Kraken Catena

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Kraken Catena
Kraken and Set Catena.png
Kraken Catena and nearby Set Catena, highlighted with arrows. The two pit chains are aligned radially from nearby Leviathan Patera
Feature typeCrater chain, tectonic rift
LocationMonad Regio, Triton
Coordinates 14°00′N35°30′E / 14.000°N 35.500°E / 14.000; 35.500 [1]
Discoverer Voyager 2
Eponym Kraken

Kraken Catena is a pit chain (catena) and likely tectonic fault [2] on Triton, the largest natural satellite of Neptune. It, along with Set Catena, is located near and is aligned approximately radially from Leviathan Patera, a major cryovolcanic feature; as such, Kraken Catena may have played a role in rift-induced cryovolcanic activity in Leviathan Patera. [2] [3] Several of Kraken Catena's pits have central steep-sided knobs, giving a moated appearance similar to the moated mountains found on Pluto's moon Charon and Uranus's moon Ariel. [3]

As with all other surface features of Triton, Kraken Catena was discovered when Voyager 2 visited the Neptune system on 25 August 1989. It is named after the Kraken of Norse mythology; the name was officially approved by the International Astronomical Union (IAU) in 1991. It is located at 14°N, 35.5°E, within Cipango Planum and Monad Regio. [1]

See also

Related Research Articles

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<span class="mw-page-title-main">Pluto</span> Dwarf planet

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<span class="mw-page-title-main">Natural satellite</span> Astronomical body that orbits a planet

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<span class="mw-page-title-main">Macula (planetary geology)</span> Unusually dark area on the surface of a planet or moon

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<span class="mw-page-title-main">Crater chain</span> Line of craters along the surface of an astronomical body

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Planetary oceanography, also called astro-oceanography or exo-oceanography, is the study of oceans on planets and moons other than Earth. Unlike other planetary sciences like astrobiology, astrochemistry, and planetary geology, it only began after the discovery of underground oceans in Saturn's moon Titan and Jupiter's moon Europa. This field remains speculative until further missions reach the oceans beneath the rock or ice layer of the moons. There are many theories about oceans or even ocean worlds of celestial bodies in the Solar System, from oceans made of diamond in Neptune to a gigantic ocean of liquid hydrogen that may exist underneath Jupiter's surface.

<span class="mw-page-title-main">Geology of Charon</span> Geologic structure and composition of Charon

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<span class="mw-page-title-main">Sputnik Planitia</span> Glaciated basin on Pluto

Sputnik Planitia is a large, partially glaciated basin on Pluto. About 1,400 by 1,200 km in size, Sputnik Planitia is partially submerged in large, bright glaciers of nitrogen ice. Named after Earth's first artificial satellite, Sputnik 1, it constitutes the western lobe of the heart-shaped Tombaugh Regio. Sputnik Planitia lies mostly in the northern hemisphere, but extends across the equator. Much of it has a surface of irregular polygons separated by troughs, interpreted as convection cells in the relatively soft nitrogen ice. The polygons average about 33 km (21 mi) across. In some cases troughs are populated by blocky mountains or hills, or contain darker material. There appear to be windstreaks on the surface with evidence of sublimation. The dark streaks are a few kilometers long and all aligned in the same direction. The planitia also contains pits apparently formed by sublimation. No craters were detectable by New Horizons, implying a surface less than 10 million years old. Modeling sublimation pit formation yields a surface age estimate of 180000+90000
−40000
years. Near the northwest margin is a field of transverse dunes, spaced about 0.4 to 1 km apart, that are thought to be composed of 200-300 μm diameter particles of methane ice derived from the nearby Al-Idrisi Montes.

<span class="mw-page-title-main">Vulcan Planitia</span> Major plain on Charon

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<span class="mw-page-title-main">Patera (planetary nomenclature)</span> Irregular type of crater

PateraPAT-ər-ə is an irregular crater, or a complex crater with scalloped edges on a celestial body. Paterae can have any origin, although the majority of them were created by volcanism. The term comes from Latin, where it refers to a shallow bowl used in antique cultures.

<span class="mw-page-title-main">Set Catena</span> Catena on Triton

Set Catena is a pit chain (catena) and likely tectonic fault located on Triton, the largest natural satellite of Neptune. It, along with Kraken Catena, is located near Leviathan Patera, a major cryovolcanic feature; as such, Set Catena may have played a role in rift-induced cryovolcanic activity in Leviathan Patera. Set Catena extends radially northwards from Leviathan Patera, terminating at another irregularly-shaped walled depression. Set Catena consists of semi-regularly spaced pits roughly 20 km separated from each other, with each pit being on average 10 km wide and up to 500 m deep. The pits may have formed from collapse or from explosive cryovolcanic eruptions, and may have been subsequently expanded by mass wasting processes.

<span class="mw-page-title-main">Leviathan Patera</span> Caldera on Triton

Leviathan Patera is a major cryovolcanic caldera on Neptune's largest moon Triton. Discovered by the Voyager 2 spacecraft in 1989, Leviathan Patera is located in Monad Regio and within Cipango Planum's western regions. Leviathan Patera is approximately 80 kilometers in diameter and may be the center of one of the largest cryovolcanic or volcanic edifices in the Solar System.

<span class="mw-page-title-main">Geology of Triton</span> Geologic structure and composition of Triton

The geology of Triton encompasses the physical characteristics of the surface, internal structure, and geological history of Neptune's largest moon Triton. With a mean density of 2.061 g/cm3, Triton is roughly 15-35% water ice by mass; Triton is a differentiated body, with an icy solid crust atop a probable subsurface ocean and a rocky core. As a result, Triton's surface geology is largely driven by the dynamics of water ice and other volatiles such as nitrogen and methane. Triton's geology is vigorous, and has been and continues to be influenced by its unusual history of capture, high internal heat, and its thin but significant atmosphere.

<span class="mw-page-title-main">Tuonela Planitia</span> Walled plain on Triton

Tuonela Planitia is an elongated plain and probable cryolava lake on Neptune's moon Triton. Located in Triton's northern hemisphere within Monad Regio, it overlies part of Triton's unusual cantaloupe terrain. As with neighboring Ruach Planitia and other walled plains on Triton, Tuonela Planitia is among the youngest features on Triton's surface.

<span class="mw-page-title-main">Ruach Planitia</span> Walled plain on Triton

Ruach Planitia is a roughly circular flat plain and probable cryolava lake on Neptune's moon Triton. It is located in Triton's northern hemisphere within Monad Regio and directly borders the cryovolcanic plains of Cipango Planum. Ruach Planitia, along with the other walled plains on Triton, is one of the youngest and flattest features on Triton.

References

  1. 1 2 "USGS Astro: Planetary Nomenclature: Feature Data Search Results". Archived from the original on 2006-09-24. Retrieved 2010-04-09.
  2. 1 2 Stern, A. S.; McKinnon, W. B. (March 1999). Triton's Surface Age and Impactor Population Revisited (Evidence for an Internal Ocean) (PDF). 30th Annual Lunar and Planetary Science Conference. Houston, TX. Bibcode:1999LPI....30.1766S. 1766.
  3. 1 2 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 .