeable atmospheric drag at altitudes as high as 700–800 km.

Temperature

Main article: Atmospheric temperature

Temperature trends in two thick layers of the atmosphere as measured between January 1979 and December 2005 by microwave sounding units and advanced microwave sounding units on NOAA weather satellites. The instruments record microwaves emitted from oxygen molecules in the atmosphere. Source:^[44]

The division of the atmosphere into layers mostly by reference to temperature is discussed above. Temperature decreases with altitude starting at sea level, but variations in this trend begin above 11 km, where the temperature stabilizes over a large vertical distance through the rest of the troposphere. In the stratosphere, starting above about 20 km, the temperature increases with height, due to heating within the ozone layer caused by the capture of significant ultraviolet radiation from the Sun by the dioxygen and ozone gas in this region. Still another region of increasing temperature with altitude occurs at very high altitudes, in the aptly-named thermosphere above 90 km.

Speed of sound

Main article: Speed of sound

Because in an ideal gas of constant composition the speed of sound depends only on temperature and not on pressure or density, the speed of sound in the atmosphere with altitude takes on the form of the complicated temperature profile (see illustration to the right), and does not mirror altitudinal changes in density or pressure.

Density and mass

Temperature and mass density against altitude from the NRLMSISE-00 standard atmosphere model (the eight dotted lines in each "decade" are at the eight cubes 8, 27, 64, ..., 729)

Main article: Density of air

The density of air at sea level is about 1.2 kg/m³ (1.2 g/L, 0.0012 g/cm³). Density is not measured directly but is calculated from measurements of temperature, pressure and humidity using the equation of state for air (a form of the ideal gas law). Atmospheric density decreases as the altitude increases. This variation can be approximately modeled using the barometric formula. More sophisticated models are used to predict the orbital decay of satellites.

The average mass of the atmosphere is about 5 quadrillion (5×10¹⁵) tonnes or 1/1,200,000 the mass of Earth. According to the American National Center for Atmospheric Research, "The total mean mass of the atmosphere is 5.1480×10¹⁸ kg with an annual range due to water vapor of 1.2 or 1.5×10¹⁵ kg, depending on whether surface pressure or water vapor data are used; somewhat smaller than the previous estimate. The mean mass of water vapor is estimated as 1.27×10¹⁶ kg and the dry air mass as 5.1352 ±0.0003×10¹⁸ kg."

Tabulated properties

Physical and thermal properties of air at atmospheric pressure^{[45]: 602 [46]}

Temperature [K]	Density [kg/m3]	Specific heat [J/(kg⋅°C)]	Dynamic viscosity [kg/(m⋅s)]	Kinematic viscosity [m2/s]	Thermal conductivity [W/(m⋅°C)]	Thermal diffusivity [m2/s]	Prandtl number [1]	Bulk modulus [K−1]
100	3.601	1026.6	6.92×10−6	1.92×10−6	0.000925	2.50×10−6	0.77	0.01
150	2.3675	1009.9	1.03×10−5	4.34×10−6	0.013735	5.75×10−6	0.753	0.006667
200	1.7684	1006.1	1.33×10−5	7.49×10−6	0.01809	1.02×10−5	0.738	0.005
250	1.4128	1005.3	1.60×10−5	1.13×10−5	0.02227	1.57×10−5	0.722	0.004
300	1.1774	1005.7	1.85×10−5	1.57×10−5	0.02624	2.22×10−5	0.708	0.003333
350	0.998	1009	2.08×10−5	2.08×10−5	0.03003	2.98×10−5	0.697	0.002857
400	0.8826	1014	2.29×10−5	2.59×10−5	0.03365	3.76×10−5	0.689	0.0025
450	0.7833	1020.7	2.48×10−5	3.17×10−5	0.03707	4.22×10−5	0.683	0.002222
500	0.7048	1029.5	2.67×10−5	3.79×10−5	0.04038	5.56×10−5	0.68	0.002
550	0.6423	1039.2	2.85×10−5	4.43×10−5	0.0436	6.53×10−5	0.68	0.001818
600	0.5879	1055.1	3.02×10−5	5.13×10−5	0.04659	7.51×10−5	0.68	0.001667
650	0.543	1063.5	3.18×10−5	5.85×10−5	0.04953	8.58×10−5	0.682	0.001538
700	0.503	1075.2	3.33×10−5	6.63×10−5	0.0523	9.67×10−5	0.684	0.001429
750	0.4709	1085.6	3.48×10−5	7.39×10−5	0.05509	1.08×10−4	0.686	0.001333
800	0.4405	1097.8	3.63×10−5	8.23×10−5	0.05779	1.20×10−4	0.689	0.00125
850	0.4149	1109.5	3.77×10−5	9.08×10−5	0.06028	1.31×10−4	0.692	0.001176
900	0.3925	1121.2	3.90×10−5	9.93×10−5	0.06279	1.43×10−4	0.696	0.001111
950	0.3716	1132.1	4.02×10−5	1.08×10−4	0.06525	1.55×10−4	0.699	0.001053
1000	0.3524	1141.7	4.15×10−5	1.18×10−4	0.06753	1.68×10−4	0.702	0.001
1100	0.3204	1160	4.44×10−5	1.39×10−4	0.0732	1.97×10−4	0.704	0.000909
1200	0.2947	1179	4.69×10−5	1.59×10−4	0.0782	2.25×10−4	0.707	0.000833
1300	0.2707	1197	4.93×10−5	1.82×10−4	0.0837	2.58×10−4	0.705	0.000769
1400	0.2515	1214	5.17×10−5	2.06×10−4	0.0891	2.92×10−4	0.705	0.000714
1500	0.2355	1230	5.40×10−5	2.29×10−4	0.0946	3.26×10−4	0.705	0.000667
1600	0.2211	1248	5.63×10−5	2.55×10−4	0.1	3.61×10−4	0.705	0.000625
1700	0.2082	1267	5.85×10−5	2.81×10−4	0.105	3.98×10−4	0.705	0.000588
1800	0.197	1287	6.07×10−5	3.08×10−4	0.111	4.38×10−4	0.704	0.000556
1900	0.1858	1309	6.29×10−5	3.39×10−4	0.117	4.81×10−4	0.704	0.000526
2000	0.1762	1338	6.50×10−5	3.69×10−4	0.124	5.26×10−4	0.702	0.0005
2100	0.1682	1372	6.72×10−5	4.00×10−4	0.131	5.72×10−4	0.7	0.000476
2200	0.1602	1419	6.93×10−5	4.33×10−4	0.139	6.12×10−4	0.707	0.000455
2300	0.1538	1482	7.14×10−5	4.64×10−4	0.149	6.54×10−4	0.71	0.000435
2400	0.1458	1574	7.35×10−5	5.04×10−4	0.161	7.02×10−4	0.718	0.000417
2500	0.1394	1688	7.57×10−5	5.44×10−4	0.175	7.44×10−4	0.73	0.0004

Optical properties

See also: Sunlight

Solar radiation (or sunlight) is the energy Earth receives from the Sun. Earth also emits radiation back into space, but at longer wavelengths that humans cannot see. Part of the incoming and emitted radiation is absorbed or reflected by the atmosphere.^[47][48] In May 2017, glints of light, seen as twinkling from an orbiting satellite a million miles away, were found to be reflected light from ice crystals in the atmosphere.^[49][50]

Scattering

Main article: Atmospheric scattering

When light passes through Earth's atmosphere, photons interact with it through scattering. If the light does not interact with the atmosphere, it is called direct radiation and is what you see if you were to look directly at the Sun. Indirect radiation is light that has been scattered in the atmosphere. For example, on an overcast day when you cannot see your shadow, there is no direct radiation reaching you, it has all been scattered. As another example, due to a phenomenon called Rayleigh scattering, shorter (blue) wavelengths scatter more easily than longer (red) wavelengths. This is why the sky looks blue; you are seeing scattered blue light. This is also why sunsets are red. Because the Sun is close to the horizon, the Sun's rays pass through more atmosphere than normal before reaching your eye. Much of the blue light has been scattered out, leaving the red light in a sunset.

Absorption

Main article: Absorption (electromagnetic radiation)

Rough plot of Earth's atmospheric transmittance (or opacity) to various wavelengths of electromagnetic radiation, including visible light

Different molecules absorb different wavelengths of radiation. For example, O₂ and O₃ absorb almost all radiation with wavelengths shorter than 300 nanometres. Water (H₂O) absorbs at many wavelengths above 700 nm. When a molecule absorbs a photon, it increases the energy of the molecule. This heats the atmosphere, but the atmosphere also cools by emitting radiation, as discussed below.

The combined absorption spectra of the gases in the atmosphere leave "windows" of low opacity, allowing the transmission of only certain bands of light. The optical window runs from around 300 nm (ultraviolet-C) up into the range humans can see, the visible spectrum (commonly called light), at roughly 400–700 nm and continues to the infrared to around 1100 nm. There are also infrared and radio windows that transmit some infrared and radio waves at longer wavelengths. For example, the radio window runs from about one centimetre to about eleven-metre waves.

Emission

Further information: Emission spectrum

Emission is the opposite of absorption, it is when an object emits radiation. Objects tend to emit amounts and wavelengths of radiation depending on their "black body" emission curves, therefore hotter objects tend to emit more radiation, with shorter wavelengths. Colder objects emit less radiation, with longer wavelengths. For example, the Sun is approximately 6,000 K (5,730 °C; 10,340 °F), its radiation peaks near 500 nm, and is visible to the human eye. Earth is approximately 290 K (17 °C; 62 °F), so its radiation peaks near 10,000 nm, and is much too long to be visible to humans.

Because of its temperature, the atmosphere emits infrared radiation. For example, on clear nights Earth's surface cools down faster than on cloudy nights. This is because clouds (H₂O) are strong absorbers and emitters of infrared radiation. This is also why it becomes colder at night at higher elevations.

The greenhouse effect is directly related to this absorption and emission effect. Some gases in the atmosphere absorb and emit infrared radiation, but do not interact with sunlight in the visible spectrum. Common examples of these are CO₂ and H₂O.

Refractive index

Distortive effect of atmospheric refraction upon the shape of the sun at the horizon

Main article: Atmospheric refraction

See also: Scintillation (astronomy)

The refractive index of air is close to, but just greater than, 1. Systematic variations in the refractive index can lead to the bending of light rays over long optical paths. One example is that, under some circumstances, observers on board ships can see other vessels just over the horizon because light is refracted in the same direction as the curvature of Earth's surface.

The refractive index of air depends on temperature,^[51] giving rise to refraction effects when the temperature gradient is large. An example of such effects is the mirage.

Circulation

Main article: Atmospheric circulation

An idealised view of three pairs of large circulation cells

Atmospheric circulation is the large-scale movement of air through the troposphere, and the means (with ocean circulation) by which heat is distributed around Earth. The large-scale structure of the atmospheric circulation varies from year to year, but the basic structure remains fairly constant because it is determined by Earth's rotation rate and the difference in solar radiation between the equator and poles.

Evolution of Earth's atmosphere

See also: History of Earth and Paleoclimatology

Earliest atmosphere

The first atmosphere, during the Early Earth's Hadean eon, consisted of gases in the solar nebula, primarily hydrogen, and probably simple hydrides such as those now found in the gas giants (Jupiter and Saturn), notably water vapor, methane and ammonia. During this earliest era, the Moon-forming collision and numerous impacts with large meteorites heated the atmosphere, driving off the most volatile gases. The collision with Theia, in particular, melted and ejected large portions of Earth's mantle and crust and outgassed significant amounts of steam which eventually cooled and condensed to contribute to ocean water at the end of the Hadean.^[52]: 10

Second atmosphere

See also: Prebiotic atmosphere

The increasing solidification of Earth's crust at the end of the Hadean closed off most of the advective heat transfer to the surface, causing the atmosphere to cool, which condensed most of the water vapor out of the air precipitating into a superocean. Further outgassing from volcanism, supplemented by gases introduced by huge asteroids during the Late Heavy Bombardment, created the subsequent Archean atmosphere, which consisted largely of nitrogen plus carbon dioxide, methane and inert gases.^[52] A major part of carbon dioxide emissions dissolved in water and reacted with metals such as calcium and magnesium during weathering of crustal rocks to form carbonates that were deposited as sediments. Water-related sediments have been found that date from as early as 3.8 billion years ago.^[53]

About 3.4 billion years ago, nitrogen formed the major component of the then-stable "second atmosphere". The influence of the evolution of life has to be taken into account rather soon in the history of the atmosphere because hints of earliest life forms appeared as early as 3.5 billion years ago.^[54] How Earth at that time maintained a climate warm enough for liquid water and life, if the early Sun put out 30% lower solar radiance than today, is a puzzle known as the "faint young Sun paradox".

The geological record however shows a continuous relatively warm surface during the complete early temperature record of Earth – with the exception of one cold glacial phase about 2.4 billion years ago. In the late Neoarchean, an oxygen-containing atmosphere began to develop, apparently due to a billion years of cyanobacterial photosynthesis (see Great Oxygenation Event), which have been found as stromatolite fossils from 2.7 billion years ago. The early basic carbon isotopy (isotope ratio proportions) strongly suggests conditions similar to the current, and that the fundamental features of the carbon cycle became established as early as 4 billion years ago.

Ancient sediments in the Gabon dating from between about 2.15 and 2.08 billion years ago provide a record of Earth's dynamic oxygenation evolution. These fluctuations in oxygenation were likely driven by the Lomagundi carbon isotope excursion.^[55]

Third atmosphere

Oxygen content of the atmosphere over the last billion years^[56][57]

Main article: Geological history of oxygen

The constant re-arrangement of continents by plate tectonics influences the long-term evolution of the atmosphere by transferring carbon dioxide to and from large continental carbonate stores. Free oxygen did not exist in the atmosphere until about 2.4 billion years ago during the Great Oxygenation Event and its appearance is indicated by the end of banded iron formations (which signals the depletion of substrates that can react with oxygen to produce ferric deposits) during the early Proterozoic eon.

Before this time, any oxygen produced by cyanobacterial photosynthesis would be readily removed by the oxidation of reducing substances on the Earth's surface, notably ferrous iron, sulfur and atmospheric methane. Free oxygen molecules did not start to accumulate in the atmosphere until the rate of production of oxygen began to exceed the availability of reductant materials that removed oxygen. This point signifies a shift from a reducing atmosphere to an oxidizing atmosphere. O₂ showed major variations during the Proterozoic, including a billion-year period of euxinia, until reaching a steady state of more than 15% by the end of the Precambrian.^[58] The rise of the more robust eukaryotic photoautotrophs (green and red algae) injected further oxygenation into the air, especially after the end of the Cryogenian global glaciation, which was followed by an evolutionary radiation event during the Ediacaran period known as the Avalon explosion, where complex metazoan life forms (including the earliest cnidarians, placozoans and bilaterians) first proliferated. The following time span from 539 million years ago to the present day is the Phanerozoic eon, during the earliest period of which, the Cambrian, more actively moving metazoan life began to appear and rapidly diversify in another radiation event called the Cambrian explosion, whose locomotive metabolism was fuelled by the rising oxygen level.

The amount of oxygen in the atmosphere has fluctuated over the last 600 million years, reaching a peak of about 30% around 280 million years ago during the Carboniferous period, significantly higher than today's 21%. Two main processes govern changes in the atmosphere: the evolution of plants and their increasing role in carbon fixation, and the consumption of oxygen by rapidly diversifying animal faunae and also by plants for photorespiration and their own metabolic needs at night. Breakdown of pyrite and volcanic eruptions release sulfur into the atmosphere, which reacts and hence reduces oxygen in the atmosphere. However, volcanic eruptions also release carbon dioxide, which can fuel oxygenic photosynthesis by terrestrial and aquatic plants. The cause of the variation of the amount of oxygen in the atmosphere is not precisely understood. Periods with more oxygen in the atmosphere were often associated with more rapid development of animals.

Air pollution

Animation shows the buildup of tropospheric CO₂ in the Northern Hemisphere with a maximum around May. The maximum in the vegetation cycle follows in the late summer. Following the peak in vegetation, the drawdown of atmospheric CO₂ due to photosynthesis is apparent, particularly over the boreal forests.

Main article: Air pollution

Air pollution is the introduction of airborne chemicals, particulate matter or biological materials that cause harm or discomfort to organisms.^[59] The population growth, industrialization and motorization of human societies have significantly increased the amount of airborne pollutants in the Earth's atmosphere, causing noticeable problems such as smogs, acid rains and pollution-related diseases. The depletion of stratospheric ozone layer, which shields the surface from harmful ionizing ultraviolet radiations, is also caused by air pollution, chiefly from chlorofluorocarbons and other ozone-depleting substances.

Since 1750, human activity, especially after the Industrial Revolution, has increased the concentrations of various greenhouse gases, most importantly carbon dioxide, methane and nitrous oxide. Greenhouse gas emissions, coupled with deforestation and destruction of wetlands via logging and land developments, have caused an observed rise in global temperatures, with the global average surface temperatures being 1.1 °C higher in the 2011–2020 decade than they were in 1850.^[60] It has raised concerns of man-made climate change, which can have significant environmental impacts such as sea level rise, ocean acidification, glacial retreat (which threatens water security), increasing extreme weather events and wildfires, ecological collapse and mass dying of wildlife.

See also

• Environment portal
• Science portal
• World portal

• Aerial perspective
• Air (classical element)
• Biosphere
• Hydrosphere
• Lithosphere
• Airglow
• Airshed
• Atmospheric dispersion modeling
• Atmospheric electricity
• Climate system
• COSPAR international reference atmosphere (CIRA)
• Environmental effects of aviation
• Global dimming
• Instrumental temperature record
• Reference atmospheric model

References

1. "Gateway to Astronaut Photos of Earth". NASA. Retrieved 2018-01-29.
2. "What Is... Earth's Atmosphere? - NASA". 2024-05-13. Retrieved 2024-06-18.
3. Lide, David R. Handbook of Chemistry and Physics. Boca Raton, FL: CRC, 1996: 14–17
4. Vázquez, M.; Hanslmeier, A. (2006). "Historical Introduction". Ultraviolet Radiation in the Solar System. Astrophysics and Space Science Library. Vol. 331. Springer Science & Business Media. p. 17. Bibcode:2005ASSL..331.....V. doi:10.1007/1-4020-3730-9_1. ISBN 978-1-4020-3730-6.
5. "Trends in Atmospheric Carbon Dioxide", Global Greenhouse Gas Reference Network, NOAA, 2019, retrieved 2019-05-31
6. "Trends in Atmospheric Methane", Global Greenhouse Gas Reference Network, NOAA, 2019, retrieved 2019-05-31
7. Haynes, H. M., ed. (2016–2017), CRC Handbook of Chemistry and Physics (97th ed.), CRC Press, p. 14-3, ISBN 978-1-4987-5428-6, which cites Allen's Astrophysical Quantities but includes only ten of its largest constituents.
8. Wallace, John M. and Peter V. Hobbs. Atmospheric Science: An Introductory Survey Archived 2018-07-28 at the Wayback Machine. Elsevier. Second Edition, 2006. ISBN 978-0-12-732951-2. Chapter 1
9. "Trace Gases". Ace.mmu.ac.uk. Archived from the original on 9 October 2010. Retrieved 2010-10-16.
10. Cox, Arthur N., ed. (2000), Allen's Astrophysical Quantities (Fourth ed.), AIP Press, pp. 258–259, ISBN 0-387-98746-0, which rounds N₂ and O₂ to four significant digits without affecting the total because 0.004% was removed from N₂ and added to O₂. It includes 20 constituents.
11. National Aeronautics and Space Administration (1976), U.S. Standard Atmosphere, 1976 (PDF), p. 3
12. Allen, C. W. (1976), Astrophysical Quantities (Third ed.), Athlone Press, p. 119, ISBN 0-485-11150-0
13. Two recent reliable sources cited here have total atmospheric compositions, including trace molecules, that exceed 100%. They are Allen's Astrophysical Quantities^[10] (2000, 100.001241343%) and CRC Handbook of Chemistry and Physics^[7] (2016–2017, 100.004667%), which cites Allen's Astrophysical Quantities. Both are used as references in this article. Both exceed 100% because their CO₂ values were increased to 345 ppmv, without changing their other constituents to compensate. This is made worse by the April 2019 CO₂ value, which is 413.32 ppmv.^[5] Although minor, the January 2019 value for CH₄ is 1866.1 ppbv (parts per billion).^[6] Two older reliable sources have dry atmospheric compositions, including trace molecules, that total less than 100%: U.S. Standard Atmosphere, 1976^[11] (99.9997147%); and Astrophysical Quantities^[12] (1976, 99.9999357%).
14. "Vital signs: Carbon Dioxide". NASA Climate. April 2022. Retrieved 16 May 2022.
15. "Vital signs: Methane". NASA Climate. April 2022. Retrieved 2 Feb 2024.
16. Detlev Möller: Luft: Chemie, Physik, Biologie, Reinhaltung, Recht. Walter de Gruyter, 2003, ISBN 3-11-016431-0, S. 173. (View in Google Books).
17. Yunus Çengel. Termodinamica e trasmissione del calore.
18. "Air - Molecular Weight and Composition". www.engineeringtoolbox.com. Retrieved 2021-04-27.
19. "Air Composition". The Engineering ToolBox. Retrieved 2017-07-04. The composition of air is unchanged until elevation of approximately 10.000 m
20. Zell, Holly (2015-03-02). "Earth's Upper Atmosphere". NASA. Retrieved 2017-02-20.
21. "Exosphere - overview". UCAR. 2011. Archived from the original on 17 May 2017. Retrieved April 19, 2015.
22. Randy Russell (2008). "The Thermosphere". Retrieved 2013-10-18.
23. "The height of the tropopause". Das.uwyo.edu. Retrieved 2012-04-18.^{[dead link‍]}
24. "Exosphere - overview". UCAR. 2011. Archived from the original on 17 May 2017. Retrieved April 19, 2015.
25. "Earth's Atmospheric Layers". January 22, 2013.
26. David C. Catling and Kevin J. Zahnle, The Planetary Air Leak, Scientific American, May 2009, p. 26 (accessed 25 July 2012)
27. Ahrens, C. Donald. Essentials of Meteorology. Published by Thomson Brooks/Cole, 2005.
28. States, Robert J.; Gardner, Chester S. (January 2000). "Thermal Structure of the Mesopause Region (80–105 km) at 40°N Latitude. Part I: Seasonal Variations". Journal of the Atmospheric Sciences. 57 (1): 66–77. Bibcode:2000JAtS...57...66S. doi:10.1175/1520-0469(2000)057<0066:TSOTMR>2.0.CO;2.
29. Joe Buchdahl. "Atmosphere, Climate & Environment Information Programme". Ace.mmu.ac.uk. Archived from the original on 2010-07-01. Retrieved 2012-04-18.
30. Journal of the Atmospheric Sciences (1993). "stratopause". Archived from the original on 2013-10-19. Retrieved 2013-10-18.
31. Barry, R.G.; Chorley, R.J. (1971). Atmosphere, Weather and Climate. London: Menthuen & Co Ltd. p. 65. ISBN 9780416079401.
32. Tyson, P.D.; Preston-Whyte, R.A. (2013). The Weather and Climate of Southern Africa (2nd ed.). Oxford: Oxford University Press. p. 4.
33. "Troposphere". Concise Encyclopedia of Science & Technology. McGraw-Hill. 1984. It contains about four-fifths of the mass of the whole atmosphere.
34. "homosphere – AMS Glossary". Amsglossary.allenpress.com. Archived from the original on 14 September 2010. Retrieved 2010-10-16.
35. Anne Marie Helmenstine, PhD (June 16, 2018). "The 4 Most Abundant Gases in Earth's Atmosphere".
36. "Earth's Atmosphere". Archived from the original on 2009-06-14.
37. "NASA – Earth Fact Sheet". Nssdc.gsfc.nasa.gov. Archived from the original on 30 October 2010. Retrieved 2010-10-16.
38. "Global Surface Temperature Anomalies". Archived from the original on 2009-03-03.
39. "Earth's Radiation Balance and Oceanic Heat Fluxes". Archived from the original on 2005-03-03.
40. "Coupled Model Intercomparison Project Control Run" (PDF). Archived from the original (PDF) on 2008-05-28.
41. Geometric altitude vs. temperature, pressure, density, and the speed of sound derived from the 1962 U.S. Standard Atmosphere.
42. Trenberth, Kevin E.; Smith, Lesley (1970-01-01). "The Mass of the Atmosphere: A Constraint on Global Analyses". Journal of Climate. 18 (6): 864. Bibcode:2005JCli...18..864T. CiteSeerX 10.1.1.727.6573. doi:10.1175/JCLI-3299.1. S2CID 16754900.
43. Lutgens, Frederick K. and Edward J. Tarbuck (1995) The Atmosphere, Prentice Hall, 6th ed., pp. 14–17, ISBN 0-13-350612-6.
44. "Atmospheric Temperature Trends, 1979–2005 : Image of the Day". Earthobservatory.nasa.gov. 2000-01-01. Retrieved 2014-06-10.
45. Holman, Jack P. (2002). Heat transfer (9th ed.). New York, NY: McGraw-Hill Companies, Inc. p. 602. ISBN 9780072406559. OCLC 46959719.
46. Bergman, Theodore L.; Lavine, Adrienne S.; Incropera, Frank P.; DeWitt, David P. (2007). Fundamentals of heat and mass transfer (6th ed.). Hoboken, NJ: John Wiley and Sons, Inc. pp. 941–950. ISBN 9780471457282. OCLC 62532755.
47. "Absorption / reflection of sunlight". Understanding Global Change. Retrieved 2023-06-13.
48. "The Atmospheric Window". National Oceanic and Atmospheric Administration. Retrieved 2023-06-13.
49. St. Fleur, Nicholas (19 May 2017). "Spotting Mysterious Twinkles on Earth From a Million Miles Away". The New York Times. Retrieved 20 May 2017.
50. Marshak, Alexander; Várnai, Tamás; Kostinski, Alexander (15 May 2017). "Terrestrial glint seen from deep space: oriented ice crystals detected from the Lagrangian point". Geophysical Research Letters. 44 (10): 5197. Bibcode:2017GeoRL..44.5197M. doi:10.1002/2017GL073248. hdl:11603/13118. S2CID 109930589.
51. Edlén, Bengt (1966). "The refractive index of air". Metrologia. 2 (2): 71–80. Bibcode:1966Metro...2...71E. doi:10.1088/0026-1394/2/2/002.
52. Zahnle, K.; Schaefer, L.; Fegley, B. (2010). "Earth's Earliest Atmospheres". Cold Spring Harbor Perspectives in Biology. 2 (10): a004895. doi:10.1101/cshperspect.a004895. PMC 2944365. PMID 20573713.
53. B. Windley: The Evolving Continents. Wiley Press, New York 1984
54. J. Schopf: Earth's Earliest Biosphere: Its Origin and Evolution. Princeton University Press, Princeton, N.J., 1983
55. Timothy W. Lyons, Christopher T. Reinhard & Noah J. Planavsky (2014). "Atmospheric oxygenation three billion years ago". Nature. 506 (7488): 307–15. Bibcode:2014Natur.506..307L. doi:10.1038/nature13068. PMID 24553238. S2CID 4443958.
56. Martin, Daniel; McKenna, Helen; Livina, Valerie (2016). "The human physiological impact of global deoxygenation". The Journal of Physiological Sciences. 67 (1): 97–106. doi:10.1007/s12576-016-0501-0. ISSN 1880-6546. PMC 5138252. PMID 27848144.
57. Graph: Atmospheric Oxygen and CO2 vs Time
58. Christopher R. Scotese, Back to Earth History : Summary Chart for the Precambrian, Paleomar Project
59. Starting from Pollution – Definition from the Merriam-Webster Online Dictionary
60. IPCC (2021). "Summary for Policymakers" (PDF). IPCC AR6 WG1. pp. 4–5. Archived from the original (PDF) on 2021-08-11. Retrieved 2021-11-20.

External links

• Buchan, Alexander (1878). "Atmosphere" . Encyclopædia Britannica. Vol. III (9th ed.). pp. 28–36.
• Interactive global map of current atmospheric and ocean surface conditions.