Atmosphere

{{Short description|Layer of gases surrounding an astronomical body held by gravity}} {{hatnote group| {{About|atmospheres of celestial bodies|other uses}} {{Redirect|Atmospheric environment|the scientific journal|Atmospheric Environment}} }} [[File:Top of Atmosphere.jpg|thumb|upright=1.5|The atmospheric gases around Earth scatter blue light (shorter wavelengths) more than light toward the red end (longer wavelengths) of the visible spectrum; thus, a blue glow over the horizon is seen when observing Earth from outer space. The Moon is visible in the background.]]

An '''atmosphere''' is a layer of gases that envelop an astronomical object, held in place by the gravity of the object. The name originates {{etymology|grc|''{{Wikt-lang|grc|ἀτμός}}'' ({{grc-transl|ἀτμός}})|vapour, steam||''{{Wikt-lang|grc|σφαῖρα}}'' ({{grc-transl|σφαῖρα}})|sphere}}.<ref name="etymology"/> An object acquires most of its atmosphere during its primordial epoch, either by accretion of matter or by outgassing of volatiles. The chemical interaction of the atmosphere with the solid surface can change its fundamental composition, as can photochemical interaction with the Sun. A planet retains an atmosphere for longer durations when the gravity is high and the temperature is low. The solar wind works to strip away a planet's outer atmosphere, although this process is slowed by a magnetosphere. The further a body is from the Sun, the lower the rate of atmospheric stripping.

Aside from Mercury, all Solar System planets have substantial atmospheres, as does the dwarf planet Pluto and the moon Titan. The high gravity and low temperature of Jupiter and the other gas giant planets allow them to retain massive atmospheres of mostly hydrogen and helium. Lower mass terrestrial planets orbit closer to the Sun, and so mainly retain higher molar mass atmospheres made of carbon, nitrogen, and oxygen, with trace amounts of inert gas. Atmospheres have been detected around exoplanets such as HD 209458 b and Kepler-7b.

A stellar atmosphere is the outer region of a star, which includes the layers above the opaque photosphere; stars of low temperature might have outer atmospheres containing compound molecules.<ref>{{cite book | title=Stardust: The Cosmic Seeds of Life | series=Astronomers' Universe | first=Sun | last=Kwok | publisher=Springer Science & Business Media | year=2013 | isbn=978-3-642-32802-2 | pages=87–88 | url=https://books.google.com/books?id=oSBEAAAAQBAJ&pg=PA88 }}</ref> Other objects with atmospheres are brown dwarfs and active comets.

==Occurrence and compositions== ===Origins=== right|thumb|Artist's impression of a newly-formed protoplanet In the nebular hypothesis, stars form during the gravitational collapse of a mass of gas and dust within an interstellar molecular cloud. This material forms a pancake-like rotating disk with the mass concentrated at the center. The protostar is created at the central mass concentration, while the planets and satellites are formed in the disk through a process of accretion. Dust settles into the median disk plane, forming materials that can collide and accrete to create planetesimals. Close to the star, these bodies grow and accumulate to form protoplanets consisting primarily of refractory materials with few volatiles. Further from the star, planetary embryos are created from accumulation of volatiles up to around ten times the mass of the Earth or more. Masses of gas are then acquired from the surrounding disk nebula, forming a gas giant around the embryo. Planetary satellites form in a similar fashion from the disk of material around the planets.<ref name=Sanchez-Lavega>{{cite book | title=An Introduction to Planetary Atmospheres | first=Agustin | last=Sanchez-Lavega | publisher=CRC Press | year=2011 | isbn=978-1-4200-6735-4 | pages=71–97 | url=https://books.google.com/books?id=lCXYQ4phwbwC&pg=PA71 }}</ref>

The primary atmosphere of a planet is produced when the gravity is sufficient to retain accreted gas against escape processes. The latter can include collisions with other bodies that impart sufficient energy for the gasses to escape. For the terrestrial planets, the high temperatures generated by their initial bombardment results in the outgassing of volatiles, creating the secondary atmosphere. The original composition and thickness of the atmosphere is thus determined by the stellar nebula's chemistry and temperature, but can be modified by processes within the astronomical body that release different atmospheric components.<ref name=Sanchez-Lavega/> The circumstellar disk will finally dissipate on time scales of about 10⁷ years, and the star will complete its contraction then ignite hydrogen fusion at its core in a time frame determined by its mass. (For example, a star with the mass of the Sun will spend {{Val|3|e=7}} years contracting.)<ref>{{cite book | title=An Introduction to the Theory of Stellar Structure and Evolution | first=Dina | last=Prialnik | publisher=Cambridge University Press | year=2000 | isbn=978-0-521-65937-6 | url=https://books.google.com/books?id=TGyzlVbgkiMC&pg=PA136 }}</ref>

===Compositions=== thumb|upright=1.2|Graphs of escape velocity against surface temperature of some Solar System objects showing which gases are retained. The objects are drawn to scale, and their data points are at the black dots in the middle. The atmospheres of the planets Venus and Mars are principally composed of carbon dioxide, nitrogen, and argon.<ref name="universetoday"/> Because Venus has no oceans or rain to dissolve the carbon dioxide, large amounts of this greenhouse gas has remained in the atmosphere. The result is a dense atmosphere about 80 times the pressure of Earth's atmosphere.<ref>{{cite book | title=The Cosmos: Astronomy in the New Millennium | first1=Jay M. | last1=Pasachoff | first2=Alex | last2=Filippenko | publisher=Cambridge University Press | year=2019 | isbn=978-1-108-43138-5 | url=https://books.google.com/books?id=VG2MDwAAQBAJ&pg=PA162 }}</ref> The planet's lack of a magnetic field and closer proximity to the Sun resulted in the loss of its hydrogen (in the form of water) after two billion years.<ref>{{cite book | title=Exoplanet Atmospheres: Physical Processes | volume=18 | series=Princeton Series in Astrophysics | first=Sara | last=Seager | publisher=Princeton University Press | year=2010 | isbn=978-0-691-14645-4 | url=https://books.google.com/books?id=7IQqEAAAQBAJ&pg=PA82 }}</ref>

Because Mars is small, cold, and lacks a magnetic field, it has retained only a sparse atmosphere. The surface air pressure of {{Val|0.6|ul=kPa}} for Mars is only 0.6% of Earth's {{Val|101.3|u=kPa}}.<ref name=Teles_2014/> The planet has probably lost at least 80–85% of its original water supply to space.<ref>{{cite journal | title=Atmospheric Loss to Space and the History of Water on Mars | last=Jakosky | first=Bruce M. | journal=Annual Review of Earth and Planetary Sciences | volume=49 | pages=71–93 | date=May 2021 | doi=10.1146/annurev-earth-062420-052845 | bibcode=2021AREPS..49...71J }}</ref> However, the planet has retained significant deposits of frozen water and carbon dioxide. If all of the frozen CO₂ were to sublimate, the air pressure could climb to {{Val|30|u=kPa}}. This is comparable to the air pressure on the top of Mount Everest.<ref name=Teles_2014>{{cite book | chapter=Mars Astrobiology: Recent Status and Progress | first=Antonio de Morais M. | last=Teles | title=Planetary Exploration and Science: Recent Results and Advances | series=Springer Geophysics | display-editors=1 | editor1-first=Shuanggen | editor1-last=Jin | editor2-first=Nader | editor2-last=Haghighipour | editor3-first=Wing-Huen | editor3-last=Ip | publisher=Springer | year=2014 | isbn=978-3-662-45052-9 | pages=220–221 | chapter-url=https://books.google.com/books?id=TZKeBQAAQBAJ&pg=PA220 }}</ref>

The composition of Earth's atmosphere is determined by the by-products of the life that it sustains. Dry air (mixture of gases) from Earth's atmosphere contains 78.08% nitrogen, 20.95% oxygen, 0.93% argon, 0.04% carbon dioxide, and traces of hydrogen, helium, and other "noble" gases (by volume), but generally a variable amount of water vapor is also present, on average about 1% at sea level.<ref name="tornadosfsu"/> Earth's persistent magnetosphere acts as a shield against atmospheric scavenging by the solar wind, as it fends off the incoming plasma at a distance of about 10 Earth radii.<ref>{{cite book | chapter=Planetary Magnetic Fields and Solar Forcing: Implications for Atmospheric Evolution | display-authors=1 | last1=Lundin | first1=Rickard | last2=Lammer | first2=Helmut | last3=Ribas | first3=Ignasi | title=Geology and Habitability of Terrestrial Planets | series=Space Sciences Series of ISSI | volume=24 | isbn=978-0-387-74287-8 | publisher=Springer Science+Business Media, LLC | year=2007 | page=245 | doi=10.1007/978-0-387-74288-5_9 | bibcode=2007ghtp.book..245L }}</ref>

The low temperatures and higher escape velocities of the Solar System's giant planets—Jupiter, Saturn, Uranus and Neptune—allow them more readily to retain gases with low molecular masses. These planets have reducing atmospheres of hydrogen and helium, with trace amounts of other elements and more complex compounds. Unlike the terrestrial planets, the gas giants lack a well-defined surface. Instead the atmosphere is maintained in hydrostatic equilibrium by intense pressure deep in the body. The dynamic weather on these bodies only occurs in a relatively thin surface layer.<ref>{{cite book | title=Drifting on Alien Winds: Exploring the Skies and Weather of Other Worlds | series=SpringerLink : Bücher | first=Michael | last=Carroll | publisher=Springer Science & Business Media | year=2011 | isbn=978-1-4419-6917-0 | pages=129–131 | url=https://books.google.com/books?id=yK2hFJFBgbUC&pg=PA129 }}</ref>

Two satellites of the outer planets possess significant atmospheres. Titan, a moon of Saturn, and Triton, a moon of Neptune, have atmospheres mainly of nitrogen.<ref name="Lorenz2014"/><ref name="Ingersoll1990"/> When in the part of its orbit closest to the Sun, Pluto has an atmosphere of nitrogen and methane similar to Triton's, but these gases are frozen when it is farther from the Sun.

Other bodies within the Solar System have extremely thin atmospheres not in equilibrium. These include the Moon (sodium gas, noble gases, hydrogen), Mercury (sodium gas), Callisto (carbon dioxide and oxygen), Europa (oxygen), Io (sulfur dioxide), and Enceladus (water vapor).

====Exoplanets==== Planetary objects around distant stars, known as exoplanets, span a more diverse range of physical properties than is found in the Solar System. These targets provide an opportunity to study atmospheres around a broad span of objects and conditions. However, observations of these targets requires much more sensitive instrumentation. The methods used to analyze these remote atmospheres are transit spectroscopy, high-resolution Doppler spectroscopy, and direct imaging.<ref>{{cite journal | title=Exoplanetary Atmospheres: Key Insights, Challenges, and Prospects | last=Madhusudhan | first=Nikku | journal=Annual Review of Astronomy and Astrophysics | date=August 2019 | volume=57 | pages=617–663 | doi=10.1146/annurev-astro-081817-051846 | arxiv=1904.03190 | bibcode=2019ARA&A..57..617M }}</ref>

Transit spectroscopy uses the transit of an exoplanet across its host star to detect its atmosphere. By comparing the radius at different wavelengths, the presence of specific components can be detected. The first such detection was in 2002, when sodium was detected in the atmosphere of HD 209458b,<ref name=Burrows_2014>{{cite journal | title=Highlights in the study of exoplanet atmospheres | last=Burrows | first=Adam S. | journal=Nature | volume=513 | issue=7518 | pages=345–352 | date=September 2014 | doi=10.1038/nature13782 | pmid=25230656 | arxiv=1409.7320 | bibcode=2014Natur.513..345B }}</ref> a gas giant with a close orbit around a star in the constellation Pegasus. Its atmosphere is heated to temperatures over 1,000&nbsp;K, and is steadily escaping into space. Hydrogen, oxygen, and carbon have been detected in the planet's inflated atmosphere by Hubble observations.<ref name="HD209458"/> Since 2002, potassium has been detected in the atmosphere of XO-2Nb, and both sodium and potassium in HD 189733 b's atmosphere.<ref name=Burrows_2014/>

Many of the discovered super earths have orbits close enough to their host star that their surfaces are expected to be magma oceans. The secondary atmospheres of these lava planets most likely consist of materials that have been vaporized from the magma, such as sodium, potassium, oxygen, and silicon oxide.<ref name=Lammer_et_al_2022/>

===Atmospheres in the Solar System=== {| class="wikitable" style="text-align:center;" ! Atmosphere ! Surface<br/>Pressure<br/>(kPa) ! Mean surface<br/>temperature<br/>(K) ! Surface<br/>gravity<br/>(ɡ₀) ! Scale<br/>height<br/>(km) !colspan=2| Primary composition<br/>(by volume) ! Notes |- !style="text-align:left;"| Sun | {{cvt|0.868|kPa|disp=number}} | 5,772 (eff.) | {{cvt|274.0|m/s2|g0|2|disp=number}} | &ndash; | 91.0% H || 8.9% He | <ref>{{cite web | title=Sun Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html | access-date=2025-08-18 }}</ref> |- !style="text-align:left;"| Mercury | Negligible | 440 | {{cvt|3.70|m/s2|g0|2|disp=number}} | &ndash; |colspan=2| Na, Mg, O, H, K, Ca | <ref>{{cite web | title=Mercury Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/mercuryfact.html | access-date=2025-08-18 }}</ref> |- !style="text-align:left;"| Venus | {{cvt|92|bar|kPa|0|disp=number}} | 737 | {{cvt|8.87|m/s2|g0|2|disp=number}} | 15.9 | 96.5% CO₂ || 3.5% N₂ | <ref>{{cite web | title=Venus Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/venusfact.html | access-date=2025-08-18 }}</ref> |- !style="text-align:left;"| Earth | {{cvt|1014|mb|kPa|0|disp=number}} | 288 | {{cvt|9.820|m/s2|g0|sigfig=3|disp=number}} | 8.5 | 78.1% N₂ || 21.0% O₂ | <ref>{{cite web | title=Earth Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/earthfact.html | access-date=2025-08-18 }}</ref> |- |style="text-align:left;"| &nbsp; Moon | Negligible | {{cvt|-20|C|K|0|disp=number}} | {{cvt|1.62|m/s2|g0|2|disp=number}} | &ndash; |colspan=2| He, Ne, H₂, Ar | <ref>{{cite web | title=Moon Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/moonfact.html | access-date=2025-08-18 }}</ref> |- !style="text-align:left;"| Mars | {{cvt|6.36|mb|kPa|0|disp=number}} | 214 | {{cvt|3.73|m/s2|g0|2|disp=number}} | 11.0 | 95.1% CO₂ || 2.6% N₂ | <ref>{{cite web | title=Mars Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/marsfact.html | access-date=2025-08-18 }}</ref> |- !style="text-align:left;"| Ceres | Negligible | {{cvt|-105|C|K|0|disp=number}} | {{cvt|0.26|m/s2|g0|2|disp=number}} | &ndash; |colspan=2| H₂O | <ref name=SSSW>{{cite web | title=Solar System Small Worlds Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/galileanfact_table.html | access-date=2025-08-18 }}</ref><ref>{{Cite journal | title=Localized sources of water vapour on the dwarf planet (1) Ceres | last1=Küppers | first1=M. | display-authors=etal | date=January 23, 2014 | journal=Nature |volume=505 |issue=7484 |pages=525–527 | bibcode=2014Natur.505..525K | doi=10.1038/nature12918 | issn=0028-0836 | pmid=24451541 | s2cid=4448395 }}</ref> |- !style="text-align:left;"| Jupiter | (At {{cvt|1|bar|kPa|0|disp=number}}) | 165 | {{cvt|25.92|m/s2|g0|2|disp=number}} | 27 | 89.8% H₂ || 10.2% He | <ref>{{cite web | title=Jupiter Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/jupiterfact.html | access-date=2025-08-18 }}</ref> |- |style="text-align:left;"| &nbsp; Io | Negligible | {{cvt|-155|C|K|0|disp=number}} | {{cvt|1.80|m/s2|g0|2|disp=number}} | &ndash; |colspan=2|SO₂ | <ref name=SSSW/><ref name=Catling_Kasting_2017>{{cite book | title=Atmospheric Evolution on Inhabited and Lifeless Worlds | first1=David C. | last1=Catling | first2=James F. | last2=Kasting | publisher=Cambridge University Press | year=2017 | isbn=978-1-316-82452-8 | page=399 | url=https://books.google.com/books?id=2nuJDgAAQBAJ&pg=PA399 }}</ref> |- |style="text-align:left;"| &nbsp; Callisto | Negligible | {{cvt|-170|C|K|0|disp=number}} | {{cvt|1.24|m/s2|g0|2|disp=number}} | &ndash; |colspan=2|O₂ and some CO₂ | <ref name=SSSW/><ref name=Catling_Kasting_2017/> |- |style="text-align:left;"| &nbsp; Europa | Negligible | {{cvt|-170|C|K|0|disp=number}} | {{cvt|1.31|m/s2|g0|2|disp=number}} | &ndash; |colspan=2|O₂ | <ref name=SSSW/><ref name=Catling_Kasting_2017/> |- |style="text-align:left;"| &nbsp; Ganymede | Negligible | {{cvt|-160|C|K|0|disp=number}} | {{cvt|1.43|m/s2|g0|2|disp=number}} | &ndash; |colspan=2|O₂ | <ref name=SSSW/><ref name=Catling_Kasting_2017/> |- !style="text-align:left;"| Saturn | (At {{cvt|1|bar|kPa|0|disp=number}}) | 134 | {{cvt|11.19|m/s2|g0|2|disp=number}} | 59.5 | 96.3% H₂ || 3.25% He | <ref>{{cite web | title=Saturn Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/saturnfact.html | access-date=2025-08-18 }}</ref> |- |style="text-align:left;"| &nbsp; Titan | {{cvt|1.47|bar|kPa|0|disp=number}} | {{cvt|-180|C|K|0|disp=number}} | {{cvt|1.35|m/s2|g0|2|disp=number}} | 20 | 98.4% N₂ || 1.5% CH₄ | <ref name=SSSW/><ref>{{cite journal | title=Isotopic Ratios in Titan's Methane: Measurements and Modeling | display-authors=1 | last1=Nixon | first1=C. A. | last2=Temelso | first2=B. | last3=Vinatier | first3=S. | last4=Teanby | first4=N. A. | last5=Bézard | first5=B. | last6=Achterberg | first6=R. K. | last7=Mandt | first7=K. E. | last8=Sherrill | first8=C. D. | last9=Irwin | first9=P. G. J. | last10=Jennings | first10=D. E. | last11=Romani | first11=P. N. | last12=Coustenis | first12=A. | last13=Flasar | first13=F. M. | journal=The Astrophysical Journal | date=April 2012 | volume=749 | issue=2 | at=id. 159 | doi=10.1088/0004-637X/749/2/159 | bibcode=2012ApJ...749..159N }}</ref><ref>{{cite journal | title=Prediction of aerodynamically-triggered condensation: Application to the Dragonfly rotorcraft in Titan's atmosphere | display-authors=1 | last1=Lorenz | first1=Ralph D. | last2=Schmitz | first2=Sven | last3=Kinzel | first3=Michael | journal=Aerospace Science and Technology | volume=114 | at=id. 106738 | date=July 2021 | article-number=106738 | doi=10.1016/j.ast.2021.106738 | bibcode=2021AeST..11406738L }}</ref> |- |style="text-align:left;"| &nbsp; Enceladus | Negligible | 72 | {{cvt|0.114|m/s2|g0|2|disp=number}} | &ndash; |colspan=2|H₂O and CO₂ | <ref>{{cite book | title=The Cambridge Planetary Handbook | first=Michael E. | last=Bakich | publisher=Cambridge University Press | year=2000 | isbn=978-0-521-63280-5 | page=251 | url=https://books.google.com/books?id=PE99nOKjbXAC&pg=PA251 }}</ref><ref>{{cite book | chapter=Clean In-Situ Subsurface Exploration of Icy Environments | display-authors=1 | last1=Dachwald | first1=B. | last2=Ulamec | first2=S. | last3=Biele | first3=Jens | title=Habitability of Other Planets and Satellites | volume=28 | series=Cellular Origin, Life in Extreme Habitats and Astrobiology | editor1-first=Jean-Pierre | editor1-last=de Vera | editor2-first=Joseph | editor2-last=Seckbach | publisher=Springer Science & Business Media | year=2013 | isbn=978-94-007-6546-7 | page=372 | chapter-url=https://books.google.com/books?id=VYjEBAAAQBAJ&pg=PA372 }}</ref><ref name=Catling_Kasting_2017/> |- !style="text-align:left;"| Uranus | (At {{cvt|1|bar|kPa|0|disp=number}}) | 76 | {{cvt|9.01|m/s2|g0|2|disp=number}} | 27.7 | 82.5% H₂ || 15.2% He | <ref>{{cite web | title=Uranus Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/uranusfact.html | access-date=2025-08-18 }}</ref> |- |style="text-align:left;"| &nbsp; Titania | Tenuous | 70 | {{cvt|0.38|m/s2|g0|2|disp=number}} | {{Val|30|to|95}} |colspan=2| Possibly CO₂, CH₄, or N₂ | <ref>{{cite journal | title=Titania's radius and an upper limit on its atmosphere from the September 8, 2001 stellar occultation | last1=Widemann | first1=T. | display-authors=etal | journal=Icarus | date=2009 | volume=199 | issue=2 | pages=458–476 | doi=10.1016/j.icarus.2008.09.011 | bibcode=2009Icar..199..458W | url=https://hal.science/hal-00506795 }}</ref> |- !style="text-align:left;"| Neptune | (At {{cvt|1|bar|kPa|0|disp=number}}) | 72 | {{cvt|11.27|m/s2|g0|2|disp=number}} | {{Val|19.1|to|20.3}} | 80.0% H₂ || 19.0% He | <ref>{{cite web | title=Neptune Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/neptunefact.html | access-date=2025-08-18 }}</ref> |- |style="text-align:left;"| &nbsp; Triton | 0.001 | 38 | {{cvt|0.78|m/s2|g0|2|disp=number}} | 14.8 |colspan=2| Mostly N₂ | <ref name=SSSW/><ref name="Ingersoll1990"/><ref>{{cite journal | title=Constraints on the evolution of the Triton atmosphere from occultations: 1989-2022 | last1=Sicardy | first1=B. | display-authors=etal | journal=Astronomy & Astrophysics | date=February 2024 | volume=682 | pages=8 | doi=10.1051/0004-6361/202348756 | arxiv=2402.02476 | bibcode=2024A&A...682L..24S }}</ref> |- !style="text-align:left;"| Pluto | 0.001 | {{Val|24|to|38}} | {{cvt|0.62|m/s2|g0|3|disp=number}} | 18 | 99% N₂ || 0.5% CH₄ | <ref>{{cite web | title=Pluto Fact Sheet | first=David R. | last=Williams | website=NASA Space Science Data Coordinated Archive | url=https://nssdc.gsfc.nasa.gov/planetary/factsheet/plutofact.html | access-date=2025-08-18 }}</ref><ref>{{cite journal | title=The atmosphere of Pluto as observed by New Horizons | display-authors=etal | last1=Gladstone | first1=G. R. | date=March 2016 | journal=Science | volume=351 | issue=6279 | at=id. aad8866 | article-number=aad8866 | doi=10.1126/science.aad8866 | bibcode=2016Sci...351.8866G | arxiv=1604.05356 | pmid=26989258 | s2cid=32043359 }}</ref>

|- !style="text-align:left;"| {{mpl-|612533|2002 XV|93}} | 0.00002 | {{Val|40|to|50}} | – | – |colspan=2| unknown; either {{chem|N|2}}, Ar, or {{chem|CH|4}}? | <ref name="Wong2026">{{Cite arxiv|last=Wong |first=Ian |last2=Protopapa |first2=Silvia |last3=Lellouch |first3=Emmanuel |date=2026-05-29 |title=Constraints on the Atmospheric Composition of {{mp|2002 XV|93}} from JWST Spectroscopy |eprint=2605.29206 |class=astro-ph.EP}}</ref> |}

==Conditions== {{main|Atmospheric pressure|Atmospheric temperature}}

An atmosphere in hydrostatic equilibrium consists of a balance between the air pressure created by the motions of the molecules, and the restraining force of gravity that prevents the molecules from escaping. The pressure decreases in altitude, producing a pressure-gradient force.<ref name=McSween_2019/> Atmospheric pressure is the force (per unit-area) perpendicular to a unit-area of planetary surface, as determined by the weight of the vertical column of atmospheric gases. In said atmospheric model, the atmospheric pressure, the weight of the mass of the gas, decreases at high altitude because of the diminishing mass of the gas above the point of barometric measurement. Air pressure varies by place and time due to meteorological conditions and atmospheric waves.<ref>{{cite book | title=Stratosphere Troposphere Interactions: An Introduction | first=K. | last=Mohanakumar | publisher=Springer Science & Business Media | year=2008 | isbn=978-1-4020-8217-7 | pages=6–7 | url=https://books.google.com/books?id=pAQDbLQXnksC&pg=PA6 }}</ref>

Units of air pressure are based upon the standard atmosphere (atm), which is 101,325&nbsp;Pa (equivalent to 760&nbsp;Torr or 14.696&nbsp;psi). For an ideal gas atmosphere, the height at which the atmospheric pressure declines by a factor of ''e'' (the base of the natural logarithm) is called the scale height (''H''). For an atmosphere of uniform temperature, the scale height is proportional to the atmospheric temperature and is inversely proportional to the product of the mean molecular mass of dry air, and the local acceleration of gravity at the point of barometric measurement.<ref name=Awiphan_2018>{{cite book | title=Exomoons to Galactic Structure: High Precision Studies with the Microlensing and Transit Methods | series=Springer Theses | first=Supachai | last=Awiphan | publisher=Springer | year=2018 | isbn=978-3-319-90957-8 | pages=29–31 | url=https://books.google.com/books?id=2wNbDwAAQBAJ&pg=PA30 }}</ref>

The temperature of the atmosphere is determined by an energy budget, which balances the heating from the incoming solar energy against the heat radiated back into space. The incoming energy is determined by the distance from the Sun, and the energy reflected back out by the planetary albedo.<ref name=McSween_2019/> When a planet is in radiative equilibrium, it has a planetary equilibrium temperature.<ref name=McSween_2019>{{cite book | title=Planetary Geoscience | first=Harry Y. | last=McSween | publisher=Cambridge University Press | year=2019 | isbn=978-1-107-14538-2 | pages=213–214 | url=https://books.google.com/books?id=oTCdDwAAQBAJ&pg=PA213 }}</ref> This differs from the global mean temperature, which may be warmer than the equilibrium temperature due to the atmospheric greenhouse effect. For example, Venus has a surface temperature of almost {{Val|460|u=C}} compared to an equilibrium temperature of {{Val|−40|u=C}}.<ref>{{cite book | chapter=Greenhouse Effect | first=Andrew A. | last=Lacis | title=Greenhouse Gases: Emission, Measurement and Management | editor-first=Guoxiang | editor-last=Liu | publisher=BoD – Books on Demand | year=2012 | isbn=978-953-51-0323-3 | pages=275–276 | chapter-url=https://books.google.com/books?id=_ayZDwAAQBAJ&pg=PA275 }}</ref>

==Structure== Planetary atmospheres are composed of layers with different properties, such as specific gaseous composition, temperature gradients, and pressure.

===Terrestrial planets=== For Earth, Mars, and Venus, the lowest level of the atmosphere is the troposphere, where most of the planet's clouds and weather are found. This extends from the ground up to 65&nbsp;km on Venus, 40&nbsp;km on Mars, and 17&nbsp;km on Earth.<ref name=de_Pater_Lissauer_2015/> The troposphere contains the bulk of the atmosphere, possessing {{Val|80|-|98|u=%}} of the total atmospheric mass.<ref>{{cite book | chapter=Terrestrial Planet Atmospheres and Biosignatures | last1=Meadows | first1=V. | first2=S. | last2=Seager | title=Exoplanets | series=The University of Arizona Space Science Series | editor-first=Sara | editor-last=Seager | publisher=University of Arizona Press | year=2011 | isbn=978-0-8165-2945-2 | page=446 | chapter-url=https://books.google.com/books?id=VlSVmxgPgGYC&pg=PA445 }}</ref> Temperature varies by altitude according to the lapse rate, as thermal energy from the ground is transported upward via convection. Infrared radiation becomes trapped by molecules of gas and water vapor.<ref name=McSween_2019/> For the Earth, the next layer is the stratosphere, which is a region of temperature increasing with altitude, creating a temperature inversion. This region contains the UV-absorbing ozone layer, at an altitude between 15&nbsp;km and 35&nbsp;km, which is responsible for the temperature rise.<ref name=de_Pater_Lissauer_2015/> Energy transport in this region occurs through radiation processes.<ref name=McSween_2019/> Lacking an oxygenated atmosphere to generate a significant layer of ozone, neither Mars nor Venus have a stratosphere.<ref name=de_Pater_Lissauer_2015>{{cite book | title=Planetary Sciences | first1=Imke | last1=de Pater | first2=Jack J. | last2=Lissauer | edition=2 | publisher=Cambridge University Press | year=2015 | isbn=978-1-316-19569-7 | pages=81–82 | url=https://books.google.com/books?id=stFpBgAAQBAJ&pg=PA81 }}</ref>

Above the troposphere-stratosphere, the next layer of the atmosphere is termed the mesosphere. In this region, the water vapor and carbon dioxide serves as a heat sink that radiates energy in the infrared. As a result, the temperature of the mesosphere decreases with altitude, reaching the coldest layer of the atmosphere at the top.<ref name=Chandra_2010/> Both Venus and Mars have an altitude range in the mesosphere where the temperature is nearly isothermal; for Mars this is above 120&nbsp;km, while for Venus it is between 63 and 75&nbsp;km altitude.<ref name=de_Pater_Lissauer_2015/>

In the lower regions of the atmosphere, turbulent mixing causes the atmospheric constituents to be evenly distributed. Above a transition layer called the homopause, molecular diffusion dominates. This results in diffuse separation of the constituents by atomic weight; that is, lower mass components diffuse upward leaving higher mass molecules near the bottom. The homopause is at an altitude of {{Val|100|-|110|u=km}} for the Earth, {{Val|115|-|130|u=km}} for Mars, and {{Val|135|-|150|u=km}} for Venus.<ref>{{cite book | chapter=Isotope Fractionation by Gravitational Escape | first1=H. | last1=Lammer | first2=S. J. | last2=Bauer | title=Solar System History from Isotopic Signatures of Volatile Elements: Volume Resulting from an ISSI Workshop 14–18 January 2002, Bern, Switzerland | volume=16 | series=Space Sciences Series of ISSI | display-editors=1 | editor1-first=R. | editor1-last=Kallenbach | editor2-first=Thérèse | editor2-last=Encrenaz | editor3-first=Johannes | editor3-last=Geiss | editor4-first=Konrad | editor4-last=Mauersberger | editor5-first=Tobias | editor5-last=Owen | editor6-first=François | editor6-last=Robert | publisher=Springer Science & Business Media | year=2012 | page=284 | isbn=978-94-010-0145-8 | chapter-url=https://books.google.com/books?id=A-LzCAAAQBAJ&pg=PA284 }}</ref>

Beyond the mesosphere is a region of the atmosphere called the thermosphere that absorbs X-rays and extreme UV from the Sun, causing temperature to rise with altitude. The thermal properties of this layer vary daily and with solar activity cycles.<ref name=Chandra_2010>{{cite book | chapter=Planetary Atmospheres | first=H. | last=Chandra | title=Heliophysical Processes | series=Astrophysics and Space Science Proceedings | display-editors=1 | editor1-first=Natchimuthuk | editor1-last=Gopalswamy | editor2-first=S. S. | editor2-last=Hasan | editor3-first=Ashok | editor3-last=Ambastha | publisher=Springer | year=2010 | isbn=978-3-642-11341-3 | page=176 | chapter-url=https://books.google.com/books?id=HI4Gyag2yp4C&pg=PA176 }}</ref> The atmospheric region from the ground through the thermosphere is referred to as the barosphere, since the barometric law holds throughout.<ref>{{cite book | title=Planetary Aeronomy: Atmosphere Environments in Planetary Systems | series=Physics of Earth and Space Environments | first1=Siegfried | last1=Bauer | first2=Helmut | last2=Lammer | publisher=Springer Science & Business Media | year=2013 | isbn=978-3-662-09362-7 | pages=4–5 | url=https://books.google.com/books?id=PXErBAAAQBAJ&pg=PA4 }}</ref>

The outermost layer of a planetary atmosphere is termed the exosphere. Here, the air pressure is so low at this altitude that the distance travelled between molecule collisions, the mean free path, is greater than the atmospheric scale height. In this region, lower mass components with a thermal velocity exceeding the escape velocity can escape into space. For the Earth, the exosphere is at an altitude of 500&nbsp;km, while it is around 210&nbsp;km for Venus and Mars.<ref>{{cite book | chapter=A Comparative Study of the Influence of the Active Young Sun on Early Atmospheres of Earth, Venus, and Mars | display-authors=1 | first1=Y. N. | last1=Yulinov | first2=H. | last2=Lammer | first3=H. I. M. | last3=Lichtenegger | first4=T. | last4=Penz | first5=D. | last5=Breuer | first6=T. | last6=Spohn | first7=R. | last7=Lundin | first8=H. K. | last8=Biernat | title=Geology and Habitability of Terrestrial Planets | volume=24 | series=Space Sciences Series of ISSI | display-editors=1 | editor1-first=Kathryn E. | editor1-last=Fishbaugh | editor2-first=Phillipe | editor2-last=Lognonné | editor3-first=François | editor3-last=Raulin | editor4-first=David J. | editor4-last=Des Marais | editor5-first=Oleg | editor5-last=Korablev | publisher=Springer Science & Business Media | year=2007 | isbn=978-0-387-74288-5 | page=209 | chapter-url=https://books.google.com/books?id=U1iOY_ObZ2UC&pg=PA209 }}</ref> On Earth, the exosphere extends to roughly 10,000&nbsp;km, where it interacts with the magnetosphere of Earth.

All three planets have an ionosphere, which is an ionized region of the upper atmosphere. The ionospheres for Mars and Venus are closer to the surface and are less dense than on the Earth.<ref>{{cite book | title=Space Biology and Medicine | volume=3 | issue=2 | first=Arnauld E. | last=Nicogossian | publisher=AIAA | year=1993 | pages=153–154 | isbn=978-1-56347-061-5 | url=https://books.google.com/books?id=zYGaHX0wNiQC&pg=PA153 }}</ref> The density of the Earth's ionosphere is greater at short distances from the planetary surface in the daytime and decreases as the ionosphere rises at night-time, thereby allowing a greater range of radio frequencies to travel greater distances.

===Gas giants=== Gas giants are primarily composed of hydrogen and helium with traces of other elements, giving the planets a low bulk density. Many of the molecules observed in the outer atmosphere are hydrides, and most of these (with the exception of H₂O and H₂S) are photochemically destroyed by solar UV in the stratosphere of Jupiter and Saturn. These compounds get re-created by thermo-chemical reactions within the hotter, lower regions of the atmosphere.<ref>{{cite book | title=Chemistry of the Solar System | first1=Katharina | last1=Lodders | first2=Bruce | last2=Fegley, Jr | publisher=Royal Society of Chemistry | year=2015 | isbn=978-1-78262-601-5 | url=https://books.google.com/books?id=B3UoDwAAQBAJ&pg=PT290 }}</ref> Complex organic compounds are recycled back to methane by the highly reducing atmosphere.<ref name=McSween_et_al_2022/> The high gravity of these planets combined with their distance from the Sun means that mass loss from their exospheres is negligible, so they form closed systems.<ref>{{cite book | chapter=Photochemistry in Outer Solar System Atmospheres | last=Strobel | first=Darrell F. | title=The Outer Planets and their Moons. Comparative Studies of the Outer Planets prior to the Exploration of the Saturn System by Cassini-Huygens | display-editors=1 | series=Space Sciences Series of ISSI | editor1-last=Encrenaz | editor1-first=T. | editor2-last=Kallenbach | editor2-first=R. | editor3-last=Owen | editor3-first=T. | editor4-last=Sotin | editor4-first=C. | isbn=1-4020-3362-1 | publisher=Springer-Verlag | location=Berlin Heidelberg | pages=155–170 | year=2005 | volume=19 | doi=10.1007/1-4020-4038-5_10 | bibcode=2005opm..book..155S | chapter-url=https://books.google.com/books?id=MbmiTd3x1UcC&pg=PA155 }}</ref>

A common feature of the gas giant planets are cloud layers that form where the combination of temperature and pressure are appropriate for condensing a particular volatile. For Jupiter and Saturn, the outermost cloud layer consists of ice particles of ammonia (NH₃), with an underlying layer of ammonium hydrosulfide (NH₄SH), then a deep layer of water clouds (H₂O). For Uranus and Neptune, the top layer is a methane (CH₄) layer of ice particles, followed by the same cloud layers as Jupiter and Saturn. One difference for Uranus and Neptune is that hydrogen sulfide (H₂S) mixes at the same level as the condensed ammonia.<ref name=Nair_et_al_2008>{{cite book | chapter=Updated Review of Planetary Atmospheric Electricity | display-authors=1 | first1=Y. | last1=Yair | first2=G. | last2=Fischer | first3=F. | last3=Sim&otilde;es | first4=N. | last4=Renno | first5=P. | last5=Zarka | title=Planetary Atmospheric Electricity | volume=30 | series=Space Sciences Series of ISSI | display-editors=1 | editor1-first=François | editor1-last=Leblanc | editor2-first=Karen | editor2-last=Aplin | editor3-first=Yoav | editor3-last=Yair | editor4-first=Giles | editor4-last=Harrison | editor5-first=Jean Pierre | editor5-last=Lebreton | editor6-first=M. | editor6-last=Blanc | publisher=Springer Science & Business Media | year=2008 | isbn=978-0-387-87664-1 | pages=41–42 | chapter-url=https://books.google.com/books?id=maJCAAAAQBAJ&pg=PA42 }}</ref> These cloud layers are optically thick, absorbing light at all wavelengths. The result is a shallower scale height for the outer atmosphere.<ref name=Awiphan_2018/> All four gas giants experience lightning activity in the water clouds, and this is generally much more powerful than terrestrial lightning. Lightning has been observed on Jupiter, but has not been optically detected on Saturn, Uranus, or Neptune most likely because of their depth.<ref name=Nair_et_al_2008/>

All of the gas giants have internal heat sources and radiate more heat than they receive from the Sun.<ref name=James_1995>{{cite book | title=Introduction to Circulating Atmospheres | series=Cambridge Atmospheric and Space Science Series | first=Ian N. | last=James | publisher=Cambridge University Press | year=1995 | isbn=978-0-521-42935-1 | url=https://books.google.com/books?id=bZ2ARhIg--MC&pg=PA344 }}</ref><ref>{{Cite arXiv | title=Internal Heat and Energy Imbalance of Uranus | display-authors=1 | last1=Wang | first1=Xinyue | last2=Li | first2=Liming | last3=Roman | first3=Michael | last4=Zhang | first4=Xi | last5=Jiang | first5=Xun | last6=Fry | first6=Patrick M. | last7=Li | first7=Cheng | last8=Milcareck | first8=Gwenael | last9=Sanchez-Lavega | first9=Agustin | last10=Perez-Hoyos | first10=Santiago | last11=Hueso | first11=Ricardo | last12=Guillot | first12=Tristan | last13=Nixon | first13=Conor A. | last14=Dyudina | first14=Ulyana A. | last15=West | first15=Robert A. | last16=Kenyon | first16=Matthew E. | date=February 2025 | eprint=2502.20722 | class=astro-ph }}</ref> Models for the interiors of Jupiter and Saturn suggest that at a certain depth the hydrogen undergoes a phase change to a metallic hydrogen fluid mixed with ice. There is possibly a diffuse or solid core of more massive elements. For Uranus and Neptune, there is no metallic hydrogen; instead there are interior layers of ice, placing these worlds in the sub-category of ice giants. At sufficient depth, the ice may transition to a supercritical fluid.<ref name=McSween_et_al_2022>{{cite book | title=Cosmochemistry | display-authors=1 | first1=Harry | last1=McSween, Jr | first2=Harry Y. | last2=McSween | first3=Gary | last3=Huss | publisher=Cambridge University Press | year=2022 | isbn=978-1-108-83983-9 | edition=2nd | url=https://books.google.com/books?id=f7hIEAAAQBAJ&pg=PA391 }}</ref>

Within the Solar System, gas giant planets formed beyond the frost line, where the temperature from the young Sun was low enough for volatiles to condense into solid grains. In some star systems, dynamic processes in the protoplanetary disk can cause a gas giant to migrate much closer to the central star, creating a hot Jupiter. A prototype example is 51 Pegasi b. Through gravitational interaction, the orbit of the planet becomes circularized and it is tidally locked into a synchronous rotation with one side constantly facing the star. The heated side becomes swollen, and high velocity winds distribute the thermal energy around the planet. The atmosphere may eventually be stripped away by the star's gravity, leaving behind a super Earth.<ref>{{cite book | title=The Planet Factory: Exoplanets and the Search for a Second Earth | first=Elizabeth | last=Tasker | publisher=Bloomsbury Publishing | year=2017 | isbn=978-1-4729-1775-1 | url=https://books.google.com/books?id=nflQDQAAQBAJ&pg=PA103 }}</ref>

At the upper mass extreme of gas giants is a class of objects known as brown dwarfs. There is no universal consensus on how to distinguish a brown dwarf from a gas giant, although a commonly used criteria is the ability to fuse deuterium at around 13 times the mass of Jupiter.<ref>{{cite journal | title=The Deuterium-burning Mass Limit for Brown Dwarfs and Giant Planets | display-authors=1 | last1=Spiegel | first1=David S. | last2=Burrows | first2=Adam | last3=Milsom | first3=John A. | journal=The Astrophysical Journal | volume=727 | issue=1 | at=id. 57 | date=January 2011 | doi=10.1088/0004-637X/727/1/57 | arxiv=1008.5150 | bibcode=2011ApJ...727...57S }}</ref> Once the initial deuterium burning phase of a brown dwarf is concluded, the internal store of heat gradually makes its way to the surface then is radiated away over time. Convection occurs around the core, and possibly at the surface if the brown dwarf is receiving energy from a nearby star. Radiative energy transfer occurs throughout the remainder of the brown dwarf. Chemistry can occur throughout the atmosphere, which, depending on the chemical species, can change the opacity to radiative energy transfer. As with gas giants, in the cooler outer regions of a brown dwarf, some molecules can condense to form clouds.<ref>{{cite journal | title=On the Cool Side: Modeling the Atmospheres of Brown Dwarfs and Giant Planets | last1=Marley | first1=M. S. | last2=Robinson | first2=T. D. | journal=Annual Review of Astronomy and Astrophysics | volume=53 | pages=279–323 | date=August 2015 | doi=10.1146/annurev-astro-082214-122522 | arxiv=1410.6512 | bibcode=2015ARA&A..53..279M }}</ref>

==Circulation== {{Main|Atmospheric circulation}} [[File:Mars general circulation.png|thumb|Global atmospheric circulation on Mars during solstice|alt=Schematic highlighting key components of the global atmospheric circulation on Mars]]

The circulation of the atmosphere occurs due to thermal differences when convection becomes a more efficient transporter of heat than thermal radiation. On planets where the primary heat source is solar radiation, excess heat in the tropics is transported to higher latitudes.<ref name=Martin_2016>{{cite book | title=Earth's Evolving Systems | first=Ronald | last=Martin | publisher=Jones & Bartlett Learning | year=2016 | isbn=978-1-284-10829-3 | pages=66–69 | edition=2nd | url=https://books.google.com/books?id=mymjDQAAQBAJ&pg=PA69 }}</ref> When a planet generates a significant amount of heat internally, such as is the case for Jupiter, convection in the atmosphere can transport thermal energy from the higher temperature interior up to the surface.<ref>{{cite journal | title=Jupiter's Interior as Revealed by Juno | last=Stevenson | first=David J. | journal=Annual Review of Earth and Planetary Sciences | volume=48 | pages=465–489 | date=May 2020 | doi=10.1146/annurev-earth-081619-052855 | bibcode=2020AREPS..48..465S }}</ref>

The thermally-driven meridional circulation of Earth, Mars, and Venus are dominated by the Hadley cell. This is created by rising air in the warmest region of the planet accompanied by descending air where it is cooler. However, there are significant differences in the circulation patterns between the three planets. For Venus, the lower atmosphere of Venus has two symmetrical equator to near pole circulation cells, with a higher altitude sub-solar to anti-solar circulation cell. On Earth, Hadley cells exist on each side of the equator, but these vary seasonally due to the planet's obliquity. Mars is similar to the Earth in this respect, but it displays greater seasonality due to its thinner atmosphere. It has two Hadley cells during equinox, but a single cell at solstice.<ref>{{cite journal | title=An Axisymmetric Limit for the Width of the Hadley Cell on Planets With Large Obliquity and Long Seasonality | last1=Guendelman | first1=I. | last2=Kaspi | first2=Y. | journal=Geophysical Research Letters | volume=45 | issue=24 | pages=13,213–13,221 | date=December 2018 | doi=10.1029/2018GL080752 | arxiv=1903.11656 | bibcode=2018GeoRL..4513213G }}</ref><ref>{{cite web | title=General circulation in Venus' atmosphere | first=R. | last=Hueso | publisher=ESA | date=November 26, 2007 | url=https://www.esa.int/ESA_Multimedia/Images/2007/11/General_circulation_in_Venus_atmosphere | access-date=2025-08-20 }}</ref>

The Earth has multiple counter-rotating convection cells, with the Hadley cell on either side of the equator, an intermediate Ferrel cell along the mid-latitudes, and polar cells at each pole. The planet's rotation induces a Coriolis force that creates a curvature in the north-south convection flow. As air moves toward a pole, the latitudinal flow remains steady but the distance needed to encircle the planet grows shorter, creating a curved path along the surface. These flows create the prevailing winds along the planet's surface. Near the equator, the air flow creates the trade winds which flow from east to west. At the mid-latitudes, the westerlies brings the air flow from the west in the United States and Europe. Finally, the polar easterlies moves polar air from east to west.<ref name=Martin_2016/>

Both Jupiter and Saturn display banded cloud formations. These are associated with alternating jets known as zonal flows that follow latitudinal lines. The bands alternate in direction, with the equatorial jet moving eastward at {{Val|150|u=km/s}} on Jupiter and {{Val|300|u=km/s}} on Saturn. It remains unclear whether these flows occur in the shallow layers around the clouds, or extend much deeper into the atmosphere.<ref>{{cite book | title=The Liquid and Supercritical Fluid States of Matter | first=John E. | last=Proctor | publisher=CRC Press | year=2020 | isbn=978-0-429-95791-8 | url=https://books.google.com/books?id=1Bj0DwAAQBAJ&pg=PT262 }}</ref> Observations of Neptune show a similar zonal flow structure. This planet displays the largest range of differential rotation in the Solar System.<ref>{{cite book | chapter=The Interior of Neptune | display-authors=1 | first1=W. B. | last1=Hubbard | first2=M. | last2=Podolak | first3=D. J. | last3=Stevenson | title=Neptune and Triton | series=Space science series | display-editors=1 | editor1-first=Dale P. | editor1-last=Cruikshank | editor2-first=Mildred Shapley | editor2-last=Matthews | editor3-first=A. M. | editor3-last=Schumann | publisher=University of Arizona Press | year=1995 | isbn=978-0-8165-1525-7 | page=131 | chapter-url=https://books.google.com/books?id=My8J0G3R1-4C&pg=PA131 }}</ref>

==Escape== {{Main|Atmospheric escape}} Surface gravity differs significantly among the planets. For example, the large gravitational force of the giant planet Jupiter retains light gases such as hydrogen and helium that escape from objects with lower gravity. Secondly, the distance from the Sun determines the energy available to heat atmospheric gas to the point where some fraction of its molecules' thermal motion exceed the planet's escape velocity, allowing those to escape a planet's gravitational grasp. Thus, distant and cold Titan, Triton, and Pluto are able to retain components of their original atmospheres despite their relatively low gravities.<ref>{{cite book | title=Photochemistry of Planetary Atmospheres | first1=Yuk Ling | last1=Yung | first2=William B. | last2=DeMore | publisher=Oxford University Press | year=1999 | isbn=978-0-19-510501-8 | pages=13–16 | url=https://books.google.com/books?id=FY3mCwAAQBAJ&pg=PA16 }}</ref>

Since a collection of gas molecules may be moving at a wide range of velocities, there will always be some fast enough to produce a slow leakage of gas into space. Lighter molecules move faster than heavier ones with the same thermal kinetic energy, and so gases of low molecular weight are lost more rapidly than those of high molecular weight. It is thought that Venus and Mars may have lost much of their water when, after being photodissociated into hydrogen and oxygen by solar ultraviolet radiation, the hydrogen escaped. Earth's magnetic field helps to prevent this, as, normally, the solar wind would greatly enhance the escape of hydrogen. However, over the past 3 billion years Earth may have lost gases through the magnetic polar regions due to auroral activity, including a net 2% of its atmospheric oxygen.<ref name="seki2001"/> The net effect, taking the most important escape processes into account, is that an intrinsic magnetic field does not protect a planet from atmospheric escape and that for some magnetizations the presence of a magnetic field works to increase the escape rate.<ref name="gunell2018"/>

Planets around small M-type main-sequence stars may be particularly prone to atmospheric loss. The star will spend an extended period as a superluminous pre-main-sequence star, then experience high levels of activity. The strong stellar magnetic field will tend to reduce the size of planetary magnetospheres, leading to greater erosion from the stellar wind. Planets around older M-type stars may become tidally locked in synchronous orbit, leading to the atmosphere being permanently frozen on the dark face.<ref name=Kopparapu_et_al_2020>{{cite book | chapter=Characterizing Exoplanet Habitability | display-authors=1 | first1=R. K. | last1=Kopparapu | first2=E. T. | last2=Wolf | first3=V. S. | last3=Meadows | title=Planetary Astrobiology | display-editors=1 | editor1-first=Victoria | editor1-last=Meadows | editor2-first=Giada | editor2-last=Arney | editor3-first=Britney | editor3-last=Schmidt | editor4-first=David J. Des | editor4-last=Marais | publisher=University of Arizona Press | year=2020 | isbn=978-0-8165-4065-5 | pages=461–464 | chapter-url=https://books.google.com/books?id=08fcDwAAQBAJ&pg=PA464 }}</ref>

Other mechanisms that can cause atmosphere depletion are solar wind-induced sputtering, impact erosion, weathering,<ref>{{cite book | title=Principles of Planetary Climate | first=Raymond T. | last=Pierrehumbert | publisher=Cambridge University Press | year=2010 | isbn=978-1-139-49506-6 | pages=9–10 | url=https://books.google.com/books?id=bO_U8f5pVR8C&pg=PA10 }}</ref> and sequestration—sometimes referred to as "freezing out"—into the regolith and polar caps.<ref>{{cite journal | title=Nitrogen Loss from Pluto's Birth to the Present Day via Atmospheric Escape, Photochemical Destruction, and Impact Erosion | display-authors=1 | last1=Johnson | first1=Perianne E. | last2=Young | first2=Leslie A. | last3=Nesvorný | first3=David | last4=Zhang | first4=Xi | journal=The Planetary Science Journal | volume=5 | issue=8 | at=id. 170 | date=August 2024 | doi=10.3847/PSJ/ad5e80 | doi-access=free | arxiv=2408.00625 | bibcode=2024PSJ.....5..170J }}</ref><ref>{{cite journal | title=The formation and stability of buried polar CO₂ deposits on Mars | display-authors=1 | last1=Manning | first1=Curtis V. | last2=Bierson | first2=Carver | last3=Putzig | first3=Nathaniel E. | last4=McKay | first4=Christopher P. | journal=Icarus | volume=317 | pages=509–517 | date=January 2019 | doi=10.1016/j.icarus.2018.07.021 | bibcode=2019Icar..317..509M }}</ref> An extreme example of the latter is a comet, which is a small body that forms beyond the frost line in the protoplanetary disk. These objects contain many types of frozen volatiles, including water, carbon dioxide, ammonia, methane, and formaldehyde. As these objects approach the Sun, the thermal radiation causes the volatiles to sublimate, creating a diffuse, dusty atmosphere around the comet; the coma. However, the gravitational potential of the comet is insufficient to retain this atmosphere.<ref>{{cite journal | title=Organic Molecules and Volatiles in Comets | display-authors=1 | last1=Yabuta | first1=Hikaru | last2=Sandford | first2=Scott A. | last3=Meech | first3=Karen J. | journal=Elements | volume=14 | issue=2 | pages=101–106 | date=April 2018 | doi=10.2138/gselements.14.2.101 | bibcode=2018Eleme..14..101Y }}</ref>

The Solar System contains a large number of bodies that are now practically airless, such as Mercury and the Moon. These objects have only an exosphere layer with particles that are essentially collisionless. In this environment, atoms and molecules are released from the surface by various means, including particle sputtering and micrometeorite impact. When the release velocity of these particles exceed the escape velocity, they are lost to space. Higher mass particles have a greater chance to be returned to the surface, which creates a chemical alteration of the surface over time.<ref name=Lammer_et_al_2022>{{cite journal | title=The Exosphere as a Boundary: Origin and Evolution of Airless Bodies in the Inner Solar System and Beyond Including Planets with Silicate Atmospheres | display-authors=1 | last1=Lammer | first1=Helmut | last2=Scherf | first2=Manuel | last3=Ito | first3=Yuichi | last4=Mura | first4=Alessandro | last5=Vorburger | first5=Audrey | last6=Guenther | first6=Eike | last7=Wurz | first7=Peter | last8=Erkaev | first8=Nikolai V. | last9=Odert | first9=Petra | journal=Space Science Reviews | volume=218 | issue=3 | at=id. 15 | date=April 2022 | doi=10.1007/s11214-022-00876-5 | arxiv=2203.01656 | bibcode=2022SSRv..218...15L }}</ref>

== Terrain == On a terrestrial planet, the part of the atmosphere that directly interacts with the ground is known as the planetary boundary layer. Atmospheres have dramatic effects on the surfaces of rocky bodies. Wind erosion is a significant factor in shaping the terrain of rocky planets with atmospheres,<ref>{{cite book | title=Introduction to Planetary Geomorphology | first=Ronald | last=Greeley | publisher=Cambridge University Press | year=2013 | isbn=978-0-521-86711-5 | pages=54–55 | url=https://books.google.com/books?id=fZwNNP-IzicC&pg=PA54 }}</ref> and over time can erase the effects of both craters and volcanoes. In addition, since liquids cannot exist without pressure, an atmosphere allows liquid to be present at the surface, resulting in lakes, rivers and oceans.<ref name=Kopparapu_et_al_2020/> Earth and Titan are known to have liquids at their surface and terrain on the planet Mars suggests that it had liquid on its surface in the past.

Objects that have no atmosphere, or that have only an exosphere, have terrain that is covered in craters. Without an atmosphere, the planet has no protection from meteoroids, and all of them collide with the surface as meteorites and create craters. For planets with a significant atmosphere, most meteoroids burn up as meteors before hitting a planet's surface. When meteoroids do impact, the effects are often erased by the action of wind.<ref name="forbesmeteor"/>

==Fields of study== From the perspective of a planetary geologist, the atmosphere acts to shape a planetary surface. Wind picks up dust and other particles which, when they collide with the terrain, erode the relief and leave deposits (eolian processes). Frost and precipitations, which depend on the atmospheric composition, also influence the relief. Climate changes can influence a planet's geological history. Conversely, studying the surface of the Earth leads to an understanding of the atmosphere and climate of other planets.<ref>{{cite book | title=Planetary Geology: An Introduction | first1=Dominic | last1=Fortes | first2=Claudio | last2=Vita-Finzi | edition=3rd | publisher=Liverpool University Press | year=2025 | isbn=978-1-78046-110-6 | url=https://books.google.com/books?id=kVtHEQAAQBAJ&pg=PA184 }}</ref>

For a meteorologist, the composition of the Earth's atmosphere is a factor affecting the climate and its variations.<ref>{{cite book | title=Lectures in Meteorology | series=Springer Atmospheric Sciences | first1=Nicole | last1=Mölders | first2=Gerhard | last2=Kramm | publisher=Springer | year=2014 | isbn=978-3-319-02144-7 | url=https://books.google.com/books?id=nWr1AwAAQBAJ&pg=PA1 }}</ref>

For a biologist or paleontologist, the Earth's atmospheric composition is closely dependent on the appearance of life and its evolution. In astrobiology, the composition of an exoplanet's atmosphere is closely intertwined with the possibility of extraterrestrial life.<ref>{{cite book | chapter=Astrobiology | first=Vera M. | last=Kolb | title=Handbook of Astrobiology | editor-first=Vera M. | editor-last=Kolb | publisher=CRC Press | year=2018 | isbn=978-1-351-66110-2 | chapter-url=https://books.google.com/books?id=wah8DwAAQBAJ&pg=PT27 }}</ref>

==See also== {{Portal|Weather}} * Atmometer (evaporimeter) * Atmospheric pressure * Cosmic shoreline * Extraterrestrial atmosphere * International Standard Atmosphere * Kármán line * Sky

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==External links== {{Commons category}} *[https://web.archive.org/web/20090421144658/http://www.allstar.fiu.edu/aero/fltenv2.htm Properties of atmospheric strata – The flight environment of the atmosphere] *[https://mappingaround.in/atmosphere-everything-you-need-to-know/ Atmosphere – Everything you need to know]

{{Atmospheres}} {{Authority control}}

Category:Atmosphere Category:Gases Category:Planetary science