| Revision as of 20:59, 4 June 2024 editArkHyena (talk | contribs)Extended confirmed users7,029 edits →Cryomagma composition← Previous edit | Revision as of 21:38, 16 November 2024 edit undoArkHyena (talk | contribs)Extended confirmed users7,029 edits →Enceladus: convertNext edit → | ||
| (25 intermediate revisions by 7 users not shown) | |||
| Line 9: | Line 9: | ||
| Although rare in the inner ], past and recent cryovolcanism is common on ]s in the outer Solar System, especially on the icy moons of the ]s and potentially amongst the ]s as well. As such, cryovolcanism is important to the geological histories of these worlds, constructing landforms or even resurfacing entire regions. Despite this, only a few eruptions have ever been observed in the Solar System. The sporadic nature of direct observations means that the true number of extant cryovolcanoes is contentious. | Although rare in the inner ], past and recent cryovolcanism is common on ]s in the outer Solar System, especially on the icy moons of the ]s and potentially amongst the ]s as well. As such, cryovolcanism is important to the geological histories of these worlds, constructing landforms or even resurfacing entire regions. Despite this, only a few eruptions have ever been observed in the Solar System. The sporadic nature of direct observations means that the true number of extant cryovolcanoes is contentious. | ||
| Like ] on the ]s, cryovolcanism is driven by escaping internal heat, often supplied by extensive ] in the case of the moons of the giant planets. However, isolated dwarf planets are capable of retaining enough internal heat from formation and radioactive decay to drive cryovolcanism on their own, an observation which has been supported by both in situ and distant observations. | Like ] on the ]s, cryovolcanism is driven by escaping ] from within a celestial object, often supplied by extensive ] in the case of the moons of the giant planets. However, isolated dwarf planets are capable of retaining enough internal heat from formation and ] to drive cryovolcanism on their own, an observation which has been supported by both in situ observations by spacecraft and distant observations by telescopes. | ||
| == Etymology and terminology == | == Etymology and terminology == | ||
| The term <em>cryovolcano</em> was coined by Steven K. Croft in a 1987 conference abstract at the Geological Society of America Abstract with Programs. The term is ultimately a combination of cryo-, from the ] ''κρῠ́ος'' (''krúos'', meaning cold or frost), and volcano.<ref name="kryos"/><ref name="PlanetaryLandforms"/>{{rp|492}} In general, terminology used to describe cryovolcanism is analogous to volcanic terminology: | The term <em>cryovolcano</em> was coined by Steven K. Croft in a 1987 conference abstract at the ] (GSA) Abstract with Programs. The term is ultimately a combination of cryo-, from the ] ''κρῠ́ος'' (''krúos'', meaning cold or frost), and volcano.<ref name="kryos"/><ref name="PlanetaryLandforms"/>{{rp|492}} In general, terminology used to describe cryovolcanism is analogous to volcanic terminology: | ||
| * <em>Cryolava</em> and <em>cryomagma</em> are distinguished in a manner similar to ] and ]. Cryomagma refers to the molten or partially molten material beneath a body's surface, where it may then erupt onto the surface. If the material is still fluid, it is classified as cryolava, which can flow in <em>cryolava channels</em>, analogs to ]s. Explosive eruptions, however, may pulverize the material into |
* <em>Cryolava</em> and <em>cryomagma</em> are distinguished in a manner similar to ] and ]. Cryomagma refers to the molten or partially molten material beneath a body's surface, where it may then erupt onto the surface. If the material is still fluid, it is classified as cryolava, which can flow in <em>cryolava channels</em>, analogs to ]s. Explosive eruptions, however, may pulverize the material into a fine "]" termed <em>cryoclastic material</em>.<ref name="gregg2021"/>{{rp|page=161–162}}<ref name="geissler2015"/>{{rp|page=768}} Cryoclastic material flowing downhill produces <em>cryoclastic flows</em>, analogs to ]s.<ref name="Fortes2007"/>{{rp|149}} | ||
| * A <em>cryovolcanic edifice</em> is a landform constructed by cryovolcanic eruptions. These may take the form of shields (analogous to terrestrial ]es),<ref name="PlanetaryLandforms"/>{{rp|487}} cones (analogous to ]s and ]s),<ref name="CroftSK1995"/>{{rp|922}} or domes (analogous to ]s).<ref name="Schenk2018"/>{{rp|431}} Cryovolcanic edifices may support |
* A <em>cryovolcanic edifice</em> is a landform constructed by cryovolcanic eruptions. These may take the form of shields (analogous to terrestrial ]es),<ref name="PlanetaryLandforms"/>{{rp|487}} cones (analogous to ]s and ]s),<ref name="CroftSK1995"/>{{rp|922}} or domes (analogous to ]s).<ref name="Schenk2018"/>{{rp|431}} Cryovolcanic edifices may support secondary landforms, such as ]-like collapse structures, cryovolcanic flow channels (analogous to lava flow features), and cryovolcanic fields and plains (analogous to ]).<ref name="PlanetaryLandforms"/>{{rp|487}} | ||
| As cryovolcanism largely takes place on icy worlds, the term <em>ice volcano</em> is sometimes used colloquially.<ref name="IceVolcano"/> | As cryovolcanism largely takes place on icy worlds, the term <em>ice volcano</em> is sometimes used colloquially.<ref name="IceVolcano"/> | ||
| Line 44: | Line 44: | ||
| {{Further information|Planetary oceanography}} | {{Further information|Planetary oceanography}} | ||
| ] | ] | ||
| Cryovolcanism implies the generation of large volumes of molten fluid in the interiors of icy worlds. A primary reservoir of such fluid are subsurface oceans.<ref name="gregg2021"/>{{rp|page=167}} Subsurface oceans are widespread amongst the icy satellites of the ]s<ref name="gregg2021"/>{{rp|page=167}} and are largely maintained by ], where the moon's |
Cryovolcanism implies the generation of large volumes of molten fluid in the interiors of icy worlds. A primary reservoir of such fluid are subsurface oceans.<ref name="gregg2021"/>{{rp|page=167}} Subsurface oceans are widespread amongst the icy satellites of the ]s<ref name="gregg2021"/>{{rp|page=167}} and are largely maintained by ], where the moon's slightly ] orbit allows the rocky core to dissipate energy and generate heat.<ref name="ucsc.2008"/>{{rp|675}} Evidence for subsurface oceans also exist for the ]s ]<ref name="mcogvern2024"/> and, to a lesser extent, ],<ref name="mccord.2005"/><ref name="cr.ceres"/> ], ],<ref name="glein2024"/>{{rp|8}} ], ], and ].<ref name=Emery2024/>{{rp|8}} In the case of Pluto and the other dwarf planets, there is comparatively little, if any, long-term tidal heating. Thus, heating must largely be self-generated, primarily coming from the decay of ] in their rocky cores.<ref name="gregg2021"/>{{rp|page=171}} | ||
| Reservoirs of cryomagma can hypothetically form within the shell of an icy world as well, either from direct localized melting or the injection of cryomagma from a deeper subsurface ocean. A convective layer in the ice shell can generate warm plumes that spread laterally at the base of the brittle icy crust. The intruding warm ice can melt impure ice, forming a lens-shaped region of melting.<ref name="schmidt2011"/><ref name="gregg2021"/>{{rp|page=173}} Other methods of producing localized melts include the buildup of stress within ], where friction may be able to generate enough heat to melt ice; and impact events that violently heat the impact site.<ref name="gregg2021"/>{{rp|page=174}} Intrusive models, meanwhile, propose that a deeper subsurface ocean directly injects cryomagma through fractures in the ice shell, much like volcanic ] and ] systems.<ref name="gregg2021"/>{{rp|page=173–174}} | Reservoirs of cryomagma can hypothetically form within the shell of an icy world as well, either from direct localized melting or the injection of cryomagma from a deeper subsurface ocean. A convective layer in the ice shell can generate warm plumes that spread laterally at the base of the brittle icy crust. The intruding warm ice can melt impure ice, forming a lens-shaped region of melting.<ref name="schmidt2011"/><ref name="gregg2021"/>{{rp|page=173}} Other proposed methods of producing localized melts include the buildup of stress within ], where friction may be able to generate enough heat to melt ice; and impact events that violently heat the impact site.<ref name="gregg2021"/>{{rp|page=174}} Intrusive models, meanwhile, propose that a deeper subsurface ocean directly injects cryomagma through fractures in the ice shell, much like volcanic ] and ] systems.<ref name="gregg2021"/>{{rp|page=173–174}} | ||
| == Cryomagma composition == | == Cryomagma composition == | ||
| Line 81: | Line 81: | ||
| {{main|Ceres (dwarf planet)#Cryovolcanism}} | {{main|Ceres (dwarf planet)#Cryovolcanism}} | ||
| ] impact basin on Ceres, with ] at center]] | ] impact basin on Ceres, with ] at center]] | ||
| ] |
] is the innermost object in the Solar System known to be cryovolcanically active. Upon the arrival of the '']'' orbiter in March 2015,<ref name="NASA-20150306"/> the dwarf planet was discovered to have numerous ] (designated as ''faculae'') located within several major impact basins, most prominently in the center of ]. These bright spots are composed primarily of various salts, and are hypothesized to have formed from impact-induced upwelling of subsurface material that erupt brine to Ceres's surface. The distribution of hydrated ] on one particular bright spot, ], indicates that the upwelling occurred recently or is currently ongoing. That brine exists in Ceres's interior implies that salts played a role in keeping Ceres's subsurface ocean liquid, potentially even to the present day.<ref name="desanctis2020"/>{{rp|786}} ''Dawn'' also discovered ] and ] (formerly Ysolos Mons), two prominent isolated mountains which are likely young cryovolcanic domes.<ref name="sori2021"/><ref name="gregg2021"/>{{rp|page=213,215}} It is expected that cryovolcanic domes eventually subside after becoming extinct due to viscous relaxation, flattening them. This would explain why Ahuna Mons appears to be the most prominent construct on Ceres, despite its geologically young age.<ref name="sori2021"/> | ||
| === Europa === | === Europa === | ||
| Line 97: | Line 97: | ||
| {{further|Rings of Saturn#E Ring}} | {{further|Rings of Saturn#E Ring}} | ||
| ] | ] | ||
| ]'s moon Enceladus is host to the most dramatic example of cryovolcanism yet observed, with a series of vents erupting 250 |
]'s moon Enceladus is host to the most dramatic example of cryovolcanism yet observed, with a series of vents erupting {{convert|250|kg|lb}} of material per second that feeds Saturn's ].<ref name="rain"/><ref name="Spahn2006"/> These eruptions take place across Enceladus's south polar region, sourced from four major ridges which form a region informally known as the ].<ref name="Porco2006"/> Enceladus's cryovolcanic activity is sustained by a global subsurface ocean.<ref name="thomas2015"/><ref name="Berne2024">{{cite journal| last1=Berne|first1=A.| last2=Simons| first2=M. | last3=Keane| first3=J.T. | last4=Leonard| first4=E.J.| last5=Park| first5=R.S.| title=Jet activity on Enceladus linked to tidally driven strike-slip motion along tiger stripes| journal=Nature Geoscience| issn=1752-0908|doi=10.1038/s41561-024-01418-0| pages = 385–391|date=April 29, 2024|volume=17 |issue=5 |bibcode=2024NatGe..17..385B }}</ref> | ||
| Other regions centered on Enceladus's leading and trailing hemispheres—the hemispheres that "face" towards or against the direction of Enceladus's orbit—exhibit similar terrain to that of the Tiger Stripes, possibly indicating that Enceladus has experienced discrete periods of heightened cryovolcanism in the past.<ref name="thomas2015"/>{{rp|42}} | Other regions centered on Enceladus's leading and trailing hemispheres—the hemispheres that "face" towards or against the direction of Enceladus's orbit—exhibit similar terrain to that of the Tiger Stripes, possibly indicating that Enceladus has experienced discrete periods of heightened cryovolcanism in the past.<ref name="thomas2015"/>{{rp|42}} | ||
| Line 106: | Line 106: | ||
| === Uranian moons === | === Uranian moons === | ||
| On 24 January 1986, ] and its ] |
On 24 January 1986, ] and its ] were explored for the first time by the ''Voyager 2'' spacecraft.<ref name="NASAV2"/> Of Uranus's five major satellites, ] and ] appear to have unusually youthful surfaces indicative of relatively recent activity. Miranda in particular has extraordinarily varied terrain, with striking angular features known as the '']'' cutting across older terrain. ] is located near Miranda's south pole and is estimated to be less than 1 billion years old,<ref name="leonard2022"/> and broad similarities between Miranda's coronae and Enceladus's south polar region have been noted. These characteristics have led to several teams of researchers to propose a cryovolcanic origin of the coronae, where eruptions of viscous cryomagma form the structures with some tectonic involvement.<ref name="schenkmoore2020"/>{{rp|11}} Ariel also exhibits widespread resurfacing, with large polygonal crustal blocks divided by large canyons (''chasmata'') with floors as young as ~0.8 ± 0.5 billion years old, while relatively flat plains may have been the site of large flood eruptions.<ref name="schenkmoore2020"/>{{rp|9–10}} | ||
| Evidence for relatively recent cryovolcanism on the other three round moons of Uranus is less clear. ] hosts large chasms but does not show any clear evidence of cryovolcanism.<ref name="schenkmoore2020"/>{{rp|6}} ] has a massive ~{{convert|11|km|mi|abbr=on}} high mountain that was observed on its limb at the time of ''Voyager 2''{{'}}s flyby; the precise origins of the mountain is unclear, but it may be of cryovolcanic origin.<ref name="schenkmoore2020"/>{{rp|4}} | Evidence for relatively recent cryovolcanism on the other three round moons of Uranus is less clear. ] hosts large chasms but does not show any clear evidence of cryovolcanism.<ref name="schenkmoore2020"/>{{rp|6}} ] has a massive ~{{convert|11|km|mi|abbr=on}} high mountain that was observed on its limb at the time of ''Voyager 2''{{'}}s flyby; the precise origins of the mountain is unclear, but it may be of cryovolcanic origin.<ref name="schenkmoore2020"/>{{rp|4}} | ||
| Line 112: | Line 112: | ||
| === Triton === | === Triton === | ||
| {{main|Geology of Triton#Cryovolcanism}} | {{main|Geology of Triton#Cryovolcanism}} | ||
| ] and its largest moon ] |
] and its largest moon ] were explored by the ''Voyager 2'' spacecraft on 25 August 1989,<ref name="NASAV2"/> revealing Triton's surface features up close for the first time.<ref name="sulcanese2023"/> With an estimated average surface age of 10–100 million years old, with some regions possibly being only a few million years old, Triton is one of the most geologically active worlds in the Solar System.<ref name="Schenk2007"/> Large-scale cryovolcanic landforms have been identified on Triton's young surface, with nearly all of Triton's observed surface features likely related to cryovolcanism.<ref name="CroftSK1995"/>{{rp|919}} One of Triton's major cryovolcanic features, ], the apparent primary vent of the Cipango Planum cryovolcanic plateau which is one of the largest volcanic or cryovolcanic edifices in the Solar System.<ref name="martin-herrero2018"/><ref name="schenk2021"/>{{efn|Using an estimated surface area of at least 490,000 km<sup>2</sup> for Cipango Planum,<ref name="schenk2021"/> this significantly surpasses ]'s area of roughly 300,000 km<sup>2</sup>.<ref name="Frankel2005"/> As Cipango Planum extended beyond Triton's ] during '']''{{'}}s closest approach, its true extent is uncertain and may be significantly larger}} | ||
| Triton hosts four walled plains: ] and ] form a northern pair, and Sipapu Planitia and Ryugu Planitia form a southern pair. The walled plains are characterized by crenulated, irregularly-shaped cliffs that enclose a flat, young plain with a single group of pits and mounds.<ref name="CroftSK1995"/>{{rp|886|894}} The walled plains are likely young cryovolcanic lakes and may represent Triton's youngest cryovolcanic features.<ref name="CroftSK1995"/>{{rp|920–921}}<ref name="mckinnon2014"/>{{rp|page=870; 872}} The regions around Ruach and Tuonela feature additional smaller subcircular depressions, some of which are partially bordered by walls and scarps. In 2014, a team of planetary scientists interpreted these depressions as diapirs, caldera collapse structures, or impact craters filled in by cryolava flows.<ref name="martin-herrero2014"/> To the south of Tuonela Planitia, isolated conical hills with central depressions have been noted as resembling terrestrial cinder cones, possibly pointing to cryovolcanic activity beyond Tuonela Planitia's plains.<ref name="CroftSK1995"/>{{rp|922}} | Triton hosts four walled plains: ] and ] form a northern pair, and Sipapu Planitia and Ryugu Planitia form a southern pair. The walled plains are characterized by crenulated, irregularly-shaped cliffs that enclose a flat, young plain with a single group of pits and mounds.<ref name="CroftSK1995"/>{{rp|886|894}} The walled plains are likely young cryovolcanic lakes and may represent Triton's youngest cryovolcanic features.<ref name="CroftSK1995"/>{{rp|920–921}}<ref name="mckinnon2014"/>{{rp|page=870; 872}} The regions around Ruach and Tuonela feature additional smaller subcircular depressions, some of which are partially bordered by walls and scarps. In 2014, a team of planetary scientists interpreted these depressions as diapirs, caldera collapse structures, or impact craters filled in by cryolava flows.<ref name="martin-herrero2014"/> To the south of Tuonela Planitia, isolated conical hills with central depressions have been noted as resembling terrestrial cinder cones, possibly pointing to cryovolcanic activity beyond Tuonela Planitia's plains.<ref name="CroftSK1995"/>{{rp|922}} | ||
| Line 121: | Line 121: | ||
| {{main|Geology of Pluto|Geology of Charon}} | {{main|Geology of Pluto|Geology of Charon}} | ||
| ], a likely cryovolcano on ]. Coleman Mons can be seen just southwest of Wright Mons]] | ], a likely cryovolcano on ]. Coleman Mons can be seen just southwest of Wright Mons]] | ||
| The dwarf planet ] and its ] |
The dwarf planet ] and its ] were explored by the '']'' spacecraft in a ] on 14 July 2015, observing their surface features in detail for the first time.<ref name="NHEncounter"/> The surface of Pluto varies dramatically in age, and several regions appear to display relatively recent cryovolcanic activity. The most reliably identified cryovolcanic structures are ] and ], two large mountains with central depressions which have led to hypotheses that they may be cryovolcanoes with peak calderas.<ref name = "News2015-11-09"/><ref name = "Witze2015-11-09"/> The two mountains are surrounded by an unusual region of hilly "hummocky terrain", and the lack of distinct flow features have led to an alternative proposal in 2022 by a team of researchers that the structures may instead be formed by sequential dome-forming eruptions, with nearby Coleman Mons being a smaller independent dome.<ref name="singer2022"/> | ||
| Virgil Fossae, a large fault within ], may also represent another site of cryovolcanism on Pluto. An estimated {{convert|300|km|mi|abbr=off}} of Virgil Fossae's western section was likely the site of a fountaining eruption, spewing and dispersing material that covered surrounding terrain up to {{convert|200|km|mi|abbr=off}} away.<ref name="cruikshank2019"/>{{rp|166}} More recently, in 2021 Hekla Cavus was hypothesized to have formed from a cryovolcanic collapse by a team of two researchers, C. J. Ahrens and V. F. Chevrier.<ref name="ahrens2021"/>{{rp|7}} Similarly, in 2021 a team of planetary scientists led by A. Emran proposed that Kiladze, a feature that is formally classified as an impact crater, is actually a cryovolcanic caldera complex.<ref name="emran2023"/> | Virgil Fossae, a large fault within ], may also represent another site of cryovolcanism on Pluto. An estimated {{convert|300|km|mi|abbr=off}} of Virgil Fossae's western section was likely the site of a fountaining eruption, spewing and dispersing material that covered surrounding terrain up to {{convert|200|km|mi|abbr=off}} away.<ref name="cruikshank2019"/>{{rp|166}} More recently, in 2021 Hekla Cavus was hypothesized to have formed from a cryovolcanic collapse by a team of two researchers, C. J. Ahrens and V. F. Chevrier.<ref name="ahrens2021"/>{{rp|7}} Similarly, in 2021 a team of planetary scientists led by A. Emran proposed that Kiladze, a feature that is formally classified as an impact crater, is actually a cryovolcanic caldera complex.<ref name="emran2023"/> | ||
| Line 130: | Line 130: | ||
| === Other dwarf planets === | === Other dwarf planets === | ||
| In 2022, low-resolution near-infrared (0.7–5 μm) ] observations by the ] (JWST) detected light hydrocarbons and complex organic molecules on the surfaces of the dwarf planets ], ], and ]. The detection indicated that all three have experienced internal melting and planetary differentiation in their pasts. The presence of volatiles on their surfaces indicates that cryovolcanism may be resupplying methane.<ref name=Emery2024/>{{rp|13}} JWST spectral observations of ] and ] revealed that hydrogen-deuterium and carbon isotopic ratios indicated that both dwarf planets are actively replenishing surface methane as well, possibly with the presence of a subsurface ocean.<ref name="glein2024"/>{{rp|8}} | In 2022, low-resolution near-infrared (0.7–5 μm) ] observations by the ] (JWST) detected light hydrocarbons and complex organic molecules on the surfaces of the dwarf planets ], ], and ]. The detection indicated that all three have experienced internal melting and planetary differentiation in their pasts. The presence of volatiles on their surfaces indicates that cryovolcanism may be resupplying methane.<ref name=Emery2024/>{{rp|13}} JWST spectral observations of ] and ] revealed that hydrogen-deuterium and carbon isotopic ratios indicated that both dwarf planets are actively replenishing surface methane as well, possibly with the presence of a subsurface ocean.<ref name="glein2024"/>{{rp|8}} | ||
| These observations, combined with the discoveries in the Pluto system by the ''New Horizons'' spacecraft, indicate that icy worlds are capable of sustaining enough heat on their own to drive cryovolcanic activity. In contrast to the icy satellites of the giant planets, where many benefit from extensive tidal heating from their parent planets, the dwarf planets must rely on heat generated primarily or almost entirely by themselves. Leftover primordial heat from formation and radiogenic heat from the decay of ] in their rocky cores likely serve as primary sources of heat. The ] of rocky material or tidal heating from interactions with their satellites |
These observations, combined with the discoveries in the Pluto system by the ''New Horizons'' spacecraft, indicate that icy worlds are capable of sustaining enough heat on their own to drive cryovolcanic activity. In contrast to the icy satellites of the giant planets, where many benefit from extensive tidal heating from their parent planets, the dwarf planets must rely on heat generated primarily or almost entirely by themselves. Leftover primordial heat from formation and radiogenic heat from the decay of ] in their rocky cores likely serve as primary sources of heat. The ] of rocky material or tidal heating from interactions with their satellites.<ref name="naturepluto"/><ref name=Emery2024/>{{rp|8}}<ref name="Saxena2018"/>{{rp|245}} | ||
| == Gallery == | == Gallery == | ||
| Line 176: | Line 176: | ||
| <ref name="Patterson2009">{{cite journal |last1=Patterson |first1=G. Wesley |last2=Collins |first2=Geoffrey C. |last3=Head |first3=James W. |last4=Pappalardo |first4=Robert T. |last5=Prockter |first5=Louise M. |last6=Lucchitta |first6=Baerbel K. |last7=Kay |first7=Jonothan P. |title=Global geological mapping of Ganymede |date=6 December 2009 |journal=Icarus |volume=207 |issue=2 |pages=845–867 |doi=10.1016/j.icarus.2009.11.035 |bibcode=2010Icar..207..845P }}</ref> | <ref name="Patterson2009">{{cite journal |last1=Patterson |first1=G. Wesley |last2=Collins |first2=Geoffrey C. |last3=Head |first3=James W. |last4=Pappalardo |first4=Robert T. |last5=Prockter |first5=Louise M. |last6=Lucchitta |first6=Baerbel K. |last7=Kay |first7=Jonothan P. |title=Global geological mapping of Ganymede |date=6 December 2009 |journal=Icarus |volume=207 |issue=2 |pages=845–867 |doi=10.1016/j.icarus.2009.11.035 |bibcode=2010Icar..207..845P }}</ref> | ||
| <ref name="gregg2021">{{cite book |last1=Gregg |first1=Tracy K. P. |last2=Lopes |first2=Rosaly M. C. |last3=Fagents |first3=Sarah A. |author-link= |date=December 2021 |title=Planetary Volcanism across the Solar System |location= |edition= |publisher= |isbn=978-0-12-813987-5 |url=https://www.sciencedirect.com/book/9780128139875/planetary-volcanism-across-the-solar-system |access-date=12 March 2024 |doi=10.1016/B978-0-12-813987-5.00005-5|s2cid=245084572 }}</ref> | <ref name="gregg2021">{{cite book |last1=Gregg |first1=Tracy K. P. |last2=Lopes |first2=Rosaly M. C. |author2-link=Rosaly Lopes |last3=Fagents |first3=Sarah A. |author-link= |date=December 2021 |title=Planetary Volcanism across the Solar System |location= |edition= |publisher= |isbn=978-0-12-813987-5 |url=https://www.sciencedirect.com/book/9780128139875/planetary-volcanism-across-the-solar-system |access-date=12 March 2024 |doi=10.1016/B978-0-12-813987-5.00005-5|s2cid=245084572 }}</ref> | ||
| <ref name="Emery2024">{{cite journal | <ref name="Emery2024">{{cite journal | ||
| Line 194: | Line 194: | ||
| |arxiv=2309.15230|bibcode=2024Icar..41416017E }}</ref> | |arxiv=2309.15230|bibcode=2024Icar..41416017E }}</ref> | ||
| <ref name="naturepluto">{{cite journal |url=http://www.nature.com/news/icy-volcanoes-may-dot-pluto-s-surface-1.18756 |title=Ice volcanoes may dot Pluto's surface |journal=Nature |author=Witze, Alexandra|doi=10.1038/nature.2015.18756 |year=2015 |s2cid=182698872 }}</ref> | <ref name="naturepluto">{{cite journal |url=http://www.nature.com/news/icy-volcanoes-may-dot-pluto-s-surface-1.18756 |title=Ice volcanoes may dot Pluto's surface |journal=Nature |author=Witze, Alexandra |doi=10.1038/nature.2015.18756 |year=2015 |s2cid=182698872 |access-date=15 November 2015 |archive-date=17 November 2015 |archive-url=https://web.archive.org/web/20151117140548/http://www.nature.com/news/icy-volcanoes-may-dot-pluto-s-surface-1.18756 |url-status=live }}</ref> | ||
| <ref name="sori2021">{{Cite journal |first1=Michael T. |last1=Sori |first2=Hanna G. |last2=Sizemore |display-authors=etal |date=December 2018 |title=Cryovolcanic rates on Ceres revealed by topography |url=https://www.nature.com/articles/s41550-018-0574-1.epdf |journal=Nature Astronomy |volume=2 |issue=12 |pages=946–950 |bibcode=2018NatAs...2..946S |doi=10.1038/s41550-018-0574-1 |access-date=17 August 2021 |s2cid=186800298 }}</ref> | <ref name="sori2021">{{Cite journal |first1=Michael T. |last1=Sori |first2=Hanna G. |last2=Sizemore |display-authors=etal |date=December 2018 |title=Cryovolcanic rates on Ceres revealed by topography |url=https://www.nature.com/articles/s41550-018-0574-1.epdf |journal=Nature Astronomy |volume=2 |issue=12 |pages=946–950 |bibcode=2018NatAs...2..946S |doi=10.1038/s41550-018-0574-1 |access-date=17 August 2021 |s2cid=186800298 |archive-date=17 August 2021 |archive-url=https://web.archive.org/web/20210817112000/https://www.nature.com/articles/s41550-018-0574-1.epdf |url-status=live }}</ref> | ||
| <ref name="Schenk2007">{{cite journal|last1= Schenk |first1=Paul M. |last2=Zahnle |first2=Kevin |title=On the negligible surface age of Triton |journal= Icarus |volume=192 |issue=1 |date=December 2007 |pages=135–149 |doi=10.1016/j.icarus.2007.07.004 |bibcode=2007Icar..192..135S }}</ref> | <ref name="Schenk2007">{{cite journal|last1= Schenk |first1=Paul M. |last2=Zahnle |first2=Kevin |title=On the negligible surface age of Triton |journal= Icarus |volume=192 |issue=1 |date=December 2007 |pages=135–149 |doi=10.1016/j.icarus.2007.07.004 |bibcode=2007Icar..192..135S }}</ref> | ||
| Line 215: | Line 215: | ||
| <ref name="glein2024">{{Cite journal |last1=Glein |first1=Christopher R. |last2=Grundy |first2=William M. |last3=Lunine |first3=Jonathan I. |last4=Wong |first4=Ian |last5=Protopapa |first5=Silvia |last6=Pinilla-Alonso |first6=Noemi |last7=Stansberry |first7=John A. |last8=Holler |first8=Bryan J. |last9=Cook |first9=Jason C. |last10=Souza-Feliciano |first10=Ana Carolina |date=April 2024 |title=Moderate D/H ratios in methane ice on Eris and Makemake as evidence of hydrothermal or metamorphic processes in their interiors: Geochemical analysis |url=https://www.sciencedirect.com/science/article/pii/S0019103524000575 |journal=Icarus |volume=412 |bibcode=2024Icar..41215999G |doi=10.1016/j.icarus.2024.115999 |arxiv=2309.05549 |s2cid=261696907 |access-date=12 March 2024 }}</ref> | <ref name="glein2024">{{Cite journal |last1=Glein |first1=Christopher R. |last2=Grundy |first2=William M. |last3=Lunine |first3=Jonathan I. |last4=Wong |first4=Ian |last5=Protopapa |first5=Silvia |last6=Pinilla-Alonso |first6=Noemi |last7=Stansberry |first7=John A. |last8=Holler |first8=Bryan J. |last9=Cook |first9=Jason C. |last10=Souza-Feliciano |first10=Ana Carolina |date=April 2024 |title=Moderate D/H ratios in methane ice on Eris and Makemake as evidence of hydrothermal or metamorphic processes in their interiors: Geochemical analysis |url=https://www.sciencedirect.com/science/article/pii/S0019103524000575 |journal=Icarus |volume=412 |bibcode=2024Icar..41215999G |doi=10.1016/j.icarus.2024.115999 |arxiv=2309.05549 |s2cid=261696907 |access-date=12 March 2024 }}</ref> | ||
| <ref name="NHEncounter">{{cite web |title=NASA's Three-Billion-Mile Journey to Pluto Reaches Historic Encounter |url=http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20150714-2 |publisher=] |date=July 14, 2015}}</ref> | <ref name="NHEncounter">{{cite web |title=NASA's Three-Billion-Mile Journey to Pluto Reaches Historic Encounter |url=http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20150714-2 |publisher=] |date=July 14, 2015 |access-date=18 May 2024 |archive-date=14 November 2021 |archive-url=https://web.archive.org/web/20211114080805/http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20150714-2 |url-status=live }}</ref> | ||
| <ref name="Porco2006">{{cite journal| doi = 10.1126/science.1123013| last1 = Porco| first1 = C. C.| author-link1 = Carolyn Porco| last2 = Helfenstein| first2 = P.| last3 = Thomas| first3 = P. C.| last4 = Ingersoll| first4 = A. P.| last5 = Wisdom| first5 = J.| last6 = West| first6 = R.| last7 = Neukum| first7 = G.| last8 = Denk| first8 = T.| last9 = Wagner| first9 = R.| date = 10 March 2006| title = Cassini Observes the Active South Pole of Enceladus| journal = Science| volume = 311| issue = 5766| pages = 1393–1401| pmid = 16527964| bibcode = 2006Sci...311.1393P| s2cid = 6976648| url = https://resolver.caltech.edu/CaltechAUTHORS:20130125-103250989| ref = {{sfnRef|Porco Helfenstein et al. 2006}}}}</ref> | <ref name="Porco2006">{{cite journal| doi = 10.1126/science.1123013| last1 = Porco| first1 = C. C.| author-link1 = Carolyn Porco| last2 = Helfenstein| first2 = P.| last3 = Thomas| first3 = P. C.| last4 = Ingersoll| first4 = A. P.| last5 = Wisdom| first5 = J.| last6 = West| first6 = R.| last7 = Neukum| first7 = G.| last8 = Denk| first8 = T.| last9 = Wagner| first9 = R.| date = 10 March 2006| title = Cassini Observes the Active South Pole of Enceladus| journal = Science| volume = 311| issue = 5766| pages = 1393–1401| pmid = 16527964| bibcode = 2006Sci...311.1393P| s2cid = 6976648| url = https://resolver.caltech.edu/CaltechAUTHORS:20130125-103250989| ref = {{sfnRef|Porco Helfenstein et al. 2006}}| access-date = 13 March 2024| archive-date = 16 June 2024| archive-url = https://web.archive.org/web/20240616103721/https://authors.library.caltech.edu/records/pjrgh-0jh74| url-status = live}}</ref> | ||
| <ref name="rain">{{cite web|url=http://www.esa.int/Our_Activities/Space_Science/Herschel/Enceladus_rains_water_onto_Saturn|title=Enceladus rains water onto Saturn|work=ESA|date=2011|access-date=January 14, 2015|archive-date=November 23, 2017|archive-url=https://web.archive.org/web/20171123034704/http://www.esa.int/Our_Activities/Space_Science/Herschel/Enceladus_rains_water_onto_Saturn|url-status=live}}</ref> | <ref name="rain">{{cite web|url=http://www.esa.int/Our_Activities/Space_Science/Herschel/Enceladus_rains_water_onto_Saturn|title=Enceladus rains water onto Saturn|work=ESA|date=2011|access-date=January 14, 2015|archive-date=November 23, 2017|archive-url=https://web.archive.org/web/20171123034704/http://www.esa.int/Our_Activities/Space_Science/Herschel/Enceladus_rains_water_onto_Saturn|url-status=live}}</ref> | ||
| Line 233: | Line 233: | ||
| <ref name="Iess2012">{{Cite journal |doi=10.1126/science.1219631 |pmid=22745254 |title=The Tides of Titan |journal=Science |volume=337 |issue=6093 |pages=457–9 |year=2012 |last1=Iess |first1=L. |last2=Jacobson |first2=R. A. |last3=Ducci |first3=M. |last4=Stevenson |first4=D. J. |last5=Lunine |first5=Jonathan I. |last6=Armstrong |first6=J. W. |last7=Asmar |first7=S. W. |last8=Racioppa |first8=P. |last9=Rappaport |first9=N. J. |last10=Tortora |first10=P. |bibcode=2012Sci...337..457I |hdl=11573/477190 |s2cid=10966007 |hdl-access=free }}</ref> | <ref name="Iess2012">{{Cite journal |doi=10.1126/science.1219631 |pmid=22745254 |title=The Tides of Titan |journal=Science |volume=337 |issue=6093 |pages=457–9 |year=2012 |last1=Iess |first1=L. |last2=Jacobson |first2=R. A. |last3=Ducci |first3=M. |last4=Stevenson |first4=D. J. |last5=Lunine |first5=Jonathan I. |last6=Armstrong |first6=J. W. |last7=Asmar |first7=S. W. |last8=Racioppa |first8=P. |last9=Rappaport |first9=N. J. |last10=Tortora |first10=P. |bibcode=2012Sci...337..457I |hdl=11573/477190 |s2cid=10966007 |hdl-access=free }}</ref> | ||
| <ref name="Lopes2013">{{cite journal |last1=Lopes |first1=R. M. C. |authorlink=Rosaly Lopes-Gautier |last2=Kirk |first2=R. L. |last3=Mitchell |first3=K. L. |last4=LeGall |first4=A. |last5=Barnes |first5=J. W. |last6=Hayes |first6=A. |last7=Kargel |first7=J. |last8=Wye |first8=L. |last9=Radebaugh |first9=J. |last10=Stofan |first10=E. R. |last11=Janssen|first11=M. A. |last12=Neish |first12=C. D. |last13=Wall |first13=S. D. |last14=Wood |first14=C. A. |last15=Lunine |first15=Jonathan I. |author-link15=Jonathan Lunine |last16=Malaska |first16=M. J.|title=Cryovolcanism on Titan: New results from Cassini RADAR and VIMS |journal=Journal of Geophysical Research: Planets |volume=118 |issue=3 |pages=416–435 |date=19 March 2013 |doi=10.1002/jgre.20062 |bibcode=2013JGRE..118..416L |url=https://hal.archives-ouvertes.fr/hal-00807740/file/Lopes_et_al-2013-Journal_of_Geophysical_Research__Planets.pdf |doi-access=free }}</ref> | <ref name="Lopes2013">{{cite journal |last1=Lopes |first1=R. M. C. |authorlink=Rosaly Lopes-Gautier |last2=Kirk |first2=R. L. |last3=Mitchell |first3=K. L. |last4=LeGall |first4=A. |last5=Barnes |first5=J. W. |last6=Hayes |first6=A. |last7=Kargel |first7=J. |last8=Wye |first8=L. |last9=Radebaugh |first9=J. |last10=Stofan |first10=E. R. |last11=Janssen |first11=M. A. |last12=Neish |first12=C. D. |last13=Wall |first13=S. D. |last14=Wood |first14=C. A. |last15=Lunine |first15=Jonathan I. |author-link15=Jonathan Lunine |last16=Malaska |first16=M. J. |title=Cryovolcanism on Titan: New results from Cassini RADAR and VIMS |journal=Journal of Geophysical Research: Planets |volume=118 |issue=3 |pages=416–435 |date=19 March 2013 |doi=10.1002/jgre.20062 |bibcode=2013JGRE..118..416L |url=https://hal.archives-ouvertes.fr/hal-00807740/file/Lopes_et_al-2013-Journal_of_Geophysical_Research__Planets.pdf |doi-access=free |access-date=2 September 2019 |archive-date=1 September 2019 |archive-url=https://web.archive.org/web/20190901143711/https://hal.archives-ouvertes.fr/hal-00807740/file/Lopes_et_al-2013-Journal_of_Geophysical_Research__Planets.pdf |url-status=live }}</ref> | ||
| <ref name="Wood2020">{{cite journal|last1= Wood|first1= C.A.|last2= Radebaugh|first2= J.|title= Morphologic Evidence for Volcanic Craters near Titan's North Polar Region|journal= Journal of Geophysical Research: Planets|year= 2020|volume= 125|issue= 8|pages= e06036|doi= 10.1029/2019JE006036 |doi-access=free |bibcode= 2020JGRE..12506036W|s2cid= 225752345}}</ref> | <ref name="Wood2020">{{cite journal|last1= Wood|first1= C.A.|last2= Radebaugh|first2= J.|title= Morphologic Evidence for Volcanic Craters near Titan's North Polar Region|journal= Journal of Geophysical Research: Planets|year= 2020|volume= 125|issue= 8|pages= e06036|doi= 10.1029/2019JE006036 |doi-access=free |bibcode= 2020JGRE..12506036W|s2cid= 225752345}}</ref> | ||
| Line 247: | Line 247: | ||
| <ref name="mckinnon2014">{{cite book |last1=McKinnon |first1=William B. |last2=Kirk |first2=Randolph L. |date=2014 |title=Encyclopedia of the Solar System |location= |edition=Third |publisher= |pages=861{{hyphen}}881 |isbn=978-0-12-415845-0 |url=https://www.sciencedirect.com/science/article/pii/B9780124158450000402 |access-date=12 March 2024 |doi=10.1016/C2010-0-67309-3}}</ref> | <ref name="mckinnon2014">{{cite book |last1=McKinnon |first1=William B. |last2=Kirk |first2=Randolph L. |date=2014 |title=Encyclopedia of the Solar System |location= |edition=Third |publisher= |pages=861{{hyphen}}881 |isbn=978-0-12-415845-0 |url=https://www.sciencedirect.com/science/article/pii/B9780124158450000402 |access-date=12 March 2024 |doi=10.1016/C2010-0-67309-3}}</ref> | ||
| <ref name="martin-herrero2014">{{cite conference |url=https://www.hou.usra.edu/meetings/lpsc2014/pdf/1177.pdf |title=Characterization and Possible Origin of Sub-Circular Depressions in Ruach Planitia Region, Triton |last1=Martin-Herrero |first1=A. |last2=Ruiz |first2=J. |last3=Romeo |first3=I. |date=March 2014 |pages= |location=The Woodlands, Texas |conference=45th Lunar and Planetary Science Conference |bibcode=2014LPI....45.1177M }}</ref> | <ref name="martin-herrero2014">{{cite conference |url=https://www.hou.usra.edu/meetings/lpsc2014/pdf/1177.pdf |title=Characterization and Possible Origin of Sub-Circular Depressions in Ruach Planitia Region, Triton |last1=Martin-Herrero |first1=A. |last2=Ruiz |first2=J. |last3=Romeo |first3=I. |date=March 2014 |pages= |location=The Woodlands, Texas |conference=45th Lunar and Planetary Science Conference |bibcode=2014LPI....45.1177M |access-date=13 March 2024 |archive-date=12 March 2024 |archive-url=https://web.archive.org/web/20240312221203/https://www.hou.usra.edu/meetings/lpsc2014/pdf/1177.pdf |url-status=live }}</ref> | ||
| <ref name="hofgartner2022">{{Cite journal |last1=Hofgartner |first1=Jason D. |last2=Birch |first2=Samuel P. D. |last3=Castillo |first3=Julie |last4=Grundy |first4=Will M. |last5=Hansen |first5=Candice J. |last6=Hayes |first6=Alexander G. |last7=Howett |first7=Carly J. A. |last8=Hurford |first8=Terry A. |last9=Martin |first9=Emily S. |last10=Mitchell |first10=Karl L. |last11=Nordheim |first11=Tom A. |last12=Poston |first12=Michael J. |last13=Prockter |first13=Louise M. |last14=Quick |first14=Lynnae C. |last15=Schenk |first15=Paul |date=2022-03-15 |title=Hypotheses for Triton's plumes: New analyses and future remote sensing tests |url=https://www.sciencedirect.com/science/article/pii/S0019103521004796 |journal=Icarus |volume=375 |pages=114835 |doi=10.1016/j.icarus.2021.114835 |issn=0019-1035|arxiv=2112.04627 |bibcode=2022Icar..37514835H }}</ref> | <ref name="hofgartner2022">{{Cite journal |last1=Hofgartner |first1=Jason D. |last2=Birch |first2=Samuel P. D. |last3=Castillo |first3=Julie |last4=Grundy |first4=Will M. |last5=Hansen |first5=Candice J. |last6=Hayes |first6=Alexander G. |last7=Howett |first7=Carly J. A. |last8=Hurford |first8=Terry A. |last9=Martin |first9=Emily S. |last10=Mitchell |first10=Karl L. |last11=Nordheim |first11=Tom A. |last12=Poston |first12=Michael J. |last13=Prockter |first13=Louise M. |last14=Quick |first14=Lynnae C. |last15=Schenk |first15=Paul |date=2022-03-15 |title=Hypotheses for Triton's plumes: New analyses and future remote sensing tests |url=https://www.sciencedirect.com/science/article/pii/S0019103521004796 |journal=Icarus |volume=375 |pages=114835 |doi=10.1016/j.icarus.2021.114835 |issn=0019-1035|arxiv=2112.04627 |bibcode=2022Icar..37514835H }}</ref> | ||
| Line 254: | Line 254: | ||
| | url = http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20151109 | | url = http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20151109 | ||
| | title = At Pluto, New Horizons Finds Geology of All Ages, Possible Ice Volcanoes, Insight into Planetary Origins | | title = At Pluto, New Horizons Finds Geology of All Ages, Possible Ice Volcanoes, Insight into Planetary Origins | ||
| | date = 9 November 2015 |
| date = 9 November 2015 | ||
| | website = New Horizons News Center | |||
| | publisher = The Johns Hopkins University Applied Physics Laboratory LLC | | publisher = The Johns Hopkins University Applied Physics Laboratory LLC | ||
| | access-date = 9 November 2015 |
| access-date = 9 November 2015 | ||
| | archive-date = 4 March 2016 | |||
| | archive-url = https://web.archive.org/web/20160304120139/http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20151109 | |||
| | url-status = live | |||
| }}</ref> | |||
| <ref name = "Witze2015-11-09">{{cite journal | <ref name = "Witze2015-11-09">{{cite journal | ||
| | url = http://www.nature.com/news/icy-volcanoes-may-dot-pluto-s-surface-1.18756 | | url = http://www.nature.com/news/icy-volcanoes-may-dot-pluto-s-surface-1.18756 | ||
| | title = Icy volcanoes may dot Pluto's surface | | title = Icy volcanoes may dot Pluto's surface | ||
| | last = Witze |
| last = Witze | ||
| | first = A. | |||
| | date = 9 November 2015 | |||
| | journal = Nature | |||
| | publisher = ] |
| publisher = ] | ||
| | access-date = 9 November 2015 | |||
| | doi = 10.1038/nature.2015.18756 | |||
| | s2cid = 182698872 | | s2cid = 182698872 | ||
| | archive-date = 17 November 2015 | |||
| | archive-url = https://web.archive.org/web/20151117140548/http://www.nature.com/news/icy-volcanoes-may-dot-pluto-s-surface-1.18756 | |||
| | url-status = live | |||
| }}</ref> | }}</ref> | ||
| Line 276: | Line 289: | ||
| <ref name="McKinnon2016">{{cite journal|last1=McKinnon|first1=W. B.|display-authors=etal|title=Convection in a volatile nitrogen-ice-rich layer drives Pluto's geological vigour|journal= Nature|volume=534|issue= 7605|date=1 June 2016|pages= 82–85|doi= 10.1038/nature18289|pmid=27251279|arxiv=1903.05571|bibcode=2016Natur.534...82M|s2cid=30903520}}</ref> | <ref name="McKinnon2016">{{cite journal|last1=McKinnon|first1=W. B.|display-authors=etal|title=Convection in a volatile nitrogen-ice-rich layer drives Pluto's geological vigour|journal= Nature|volume=534|issue= 7605|date=1 June 2016|pages= 82–85|doi= 10.1038/nature18289|pmid=27251279|arxiv=1903.05571|bibcode=2016Natur.534...82M|s2cid=30903520}}</ref> | ||
| <ref name="desch2017">{{Cite journal |last1=Desch |first1=S. J. |last2=Neveu |first2=M. |date=2017 |title=Differentiation and cryovolcanism on Charon: A view before and after New Horizons |url=https://www.sciencedirect.com/science/article/pii/S0019103516307904 |journal=Icarus |series= |language=en |volume=287|pages=175–186|bibcode= |
<ref name="desch2017">{{Cite journal |last1=Desch |first1=S. J. |last2=Neveu |first2=M. |date=2017 |title=Differentiation and cryovolcanism on Charon: A view before and after New Horizons |url=https://www.sciencedirect.com/science/article/pii/S0019103516307904 |journal=Icarus |series= |language=en |volume=287 |pages=175–186 |bibcode=2017Icar..287..175D |doi=10.1016/j.icarus.2016.11.037 |issn= |access-date=13 March 2024 |archive-date=1 October 2017 |archive-url=https://web.archive.org/web/20171001125311/http://www.sciencedirect.com/science/article/pii/S0019103516307904 |url-status=live }}</ref> | ||
| <ref name="Showman1999">{{cite journal |last1=Showman |first1=Adam P. |last2=Malhotra |first2=Renu |title=The Galilean Satellites |date=October 1, 1999 |journal=Science |volume=286 |pages=77–84 |doi=10.1126/science.286.5437.77 |url=http://www.lpl.arizona.edu/~showman/publications/showman-malhotra-1999.pdf |pmid=10506564 |issue=5437 |access-date=January 17, 2008 |archive-date=May 14, 2011 |archive-url=https://web.archive.org/web/20110514231040/http://www.lpl.arizona.edu/~showman/publications/showman-malhotra-1999.pdf |url-status=live }}</ref> | <ref name="Showman1999">{{cite journal |last1=Showman |first1=Adam P. |last2=Malhotra |first2=Renu |title=The Galilean Satellites |date=October 1, 1999 |journal=Science |volume=286 |pages=77–84 |doi=10.1126/science.286.5437.77 |url=http://www.lpl.arizona.edu/~showman/publications/showman-malhotra-1999.pdf |pmid=10506564 |issue=5437 |access-date=January 17, 2008 |archive-date=May 14, 2011 |archive-url=https://web.archive.org/web/20110514231040/http://www.lpl.arizona.edu/~showman/publications/showman-malhotra-1999.pdf |url-status=live }}</ref> | ||
| Line 284: | Line 297: | ||
| <ref name="mccord.2005">{{cite journal |last=McCord |first=Thomas B. |title=Ceres: Evolution and current state |journal=Journal of Geophysical Research |volume=110 |issue=E5 |page=E05009 |date=2005 |doi=10.1029/2004JE002244 |bibcode=2005JGRE..110.5009M |doi-access=free }}</ref> | <ref name="mccord.2005">{{cite journal |last=McCord |first=Thomas B. |title=Ceres: Evolution and current state |journal=Journal of Geophysical Research |volume=110 |issue=E5 |page=E05009 |date=2005 |doi=10.1029/2004JE002244 |bibcode=2005JGRE..110.5009M |doi-access=free }}</ref> | ||
| <ref name="cr.ceres">{{cite journal |last1=Castillo-Rogez |first1=J. C. |last2=McCord |first2=T. B. |last3=Davis |first3=A. G. |title=Ceres: evolution and present state |journal=Lunar and Planetary Science |volume=XXXVIII |pages=2006–2007 |date=2007 |url=http://www.lpi.usra.edu/meetings/lpsc2007/pdf/2006.pdf |access-date=2009-06-25 }}</ref> | <ref name="cr.ceres">{{cite journal |last1=Castillo-Rogez |first1=J. C. |last2=McCord |first2=T. B. |last3=Davis |first3=A. G. |title=Ceres: evolution and present state |journal=Lunar and Planetary Science |volume=XXXVIII |pages=2006–2007 |date=2007 |url=http://www.lpi.usra.edu/meetings/lpsc2007/pdf/2006.pdf |access-date=2009-06-25 |archive-date=24 February 2011 |archive-url=https://web.archive.org/web/20110224014228/http://www.lpi.usra.edu/meetings/lpsc2007/pdf/2006.pdf |url-status=live }}</ref> | ||
| <ref name="mcogvern2024">{{cite journal |last1=McGovern |first1=J. C. |last2=Nguyen |first2=A. L. |title=The role of Pluto's ocean's salinity in supporting nitrogen ice loads within the Sputnik Planitia basin |journal=Icarus |volume=412 |date=April 2024 |url=https://www.sciencedirect.com/science/article/pii/S0019103524000265 |access-date=13 March 2024 |bibcode=2024Icar..41215968M |doi=10.1016/j.icarus.2024.115968 |s2cid=267316007 }}</ref> | <ref name="mcogvern2024">{{cite journal |last1=McGovern |first1=J. C. |last2=Nguyen |first2=A. L. |title=The role of Pluto's ocean's salinity in supporting nitrogen ice loads within the Sputnik Planitia basin |journal=Icarus |volume=412 |date=April 2024 |url=https://www.sciencedirect.com/science/article/pii/S0019103524000265 |access-date=13 March 2024 |bibcode=2024Icar..41215968M |doi=10.1016/j.icarus.2024.115968 |s2cid=267316007 }}</ref> | ||
| Line 295: | Line 308: | ||
| <ref name="IceVolcano">{{cite web |url=https://www.space.com/pluto-recent-ice-volcanoes-new-horizons |title=Ice volcanoes on Pluto may still be erupting |date=1 April 2022 |last1=Sohn |first1=Rebecca |publisher=Space.com }}</ref> | <ref name="IceVolcano">{{cite web |url=https://www.space.com/pluto-recent-ice-volcanoes-new-horizons |title=Ice volcanoes on Pluto may still be erupting |date=1 April 2022 |last1=Sohn |first1=Rebecca |publisher=Space.com }}</ref> | ||
| <ref name="NASA-20150306">{{cite web |last1=Landau |first1=Elizabeth |last2=Brown |first2=Dwayne |title=NASA Spacecraft Becomes First to Orbit a Dwarf Planet |url=http://www.jpl.nasa.gov/news/news.php?feature=4503 |date=March 6, 2015 |publisher=NASA |access-date=March 6, 2015}}</ref> | <ref name="NASA-20150306">{{cite web |last1=Landau |first1=Elizabeth |last2=Brown |first2=Dwayne |title=NASA Spacecraft Becomes First to Orbit a Dwarf Planet |url=http://www.jpl.nasa.gov/news/news.php?feature=4503 |date=March 6, 2015 |publisher=NASA |access-date=March 6, 2015 |archive-date=7 March 2015 |archive-url=https://web.archive.org/web/20150307062258/http://www.jpl.nasa.gov/news/news.php?feature=4503 |url-status=live }}</ref> | ||
| <ref name="ArgadnelGPN">{{gpn|361|Argadnel Regio}} (Center Latitude: -14.60°, Center Longitude: 208.50°)</ref> | <ref name="ArgadnelGPN">{{gpn|361|Argadnel Regio}} (Center Latitude: -14.60°, Center Longitude: 208.50°)</ref> | ||
| Line 303: | Line 316: | ||
| <ref name="Schenk2018">{{cite journal|last1= Schenk|first1=P. M.|last2= Beyer|first2=R. A.|last3= McKinnon|first3=W. B.|last4= Moore|first4=J. M.|last5= Spencer|first5=J. R.|last6= White|first6=O. L.|last7= Singer|first7= K.|last8= Nimmo|first8= F.|last9= Thomason|first9= C.|last10= Lauer|first10=T. R.|last11= Robbins|first11= S.|last12= Umurhan|first12=O. M.|last13= Grundy|first13=W. M.|last14= Stern|first14=S. A.|last15= Weaver|first15=H. A.|last16= Young|first16=L. A.|last17= Smith|first17=K. E.|last18= Olkin|first18= C.|title= Basins, fractures and volcanoes: Global cartography and topography of Pluto from New Horizons|journal= Icarus|volume= 314|date=November 2018|pages= 400–433|doi= 10.1016/j.icarus.2018.06.008|bibcode= 2018Icar..314..400S|s2cid=126273376 }}</ref> | <ref name="Schenk2018">{{cite journal|last1= Schenk|first1=P. M.|last2= Beyer|first2=R. A.|last3= McKinnon|first3=W. B.|last4= Moore|first4=J. M.|last5= Spencer|first5=J. R.|last6= White|first6=O. L.|last7= Singer|first7= K.|last8= Nimmo|first8= F.|last9= Thomason|first9= C.|last10= Lauer|first10=T. R.|last11= Robbins|first11= S.|last12= Umurhan|first12=O. M.|last13= Grundy|first13=W. M.|last14= Stern|first14=S. A.|last15= Weaver|first15=H. A.|last16= Young|first16=L. A.|last17= Smith|first17=K. E.|last18= Olkin|first18= C.|title= Basins, fractures and volcanoes: Global cartography and topography of Pluto from New Horizons|journal= Icarus|volume= 314|date=November 2018|pages= 400–433|doi= 10.1016/j.icarus.2018.06.008|bibcode= 2018Icar..314..400S|s2cid=126273376 }}</ref> | ||
| <ref name="kryos">{{cite encyclopedia |url=https://www.perseus.tufts.edu/hopper/text?doc=Perseus:text:1999.04.0057:entry=kru/os |title=κρύος |encyclopedia=A Greek–English Lexicon |publisher=Clarendon Press |date=1940 |last1=Liddell |first1=Henry George |last2=Scott |first2=Robert }}</ref> | <ref name="kryos">{{cite encyclopedia |url=https://www.perseus.tufts.edu/hopper/text?doc=Perseus:text:1999.04.0057:entry=kru/os |title=κρύος |encyclopedia=A Greek–English Lexicon |publisher=Clarendon Press |date=1940 |last1=Liddell |first1=Henry George |last2=Scott |first2=Robert |access-date=13 May 2024 |archive-date=12 January 2024 |archive-url=https://web.archive.org/web/20240112170653/https://www.perseus.tufts.edu/hopper/text?doc=Perseus:text:1999.04.0057:entry=kru/os |url-status=live }}</ref> | ||
| <ref name="PlanetaryLandforms">{{cite encyclopedia |url=https://link.springer.com/referencework/10.1007/978-1-4614-3134-3 |title=Encyclopedia of Planetary Landforms |editor-last1=Hargitai |editor-first1=Henrik |editor-last2=Kereszturi |editor-first2=Ákos |edition=first |isbn=978-1-4614-3133-6 |doi=10.1007/978-1-4614-3134-3 |publisher=Springer New York |date=2015 }}</ref> | <ref name="PlanetaryLandforms">{{cite encyclopedia |url=https://link.springer.com/referencework/10.1007/978-1-4614-3134-3 |title=Encyclopedia of Planetary Landforms |editor-last1=Hargitai |editor-first1=Henrik |editor-last2=Kereszturi |editor-first2=Ákos |edition=first |isbn=978-1-4614-3133-6 |doi=10.1007/978-1-4614-3134-3 |publisher=Springer New York |date=2015 }}</ref> | ||
| Line 311: | Line 324: | ||
| <ref name="Moore2007">{{cite journal |last1=Moore |first1=M. H. |last2=Ferrante |first2=R. F. |last3=Hudson |first3=R. L. |last4=Stone |first4=J. N. |title=Ammonia–water ice laboratory studies relevant to outer Solar System surfaces |date=September 2007 |journal=Icarus |volume=190 |issue=1 |pages=260–273 |doi=10.1016/j.icarus.2007.02.020 |bibcode=2007Icar..190..260M }}</ref> | <ref name="Moore2007">{{cite journal |last1=Moore |first1=M. H. |last2=Ferrante |first2=R. F. |last3=Hudson |first3=R. L. |last4=Stone |first4=J. N. |title=Ammonia–water ice laboratory studies relevant to outer Solar System surfaces |date=September 2007 |journal=Icarus |volume=190 |issue=1 |pages=260–273 |doi=10.1016/j.icarus.2007.02.020 |bibcode=2007Icar..190..260M }}</ref> | ||
| <ref name="Solomatov1998">{{cite journal|doi=10.1046/j.1365-246X.1998.00521.x|title=Mantle convection with a brittle lithosphere: thoughts on the global tectonic styles of the Earth and Venus|year=1998|last1=Moresi|first1=Louis|last2=Solomatov|first2=Viatcheslav|journal=Geophysical Journal International|volume=133|issue=3|pages=669–82|citeseerx = 10.1.1.30.5989|bibcode = 1998GeoJI.133..669M }}</ref> | <ref name="Solomatov1998">{{cite journal|doi=10.1046/j.1365-246X.1998.00521.x|title=Mantle convection with a brittle lithosphere: thoughts on the global tectonic styles of the Earth and Venus|year=1998|last1=Moresi|first1=Louis|last2=Solomatov|first2=Viatcheslav|journal=Geophysical Journal International|volume=133|issue=3|pages=669–82|doi-access=free |citeseerx = 10.1.1.30.5989|bibcode = 1998GeoJI.133..669M }}</ref> | ||
| <ref name="Saxena2018">{{cite journal |last1=Saxena |first1=Prabal |last2=Renaud |first2=Joe P. |last3=Henning |first3=Wade G. |last4=Jutzi |first4=Martin |last5=Hurford |first5=Terry |title=Relevance of tidal heating on large TNOs |date=March 2018 |doi=10.1016/j.icarus.2017.11.023 |bibcode=2018Icar..302..245S |arxiv=1706.04682 |journal=Icarus |volume=302 |pages=245–260 }}</ref> | <ref name="Saxena2018">{{cite journal |last1=Saxena |first1=Prabal |last2=Renaud |first2=Joe P. |last3=Henning |first3=Wade G. |last4=Jutzi |first4=Martin |last5=Hurford |first5=Terry |title=Relevance of tidal heating on large TNOs |date=March 2018 |doi=10.1016/j.icarus.2017.11.023 |bibcode=2018Icar..302..245S |arxiv=1706.04682 |journal=Icarus |volume=302 |pages=245–260 }}</ref> | ||
| <ref name="NASAV2">{{cite web |url=https://science.nasa.gov/mission/voyager/voyager-2/ |title=Voyager 2 |date=March 2024 |last1=Bolles |first1=Dana |publisher=NASA }}</ref> | <ref name="NASAV2">{{cite web |url=https://science.nasa.gov/mission/voyager/voyager-2/ |title=Voyager 2 |date=March 2024 |last1=Bolles |first1=Dana |publisher=NASA |access-date=21 May 2024 |archive-date=18 May 2024 |archive-url=https://web.archive.org/web/20240518211533/https://science.nasa.gov/mission/voyager/voyager-2/ |url-status=live }}</ref> | ||
| }} <!-- end of reflist --> | }} <!-- end of reflist --> | ||
Revision as of 21:38, 16 November 2024
Type of volcano that erupts volatiles such as water, ammonia or methane, instead of molten rock
For ice mounds on Earth, see Ice volcano.
A cryovolcano (sometimes informally referred to as an ice volcano) is a type of volcano that erupts gases and volatile material such as liquid water, ammonia, and hydrocarbons. The erupted material is collectively referred to as cryolava; it originates from a reservoir of subsurface cryomagma. Cryovolcanic eruptions can take many forms, such as fissure and curtain eruptions, effusive cryolava flows, and large-scale resurfacing, and can vary greatly in output volumes. Immediately after an eruption, cryolava quickly freezes, constructing geological features and altering the surface.
Although rare in the inner Solar System, past and recent cryovolcanism is common on planetary objects in the outer Solar System, especially on the icy moons of the giant planets and potentially amongst the dwarf planets as well. As such, cryovolcanism is important to the geological histories of these worlds, constructing landforms or even resurfacing entire regions. Despite this, only a few eruptions have ever been observed in the Solar System. The sporadic nature of direct observations means that the true number of extant cryovolcanoes is contentious.
Like volcanism on the terrestrial planets, cryovolcanism is driven by escaping internal heat from within a celestial object, often supplied by extensive tidal heating in the case of the moons of the giant planets. However, isolated dwarf planets are capable of retaining enough internal heat from formation and radioactive decay to drive cryovolcanism on their own, an observation which has been supported by both in situ observations by spacecraft and distant observations by telescopes.
Etymology and terminology
The term cryovolcano was coined by Steven K. Croft in a 1987 conference abstract at the Geological Society of America (GSA) Abstract with Programs. The term is ultimately a combination of cryo-, from the Ancient Greek κρῠ́ος (krúos, meaning cold or frost), and volcano. In general, terminology used to describe cryovolcanism is analogous to volcanic terminology:
- Cryolava and cryomagma are distinguished in a manner similar to lava and magma. Cryomagma refers to the molten or partially molten material beneath a body's surface, where it may then erupt onto the surface. If the material is still fluid, it is classified as cryolava, which can flow in cryolava channels, analogs to lava channels. Explosive eruptions, however, may pulverize the material into a fine "ash" termed cryoclastic material. Cryoclastic material flowing downhill produces cryoclastic flows, analogs to pyroclastic flows.
- A cryovolcanic edifice is a landform constructed by cryovolcanic eruptions. These may take the form of shields (analogous to terrestrial shield volcanoes), cones (analogous to cinder cones and spatter cones), or domes (analogous to lava domes). Cryovolcanic edifices may support secondary landforms, such as caldera-like collapse structures, cryovolcanic flow channels (analogous to lava flow features), and cryovolcanic fields and plains (analogous to lava fields and plains).
As cryovolcanism largely takes place on icy worlds, the term ice volcano is sometimes used colloquially.
Types of cryovolcanism
Explosive eruptions
Explosive cryovolcanism, or cryoclastic eruptions, is expected to be driven by the exsolvation of dissolved volatile gasses as pressure drops whilst cryomagma ascends, much like the mechanisms of explosive volcanism on terrestrial planets. Whereas terrestrial explosive volcanism is primarily driven by dissolved water (H2O), carbon dioxide (CO2), and sulfur dioxide (SO2), explosive cryovolcanism may instead be driven by methane (CH4) and carbon monoxide (CO). Upon eruption, cryovolcanic material is pulverized in violent explosions much like volcanic ash and tephra, producing cryoclastic material.
Effusive eruptions
Effusive cryovolcanism takes place with little to no explosive activity and is instead characterized by widespread cryolava flows which cover the pre-existing landscape. In contrast to explosive cryovolcanism, no instances of active effusive cryovolcanism have been observed. Structures constructed by effusive eruptions depend on the viscosity of the erupted material. Eruptions of less viscous cryolava can resurface large regions and form expansive, relatively flat plains, similar to shield volcanoes and flood basalt eruptions on terrestrial planets. More viscous erupted material does not travel as far, and instead can construct localized high-relief features such as cryovolcanic domes.
Mechanisms
For cryovolcanism to occur, three conditions must be met: an ample supply of cryomagma must be produced in a reservoir, the cryomagma must have a force driving ascent, and conduits need to be formed to the surface where cryomagma is able to ascend.
Ascent
A major challenge in models of cryovolcanic mechanisms is that liquid water is substantially denser than water ice, in contrast to silicates where liquid magma is less dense than solid rock. As such, cryomagma must overcome this in order to erupt onto a body's surface. A variety of hypotheses have been proposed by planetary scientists to explain how cryomagma erupts onto the surface:
- Compositional buoyancy: the introduction of impurities such as ammonia, which is expected to be common in the outer Solar System, can help lower the densities of cryomagmas. However, the presence of impurities in cryomagma alone is unlikely to succeed in overcoming the density barrier. Conversely, the density of the ice shell can be increased through impurities as well, such as the inclusion silicate particles and salts. In particular, objects that are only partially differentiated into a rocky core and icy mantle are likely to have ice shells rich in silicate particles.
- Gas-driven buoyancy: besides affecting density, the inclusion of more volatile impurities may help decrease the density of cryomagma as it ascends by the formation of gas bubbles. The volatile compounds are fully dissolved in the cryomagma when pressurized deep beneath the surface. Should the cryomagma ascend, the cryomagma is depressurized. This leads to the exsolution of the volatiles out of the cryomagma, forming gas bubbles that help lower the density of the bulk solution.
- Internal pressurization: the progressive pressurization of a subsurface ocean as it cools and freezes may be enough to force cryomagma to ascend to the surface due to water's unusual property of expanding upon freezing. Internal ocean pressurization does not necessitate the addition of other volatile compounds.
Eruption
In addition to overcoming the density barrier, cryomagma also requires a way to reach the surface in order to erupt. Fractures in particular, either the result of global or localized stress in the icy crust, providing potential eruptive conduits for cryomagma to exploit. Such stresses may come from tidal forces as an object orbits around a parent planet, especially if the object is on an eccentric orbit or if its orbit changes. True polar wander, where the object's surface shifts relative to its rotational axis, can introduce deformities in the ice shell. Impact events also provide an additional source of fracturing by violently disrupting and weakening the crust.
An alternative model for cryovolcanic eruptions invokes solid-state convection and diapirism. If a portion of an object's ice shell is warm and ductile enough, it could begin to convect, much as the Earth's mantle does. As the ice convects, warmer ice becomes buoyant relative to surrounding colder ice, rising towards the surface. The convection can be aided by local density differences in the ice due to an uneven distribution of impurities in the ice shell. If the warm ice intrudes on particularly impure ice (such as ice containing large amounts of salts), the warm ice can lead to the melting of the impure ice. The melting may then go on to erupt or uplift terrain to form surface diapirs.
Cryomagma reservoir generation
Further information: Planetary oceanography
Cryovolcanism implies the generation of large volumes of molten fluid in the interiors of icy worlds. A primary reservoir of such fluid are subsurface oceans. Subsurface oceans are widespread amongst the icy satellites of the giant planets and are largely maintained by tidal heating, where the moon's slightly eccentric orbit allows the rocky core to dissipate energy and generate heat. Evidence for subsurface oceans also exist for the dwarf planets Pluto and, to a lesser extent, Ceres, Eris, Makemake, Sedna, Gonggong, and Quaoar. In the case of Pluto and the other dwarf planets, there is comparatively little, if any, long-term tidal heating. Thus, heating must largely be self-generated, primarily coming from the decay of radioactive isotopes in their rocky cores.
Reservoirs of cryomagma can hypothetically form within the shell of an icy world as well, either from direct localized melting or the injection of cryomagma from a deeper subsurface ocean. A convective layer in the ice shell can generate warm plumes that spread laterally at the base of the brittle icy crust. The intruding warm ice can melt impure ice, forming a lens-shaped region of melting. Other proposed methods of producing localized melts include the buildup of stress within strike-slip faults, where friction may be able to generate enough heat to melt ice; and impact events that violently heat the impact site. Intrusive models, meanwhile, propose that a deeper subsurface ocean directly injects cryomagma through fractures in the ice shell, much like volcanic dike and sill systems.
Cryomagma composition
Water is expected to be the dominant component of cryomagmas. Besides water, cryomagma may contain additional impurities, drastically changing its properties. Certain compounds can lower the density of cryomagma. Ammonia (NH3) in particular may be a common component of cryomagmas, and has been detected in the plumes of Saturn's moon Enceladus. A partially frozen ammonia-water eutectic mixture can be positively buoyant with respect to the icy crust, enabling its eruption. Methanol (CH3OH) can lower cryomagma density even further, whilst significantly increasing viscosity. Conversely, some impurities can increase the density of cryomagma. Salts, such as magnesium sulfate (MgSO4) and sodium sulfate (Na2SO4) significantly increases density with comparatively minor changes in viscosity. Salty or briny cryomagma compositions may be important cryovolcanism on Jupiter's icy moons, where salt-dominated impurities are likely more common. Besides affecting density and viscosity, the inclusions of impurities—particularly salts and especially ammonia—can encourage melting by significantly lowering the melting point of cryomagma.
| Cryomagma composition, mass % | Melting point (K) | Liquid density (g/cm) | Liquid viscosity (Pa·s) | Solid density (g/cm) |
|---|---|---|---|---|
| Pure water 100% H2O |
273 | 1.000 | 0.0017 | 0.917 |
| Brine 81.2% H2O, 16% MgSO4, 2.8% Na2SO4 |
268 | 1.19 | 0.007 | 1.13 |
| Ammonia and water 67.4% H2O, 32.6% NH3 |
176 | 0.946 | 4 | 0.962 |
| Ammonia, water, and methanol 47% H2O, 23% NH3, 30% CH3OH |
153 | 0.978 | 4,000 | – |
| Nitrogen and methane 86.5% N2, 13.5% CH4 |
62 | 0.783 | 0.0003 | – |
| Basaltic lava (comparison) | – | – | ~10-100 | – |
Observations
Although there are broad parallels between cryovolcanism and terrestrial (or "silicate") volcanism, such as the construction of domes and shields, the definitive identification of cryovolcanic structures is difficult. The unusual properties of water-dominated cryolava, for example, means that cryovolcanic features are difficult to interpret using criteria applied to terrestrial volcanic features.
Ceres
Main article: Ceres (dwarf planet) § Cryovolcanism
Ceres is the innermost object in the Solar System known to be cryovolcanically active. Upon the arrival of the Dawn orbiter in March 2015, the dwarf planet was discovered to have numerous bright spots (designated as faculae) located within several major impact basins, most prominently in the center of Occator Crater. These bright spots are composed primarily of various salts, and are hypothesized to have formed from impact-induced upwelling of subsurface material that erupt brine to Ceres's surface. The distribution of hydrated sodium chloride on one particular bright spot, Cerealia Facula, indicates that the upwelling occurred recently or is currently ongoing. That brine exists in Ceres's interior implies that salts played a role in keeping Ceres's subsurface ocean liquid, potentially even to the present day. Dawn also discovered Ahuna Mons and Yamor Mons (formerly Ysolos Mons), two prominent isolated mountains which are likely young cryovolcanic domes. It is expected that cryovolcanic domes eventually subside after becoming extinct due to viscous relaxation, flattening them. This would explain why Ahuna Mons appears to be the most prominent construct on Ceres, despite its geologically young age.
Europa
Main article: Europa (moon) § Surface featuresEuropa receives enough tidal heating from Jupiter to sustain a global liquid water ocean. Its surface is exceedingly young, at roughly 60 to 90 million years old. Its most striking features, a dense web of linear cracks and faults termed lineae, appear to be the sites of active resurfacing on Europa, proceeding in a manner similar to Earth's mid-ocean ridges. In addition to this, Europa may experience a form of subduction, with one block of its icy crust sliding underneath another.
Despite its young surface age, few, if any, distinct cryovolcanoes have been definitively identified on the Europan surface in the past. Nevertheless, observations of Europa from the Hubble Space Telescope (HST) in December 2012 detected columns of excess water vapor up to 200 kilometres (120 miles) high, hinting at the existence of weak, possibly cryovolcanic plumes. The plumes were observed again by the HST in 2014. However, as these are distant observations, the plumes have yet to be definitively confirmed as eruptions. Recent analyses of some Europan surface features have proposed cryovolcanic origins for them as well. In 2011, Europa's chaos terrain, where the crust appears especially disrupted, was interpreted by a team of researchers as the site of very shallow cryomagma lakes. As these subsurface lakes melt and refreeze, they fracture Europa's crust into small blocks, creating the chaos terrain. Later, in 2023, a field of cryovolcanic cones was tentatively identified near the western edge of Argadnel Regio, a region in Europa's southern hemisphere.
Ganymede
Ganymede's surface, like Europa's, is heavily tectonized yet appears to have few cryovolcanic features. By 2009, at least 30 irregularly-shaped depressions (termed paterae) were identified on Ganymede's surface from Voyager and Galileo imagery. The paterae have been hypothesized by several teams of planetary scientists as caldera-like cryovolcanic vents. However, conclusive evidence for a cryovolcanic origin of these structures remains elusive in imagery.
Enceladus
Main article: Enceladus § South polar plumes Further information: Rings of Saturn § E Ring
Saturn's moon Enceladus is host to the most dramatic example of cryovolcanism yet observed, with a series of vents erupting 250 kilograms (550 lb) of material per second that feeds Saturn's E ring. These eruptions take place across Enceladus's south polar region, sourced from four major ridges which form a region informally known as the Tiger Stripes. Enceladus's cryovolcanic activity is sustained by a global subsurface ocean.
Other regions centered on Enceladus's leading and trailing hemispheres—the hemispheres that "face" towards or against the direction of Enceladus's orbit—exhibit similar terrain to that of the Tiger Stripes, possibly indicating that Enceladus has experienced discrete periods of heightened cryovolcanism in the past.
Titan
Main article: Titan (moon) § Cryovolcanism and mountainsSaturn's moon Titan has a dense atmospheric haze layer which permanently obscures visible observations of its surface features, making the definitive identification of cryovolcanic structures especially difficult. Titan has an extensive subsurface ocean, encouraging searches for evidence of cryovolcanism. From Cassini radar data, several features have been proposed as candidate cryovolcanoes, most notably Doom Mons, a mountain reminiscent of a shield or dome edifice; and the neighoring Sotra Patera, an ovular depression that resembles a caldera. Several round lakes and depressions in Titan's polar regions show structural evidence of an explosive origin, including overlapping depressions, raised rims (or "ramparts"), and islands or mountains within depression rim. These characteristics led to a 2020 hypothesis by planetary scientists Charles A. Wood and Jani Radebaugh that they form from either maar-like eruptions—forming by explosions of boiling subsurface liquid as it is rapidly heated by magma (in this case, cryomagma)—or the flooding of collapse calderas.
Uranian moons
On 24 January 1986, Uranus and its system of moons were explored for the first time by the Voyager 2 spacecraft. Of Uranus's five major satellites, Miranda and Ariel appear to have unusually youthful surfaces indicative of relatively recent activity. Miranda in particular has extraordinarily varied terrain, with striking angular features known as the coronae cutting across older terrain. Inverness Corona is located near Miranda's south pole and is estimated to be less than 1 billion years old, and broad similarities between Miranda's coronae and Enceladus's south polar region have been noted. These characteristics have led to several teams of researchers to propose a cryovolcanic origin of the coronae, where eruptions of viscous cryomagma form the structures with some tectonic involvement. Ariel also exhibits widespread resurfacing, with large polygonal crustal blocks divided by large canyons (chasmata) with floors as young as ~0.8 ± 0.5 billion years old, while relatively flat plains may have been the site of large flood eruptions.
Evidence for relatively recent cryovolcanism on the other three round moons of Uranus is less clear. Titania hosts large chasms but does not show any clear evidence of cryovolcanism. Oberon has a massive ~11 km (6.8 mi) high mountain that was observed on its limb at the time of Voyager 2's flyby; the precise origins of the mountain is unclear, but it may be of cryovolcanic origin.
Triton
Main article: Geology of Triton § CryovolcanismNeptune and its largest moon Triton were explored by the Voyager 2 spacecraft on 25 August 1989, revealing Triton's surface features up close for the first time. With an estimated average surface age of 10–100 million years old, with some regions possibly being only a few million years old, Triton is one of the most geologically active worlds in the Solar System. Large-scale cryovolcanic landforms have been identified on Triton's young surface, with nearly all of Triton's observed surface features likely related to cryovolcanism. One of Triton's major cryovolcanic features, Leviathan Patera, the apparent primary vent of the Cipango Planum cryovolcanic plateau which is one of the largest volcanic or cryovolcanic edifices in the Solar System.
Triton hosts four walled plains: Ruach Planitia and Tuonela Planitia form a northern pair, and Sipapu Planitia and Ryugu Planitia form a southern pair. The walled plains are characterized by crenulated, irregularly-shaped cliffs that enclose a flat, young plain with a single group of pits and mounds. The walled plains are likely young cryovolcanic lakes and may represent Triton's youngest cryovolcanic features. The regions around Ruach and Tuonela feature additional smaller subcircular depressions, some of which are partially bordered by walls and scarps. In 2014, a team of planetary scientists interpreted these depressions as diapirs, caldera collapse structures, or impact craters filled in by cryolava flows. To the south of Tuonela Planitia, isolated conical hills with central depressions have been noted as resembling terrestrial cinder cones, possibly pointing to cryovolcanic activity beyond Tuonela Planitia's plains.
Triton's southern polar ice cap is marked by a multitude of dark streaks, likely composed of organic tholins deposited by wind-blown plumes. At least two plumes, the Mahilani Plume and the Hili Plume, have been observed, with the two plumes reaching 8 kilometres (5.0 miles) in altitude. These plumes have been hypothesized by numerous teams of researchers in the early 1990s to be driven by the buildup of nitrogen gas underneath solid nitrogen ice through a sort of solid greenhouse effect; however, more recent analysis in 2022 disfavors the solid greenhouse effect model. An alternative cryovolcanic model, first proposed by R. L. Kirk and collaborators in 1995, instead suggests that the plumes represent explosive cryovolcanic eruption columns—an interpretation supported by the estimated observed output rate of ~200 kg/s, comparable to the output of Enceladus's plumes.
Pluto and Charon
Main articles: Geology of Pluto and Geology of Charon
The dwarf planet Pluto and its system of five moons were explored by the New Horizons spacecraft in a flyby on 14 July 2015, observing their surface features in detail for the first time. The surface of Pluto varies dramatically in age, and several regions appear to display relatively recent cryovolcanic activity. The most reliably identified cryovolcanic structures are Wright Mons and Piccard Mons, two large mountains with central depressions which have led to hypotheses that they may be cryovolcanoes with peak calderas. The two mountains are surrounded by an unusual region of hilly "hummocky terrain", and the lack of distinct flow features have led to an alternative proposal in 2022 by a team of researchers that the structures may instead be formed by sequential dome-forming eruptions, with nearby Coleman Mons being a smaller independent dome.
Virgil Fossae, a large fault within Belton Regio, may also represent another site of cryovolcanism on Pluto. An estimated 300 kilometres (190 miles) of Virgil Fossae's western section was likely the site of a fountaining eruption, spewing and dispersing material that covered surrounding terrain up to 200 kilometres (120 miles) away. More recently, in 2021 Hekla Cavus was hypothesized to have formed from a cryovolcanic collapse by a team of two researchers, C. J. Ahrens and V. F. Chevrier. Similarly, in 2021 a team of planetary scientists led by A. Emran proposed that Kiladze, a feature that is formally classified as an impact crater, is actually a cryovolcanic caldera complex.
Although Sputnik Planitia represents the youngest surface on Pluto, it is not a cryovolcanic structure; Sputnik Planitia continuously resurfaces itself with the convective overturning of glacial nitrogen ice, fuelled by Pluto's internal heat and sublimation into Pluto's atmosphere.
Charon's surface dichotomy indicates that a large section of its surface may have been flooded in large, effusive eruptions, similar to the Lunar maria. These floodplains form Vulcan Planitia and may have erupted as Charon's internal ocean froze.
Other dwarf planets
In 2022, low-resolution near-infrared (0.7–5 μm) spectroscopic observations by the James Webb Space Telescope (JWST) detected light hydrocarbons and complex organic molecules on the surfaces of the dwarf planets Quaoar, Gonggong, and Sedna. The detection indicated that all three have experienced internal melting and planetary differentiation in their pasts. The presence of volatiles on their surfaces indicates that cryovolcanism may be resupplying methane. JWST spectral observations of Eris and Makemake revealed that hydrogen-deuterium and carbon isotopic ratios indicated that both dwarf planets are actively replenishing surface methane as well, possibly with the presence of a subsurface ocean.
These observations, combined with the discoveries in the Pluto system by the New Horizons spacecraft, indicate that icy worlds are capable of sustaining enough heat on their own to drive cryovolcanic activity. In contrast to the icy satellites of the giant planets, where many benefit from extensive tidal heating from their parent planets, the dwarf planets must rely on heat generated primarily or almost entirely by themselves. Leftover primordial heat from formation and radiogenic heat from the decay of radioactive isotopes in their rocky cores likely serve as primary sources of heat. The serpentinization of rocky material or tidal heating from interactions with their satellites.
Gallery
Various examples of probable cryovolcanic structures in the Solar System-
Ruach Planitia and Tuonela Planitia, Triton
-
Detail mosaic of Leviathan Patera, Triton
-
Radar image of Doom Mons, Titan
-
Ahuna Mons, Ceres
-
Topography map of Wright Mons and Piccard Mons, Pluto
-
Dome in Murias Chaos, Europa
-
Elsinore Corona, Miranda
-
Inverness Corona, Miranda
-
Plumes of Enceladus
-
Enceladus feeding the E ring
.jpg)
.png)
.jpg)
.png)
See also
- List of extraterrestrial volcanoes
- Extraterrestrial liquid water – Liquid water naturally occurring outside Earth
- Planetary oceanography – Study of extraterrestrial oceans
- Ice volcano – Wave-driven mound of ice formed on terrestrial lakes
- Frazil ice – Collections of ice crystals in open water
- Pingo – Mound of earth-covered ice
Notes
- Using an estimated surface area of at least 490,000 km for Cipango Planum, this significantly surpasses Olympus Mons's area of roughly 300,000 km. As Cipango Planum extended beyond Triton's terminator during Voyager 2's closest approach, its true extent is uncertain and may be significantly larger
References
- Liddell, Henry George; Scott, Robert (1940). "κρύος". A Greek–English Lexicon. Clarendon Press. Archived from the original on 12 January 2024. Retrieved 13 May 2024.
- ^ Hargitai, Henrik; Kereszturi, Ákos, eds. (2015). Encyclopedia of Planetary Landforms (first ed.). Springer New York. doi:10.1007/978-1-4614-3134-3. ISBN 978-1-4614-3133-6.
- ^ Gregg, Tracy K. P.; Lopes, Rosaly M. C.; Fagents, Sarah A. (December 2021). Planetary Volcanism across the Solar System. doi:10.1016/B978-0-12-813987-5.00005-5. ISBN 978-0-12-813987-5. S2CID 245084572. Retrieved 12 March 2024.
- ^ Geissler, Paul (2015). The Encyclopedia of Volcanoes (Second ed.). pp. 763–776. doi:10.1016/B978-0-12-385938-9.00044-4. ISBN 978-0-12-385938-9. Retrieved 12 March 2024.
- Fortes, A. D.; Gindrod, P. M.; Trickett, S. K.; Vočadlo, L. (May 2007). "Ammonium sulfate on Titan: Possible origin and role in cryovolcanism". Icarus. 188 (1): 139–153. Bibcode:2007Icar..188..139F. doi:10.1016/j.icarus.2006.11.002.
- ^ Croft, S. K.; Kargel, J. S.; Kirk, R. L.; et al. (1995). "The geology of Triton". Neptune and Triton: 879–947. Bibcode:1995netr.conf..879C.
- Schenk, P. M.; Beyer, R. A.; McKinnon, W. B.; Moore, J. M.; Spencer, J. R.; White, O. L.; Singer, K.; Nimmo, F.; Thomason, C.; Lauer, T. R.; Robbins, S.; Umurhan, O. M.; Grundy, W. M.; Stern, S. A.; Weaver, H. A.; Young, L. A.; Smith, K. E.; Olkin, C. (November 2018). "Basins, fractures and volcanoes: Global cartography and topography of Pluto from New Horizons". Icarus. 314: 400–433. Bibcode:2018Icar..314..400S. doi:10.1016/j.icarus.2018.06.008. S2CID 126273376.
- Sohn, Rebecca (1 April 2022). "Ice volcanoes on Pluto may still be erupting". Space.com.
- Moore, M. H.; Ferrante, R. F.; Hudson, R. L.; Stone, J. N. (September 2007). "Ammonia–water ice laboratory studies relevant to outer Solar System surfaces". Icarus. 190 (1): 260–273. Bibcode:2007Icar..190..260M. doi:10.1016/j.icarus.2007.02.020.
- ^ Manga, M.; Wang, C. -Y. (April 2007). "Pressurized oceans and the eruption of liquid water on Europa and Enceladus". Geophysical Research Letters. 34 (7). Bibcode:2007GeoRL..34.7202M. doi:10.1029/2007GL029297. Retrieved 12 March 2024.
- Moresi, Louis; Solomatov, Viatcheslav (1998). "Mantle convection with a brittle lithosphere: thoughts on the global tectonic styles of the Earth and Venus". Geophysical Journal International. 133 (3): 669–82. Bibcode:1998GeoJI.133..669M. CiteSeerX 10.1.1.30.5989. doi:10.1046/j.1365-246X.1998.00521.x.
- "Tidal heating and the long-term stability of a subsurface ocean on Enceladus" (PDF). Archived from the original (PDF) on 21 July 2010. Retrieved 14 October 2011.
- McGovern, J. C.; Nguyen, A. L. (April 2024). "The role of Pluto's ocean's salinity in supporting nitrogen ice loads within the Sputnik Planitia basin". Icarus. 412. Bibcode:2024Icar..41215968M. doi:10.1016/j.icarus.2024.115968. S2CID 267316007. Retrieved 13 March 2024.
- McCord, Thomas B. (2005). "Ceres: Evolution and current state". Journal of Geophysical Research. 110 (E5): E05009. Bibcode:2005JGRE..110.5009M. doi:10.1029/2004JE002244.
- Castillo-Rogez, J. C.; McCord, T. B.; Davis, A. G. (2007). "Ceres: evolution and present state" (PDF). Lunar and Planetary Science. XXXVIII: 2006–2007. Archived (PDF) from the original on 24 February 2011. Retrieved 25 June 2009.
- ^ Glein, Christopher R.; Grundy, William M.; Lunine, Jonathan I.; Wong, Ian; Protopapa, Silvia; Pinilla-Alonso, Noemi; Stansberry, John A.; Holler, Bryan J.; Cook, Jason C.; Souza-Feliciano, Ana Carolina (April 2024). "Moderate D/H ratios in methane ice on Eris and Makemake as evidence of hydrothermal or metamorphic processes in their interiors: Geochemical analysis". Icarus. 412. arXiv:2309.05549. Bibcode:2024Icar..41215999G. doi:10.1016/j.icarus.2024.115999. S2CID 261696907. Retrieved 12 March 2024.
- ^ Emery, J. P.; Wong, I.; Brunetto, R.; Cook, R.; Pinilla-Alonso, N.; Stansberry, J. A.; et al. (March 2024). "A Tale of 3 Dwarf Planets: Ices and Organics on Sedna, Gonggong, and Quaoar from JWST Spectroscopy". Icarus. 414 (116017). arXiv:2309.15230. Bibcode:2024Icar..41416017E. doi:10.1016/j.icarus.2024.116017.
- ^ Schmidt, Britney; Blankenship, Don; Patterson, Wes; Schenk, Paul (24 November 2011). "Active formation of 'chaos terrain' over shallow subsurface water on Europa". Nature. 479 (7374): 502–505. Bibcode:2011Natur.479..502S. doi:10.1038/nature10608. PMID 22089135. S2CID 4405195.
- Kargel, J. S. (1995). "Cryovolcanism on the Icy Satellites". Earth, Moon, and Planets. 67 (1–3): 101–113. Bibcode:1995EM&P...67..101K. doi:10.1007/BF00613296. S2CID 54843498. Retrieved 12 March 2024.
- Philpotts, Anthony R.; Ague, Jay J. (2009). Principles of igneous and metamorphic petrology (2nd ed.). Cambridge, UK: Cambridge University Press. pp. 53–55. ISBN 9780521880060.
- Landau, Elizabeth; Brown, Dwayne (6 March 2015). "NASA Spacecraft Becomes First to Orbit a Dwarf Planet". NASA. Archived from the original on 7 March 2015. Retrieved 6 March 2015.
- De Sanctis, M; Ammannito, E; Raponi, A; Frigeri, A; Ferrari, M; Carrozzo, F; Ciarniello, M; Formisano, M; Rousseau, B; Tosi, F.; Zambon, F.; Raymond, C. A.; Russell, C. T. (10 August 2020). "Fresh emplacement of hydrated sodium chloride on Ceres from ascending salty fluids". Nature Astronomy. 4 (8): 786–93. Bibcode:2020NatAs...4..786D. doi:10.1038/s41550-020-1138-8. S2CID 225442620.
- ^ Sori, Michael T.; Sizemore, Hanna G.; et al. (December 2018). "Cryovolcanic rates on Ceres revealed by topography". Nature Astronomy. 2 (12): 946–950. Bibcode:2018NatAs...2..946S. doi:10.1038/s41550-018-0574-1. S2CID 186800298. Archived from the original on 17 August 2021. Retrieved 17 August 2021.
- Schenk, Paul M.; Chapman, Clark R.; Zahnle, Kevin; and Moore, Jeffrey M. (2004) "Chapter 18: Ages and Interiors: the Cratering Record of the Galilean Satellites" Archived 24 December 2016 at the Wayback Machine, pp. 427 ff. in Bagenal, Fran; Dowling, Timothy E.; and McKinnon, William B., editors; Jupiter: The Planet, Satellites and Magnetosphere, Cambridge University Press, ISBN 0-521-81808-7.
- ^ Kattenhorn, Simon A. (March 2018). "Commentary: The Feasibility of Subduction and Implications for Plate Tectonics on Jupiter's Moon Europa". Journal of Geophysical Research: Planets. 123 (3): 684–689. Bibcode:2018JGRE..123..684K. doi:10.1002/2018JE005524.
- Figueredo, Patricio H.; Greeley, Ronald (February 2004). "Resurfacing history of Europa from pole-to-pole geological mapping". Icarus. 167 (2): 287–312. Bibcode:2004Icar..167..287F. doi:10.1016/j.icarus.2003.09.016.
- Fletcher, Leigh (12 December 2013). "The Plumes of Europa". The Planetary Society. Archived from the original on 15 December 2013. Retrieved 17 December 2013.
- "NASA's Hubble Spots Possible Water Plumes Erupting on Jupiter's Moon Europa". NASA. 26 September 2016. Retrieved 13 May 2015.
- Bradák, Balázs; Kereszturi, Ákos; Gomez, Christopher (November 2023). "Tectonic analysis of a newly identified putative cryovolcanic field on Europa". Advances in Space Research. 72 (9): 4064–4073. Bibcode:2023AdSpR..72.4064B. doi:10.1016/j.asr.2023.07.062. S2CID 260798414.
- "Argadnel Regio". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program. (Center Latitude: -14.60°, Center Longitude: 208.50°)
- Showman, Adam P.; Malhotra, Renu (1 October 1999). "The Galilean Satellites" (PDF). Science. 286 (5437): 77–84. doi:10.1126/science.286.5437.77. PMID 10506564. Archived (PDF) from the original on 14 May 2011. Retrieved 17 January 2008.
- Solomonidou, Anezina; Malaska, Michael; Stephan, Katrin; Soderlund, Krista; Valenti, Martin; Lucchetti, Alice; Kalousova, Klara; Lopes, Rosaly (September 2022). Ganymede paterae: a priority target for JUICE. 16th Europlanet Science Congress 2022. Palacio de Congresos de Granada, Spain and online. doi:10.5194/epsc2022-423.
- Patterson, G. Wesley; Collins, Geoffrey C.; Head, James W.; Pappalardo, Robert T.; Prockter, Louise M.; Lucchitta, Baerbel K.; Kay, Jonothan P. (6 December 2009). "Global geological mapping of Ganymede". Icarus. 207 (2): 845–867. Bibcode:2010Icar..207..845P. doi:10.1016/j.icarus.2009.11.035.
- "Enceladus rains water onto Saturn". ESA. 2011. Archived from the original on 23 November 2017. Retrieved 14 January 2015.
- Spahn, F.; et al. (10 March 2006). "Cassini Dust Measurements at Enceladus and Implications for the Origin of the E Ring". Science. 311 (5766): 1416–8. Bibcode:2006Sci...311.1416S. CiteSeerX 10.1.1.466.6748. doi:10.1126/science.1121375. PMID 16527969. S2CID 33554377.
- Porco, C. C.; Helfenstein, P.; Thomas, P. C.; Ingersoll, A. P.; Wisdom, J.; West, R.; Neukum, G.; Denk, T.; Wagner, R. (10 March 2006). "Cassini Observes the Active South Pole of Enceladus". Science. 311 (5766): 1393–1401. Bibcode:2006Sci...311.1393P. doi:10.1126/science.1123013. PMID 16527964. S2CID 6976648. Archived from the original on 16 June 2024. Retrieved 13 March 2024.
- ^ Thomas, P. C.; Tajeddine, R.; et al. (2016). "Enceladus's measured physical libration requires a global subsurface ocean". Icarus. 264: 37–47. arXiv:1509.07555. Bibcode:2016Icar..264...37T. doi:10.1016/j.icarus.2015.08.037. S2CID 118429372.
- Berne, A.; Simons, M.; Keane, J.T.; Leonard, E.J.; Park, R.S. (29 April 2024). "Jet activity on Enceladus linked to tidally driven strike-slip motion along tiger stripes". Nature Geoscience. 17 (5): 385–391. Bibcode:2024NatGe..17..385B. doi:10.1038/s41561-024-01418-0. ISSN 1752-0908.
- Iess, L.; Jacobson, R. A.; Ducci, M.; Stevenson, D. J.; Lunine, Jonathan I.; Armstrong, J. W.; Asmar, S. W.; Racioppa, P.; Rappaport, N. J.; Tortora, P. (2012). "The Tides of Titan". Science. 337 (6093): 457–9. Bibcode:2012Sci...337..457I. doi:10.1126/science.1219631. hdl:11573/477190. PMID 22745254. S2CID 10966007.
- Lopes, R. M. C.; Kirk, R. L.; Mitchell, K. L.; LeGall, A.; Barnes, J. W.; Hayes, A.; Kargel, J.; Wye, L.; Radebaugh, J.; Stofan, E. R.; Janssen, M. A.; Neish, C. D.; Wall, S. D.; Wood, C. A.; Lunine, Jonathan I.; Malaska, M. J. (19 March 2013). "Cryovolcanism on Titan: New results from Cassini RADAR and VIMS" (PDF). Journal of Geophysical Research: Planets. 118 (3): 416–435. Bibcode:2013JGRE..118..416L. doi:10.1002/jgre.20062. Archived (PDF) from the original on 1 September 2019. Retrieved 2 September 2019.
- ^ Wood, C.A.; Radebaugh, J. (2020). "Morphologic Evidence for Volcanic Craters near Titan's North Polar Region". Journal of Geophysical Research: Planets. 125 (8): e06036. Bibcode:2020JGRE..12506036W. doi:10.1029/2019JE006036. S2CID 225752345.
- ^ Bolles, Dana (March 2024). "Voyager 2". NASA. Archived from the original on 18 May 2024. Retrieved 21 May 2024.
- Leonard, Erin Janelle; Beddingfield, Chloe B.; Elder, Catherine M.; Nordheim, Tom Andrei (December 2022). The Geologic History of Miranda's Inverness Corona. AGU Fall Meeting 2022. Chicago, Illinois. Bibcode:2022AGUFM.P32E1872L.
- ^ Schenk, Paul M.; Moore, Jeffrey M. (December 2020). "Topography and geology of Uranian mid-sized icy satellites in comparison with Saturnian and Plutonian satellites". Philosophical Transactions of the Royal Society A. 378 (2187). Bibcode:2020RSPTA.37800102S. doi:10.1098/rsta.2020.0102. PMID 33161858.
- Sulcanese, Davide; Cioria, Camilla; Kokin, Osip; Mitri, Giuseppe; Pondrelli, Monica; Chiarolanza, Giancula (March 2023). "Geological analysis of Monad Regio, Triton: Possible evidence of endogenic and exogenic processes". Icarus. 392. Bibcode:2023Icar..39215368S. doi:10.1016/j.icarus.2022.115368. S2CID 254173536. Retrieved 12 March 2024.
- Schenk, Paul M.; Zahnle, Kevin (December 2007). "On the negligible surface age of Triton". Icarus. 192 (1): 135–149. Bibcode:2007Icar..192..135S. doi:10.1016/j.icarus.2007.07.004.
- Martin-Herrero, Alvaro; Romeo, Ignacio; Ruiz, Javier (2018). "Heat flow in Triton: Implications for heat sources powering recent geologic activity". Planetary and Space Science. 160: 19–25. Bibcode:2018P&SS..160...19M. doi:10.1016/j.pss.2018.03.010. S2CID 125508759.
- ^ Schenk, Paul; Beddingfield, Chloe; Bertrand, Tanguy; et al. (September 2021). "Triton: Topography and Geology of a Probable Ocean World with Comparison to Pluto and Charon". Remote Sensing. 13 (17): 3476. Bibcode:2021RemS...13.3476S. doi:10.3390/rs13173476.
- Frankel, C.S. (2005). Worlds on Fire: Volcanoes on the Earth, the Moon, Mars, Venus and Io; Cambridge University Press: Cambridge, UK, p. 132. ISBN 978-0-521-80393-9.
- ^ McKinnon, William B.; Kirk, Randolph L. (2014). Encyclopedia of the Solar System (Third ed.). pp. 861–881. doi:10.1016/C2010-0-67309-3. ISBN 978-0-12-415845-0. Retrieved 12 March 2024.
- Martin-Herrero, A.; Ruiz, J.; Romeo, I. (March 2014). Characterization and Possible Origin of Sub-Circular Depressions in Ruach Planitia Region, Triton (PDF). 45th Lunar and Planetary Science Conference. The Woodlands, Texas. Bibcode:2014LPI....45.1177M. Archived (PDF) from the original on 12 March 2024. Retrieved 13 March 2024.
- Hofgartner, Jason D.; Birch, Samuel P. D.; Castillo, Julie; Grundy, Will M.; Hansen, Candice J.; Hayes, Alexander G.; Howett, Carly J. A.; Hurford, Terry A.; Martin, Emily S.; Mitchell, Karl L.; Nordheim, Tom A.; Poston, Michael J.; Prockter, Louise M.; Quick, Lynnae C.; Schenk, Paul (15 March 2022). "Hypotheses for Triton's plumes: New analyses and future remote sensing tests". Icarus. 375: 114835. arXiv:2112.04627. Bibcode:2022Icar..37514835H. doi:10.1016/j.icarus.2021.114835. ISSN 0019-1035.
- "NASA's Three-Billion-Mile Journey to Pluto Reaches Historic Encounter". Johns Hopkins University Applied Physics Laboratory. 14 July 2015. Archived from the original on 14 November 2021. Retrieved 18 May 2024.
- "At Pluto, New Horizons Finds Geology of All Ages, Possible Ice Volcanoes, Insight into Planetary Origins". New Horizons News Center. The Johns Hopkins University Applied Physics Laboratory LLC. 9 November 2015. Archived from the original on 4 March 2016. Retrieved 9 November 2015.
- Witze, A. (9 November 2015). "Icy volcanoes may dot Pluto's surface". Nature. Nature Publishing Group. doi:10.1038/nature.2015.18756. S2CID 182698872. Archived from the original on 17 November 2015. Retrieved 9 November 2015.
- Singer, Kelsi N. (29 March 2022). "Large-scale cryovolcanic resurfacing on Pluto". Nature Communications. 13 (1): 1542. arXiv:2207.06557. Bibcode:2022NatCo..13.1542S. doi:10.1038/s41467-022-29056-3. PMC 8964750. PMID 35351895.
- Cruikshank, Dale P.; Umurhan, Orkan M.; Beyer, Ross A.; Schmitt, Bernard; Keane, James T.; Runyon, Kirby D.; Atri, Dimitra; White, Oliver L.; Matsuyama, Isamu; Moore, Jeffrey M.; McKinnon, William B.; Sandford, Scott A.; Singer, Kelsi N.; Grundy, William M.; Dalle Ore, Cristina M.; Cook, Jason C.; Bertrand, Tanguy; Stern, S. Alan; Olkin, Catherine B.; Weaver, Harold A.; Young, Leslie A.; Spencer, John R.; Lisse, Carey M.; Binzel, Richard P.; Earle, Alissa M.; Robbins, Stuart J.; Gladstone, G. Randall; Cartwright, Richard J.; Ennico, Kimberly (15 September 2019). "Recent cryovolcanism in Virgil Fossae on Pluto". Icarus. 330: 155–168. Bibcode:2019Icar..330..155C. doi:10.1016/j.icarus.2019.04.023. S2CID 149983734.
- Ahrens, C. J.; Chevrier, V. F. (March 2021). "Investigation of the morphology and interpretation of Hekla Cavus, Pluto". Icarus. 356. Bibcode:2021Icar..35614108A. doi:10.1016/j.icarus.2020.114108.
- Emran, A.; Dalle Ore, C. M.; Cruikshank, D. P.; Cook, J. C. (March 2021). "Surface composition of Pluto's Kiladze area and relationship to cryovolcanism". Icarus. 404. arXiv:2303.17072. Bibcode:2023Icar..40415653E. doi:10.1016/j.icarus.2023.115653.
- McKinnon, W. B.; et al. (1 June 2016). "Convection in a volatile nitrogen-ice-rich layer drives Pluto's geological vigour". Nature. 534 (7605): 82–85. arXiv:1903.05571. Bibcode:2016Natur.534...82M. doi:10.1038/nature18289. PMID 27251279. S2CID 30903520.
- Desch, S. J.; Neveu, M. (2017). "Differentiation and cryovolcanism on Charon: A view before and after New Horizons". Icarus. 287: 175–186. Bibcode:2017Icar..287..175D. doi:10.1016/j.icarus.2016.11.037. Archived from the original on 1 October 2017. Retrieved 13 March 2024.
- Witze, Alexandra (2015). "Ice volcanoes may dot Pluto's surface". Nature. doi:10.1038/nature.2015.18756. S2CID 182698872. Archived from the original on 17 November 2015. Retrieved 15 November 2015.
- Saxena, Prabal; Renaud, Joe P.; Henning, Wade G.; Jutzi, Martin; Hurford, Terry (March 2018). "Relevance of tidal heating on large TNOs". Icarus. 302: 245–260. arXiv:1706.04682. Bibcode:2018Icar..302..245S. doi:10.1016/j.icarus.2017.11.023.
