Burney (crater)

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Burney
Burney Basin Pluto.png
A New Horizons of Burney basin, center. An ancient impact basin, its heavily eroded state makes it difficult to discern; its concentric rings are only slightly brighter than the surrounding plains
Feature typeMulti-ring impact basin
Location Venera Terra, Pluto
Coordinates 45°41′N133°47′E / 45.683°N 133.783°E / 45.683; 133.783 [1]
Diameter296–350 km (184–217 mi) [1] [2]
Depth~1.8–3 km (1.1–1.9 mi) [2] [3] :123
Discoverer New Horizons
Eponym Venetia Burney

Burney, sometimes referred to as the Burney basin, [4] [5] is the second-largest known impact basin on the dwarf planet Pluto. With a diameter of over 290 kilometers and possibly up to 350 kilometers, it is the second-largest known impact basin on Pluto, after the Sputnik Planitia basin. Burney is the only impact basin with visible multiple rings known on Pluto and is thus classified as a multi-ringed impact basin, [lower-alpha 1] though its rings have been heavily eroded due to Burney's age.

Contents

Discovery and naming

As with the rest of Pluto's surface features, Burney was first seen on the New Horizons flyby of Pluto and its five moons on 14 July 2015. The impact basin was informally named Burney by the New Horizons team in honor of Venetia Burney, who suggested the name Pluto to the dwarf planet's discoverer Clyde Tombaugh in 1930. [7] [8] :10 The name was officially approved by the International Astronomical Union (IAU) on 8 August 2017. [1]

Geology

PIA20200-Pluto-BurneyBasin-CratersPlains-20150714.jpg
A high-resolution New Horizons image of a section of Burney and its interior craters. One of Burney's rings form a chain of mountains that arcs across the image. Scale bar of 6 mi (9.7 km) is at the top left
Burney Topology.png
A topography map of Burney, where its Mare Orientale-style degraded peak rings and central depression are much more apparent

Burney is the second-largest impact feature known on Pluto, after the massive basin that encloses Sputnik Planitia. [3] :123 It is ancient, with an estimated age of at least 4 billion years old, and heavily eroded. [9] [3] :142 The structure of Burney resembles that of the Mare Orientale basin on the Moon, with a series of concentric peak rings that enclose a central depression. Burney's degraded state makes it difficult to discern its extent due to the subtle nature of its peak rings; Burney may have anywhere from 2-4 such rings. As such, estimates for Burney's diameter range from ~290 kilometers to ~350 kilometers. [2] [1] The peak rings of Burney are discontinuous and crenulated, standing roughly 500-1,000 meters high. The central depression of Burney is approximately 180 kilometers across and roughly 1.8-3 kilometers deep. [2] [3] :123 Within Burney are numerous smaller impact craters, one of which has been officially named Hardaway. [10]

Much of Burney basin is glaciated, its surface covered in bright, coarse grains of nitrogen ice mixed with water ice. [11] [12] The peak rings of Burney are additionally coated in methane ice, indicating that methane preferentially condenses on high-altitude mountain peaks within Burney. By contrast, Burney's floor is poor in methane ice and much smoother than the surrounding plains, possibly from differences in erosion or from heavier glaciation. [9] [3] :127–128 Several dark streaks similar to those found in Sputnik Planitia were observed in and around Burney. [13] Models of Pluto's climate indicate that Burney likely experiences downward-flowing katabatic winds. [14]

Surrounding Burney basin is a broad region to the northwest of Sputnik Planitia that hosts a type of terrain informally called washboard terrain. This terrain is characterized by parallel ridges spaced 1-2 kilometers apart and covers large parts of Burney's basin floor. One hypothesis for the origin of the washboard terrain is from the collection and deposition of material from ancient glaciation. The age of the washboard terrain appears to only marginally postdate the impact event that created Burney. [9]

See also

Notes

  1. Simonelli, a similarly-sized crater on the anti-encounter hemisphere of Pluto, may have multiple rings. [3] :123 Sputik Planitia basin, though much larger, does not have visible rings; any such features are buried beneath its nitrogen glaciers. The blocky mountains alongside Sputnik Planitia's western border may be related to a peak ring within the basin. [6]

Related Research Articles

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

Pluto is a dwarf planet in the Kuiper belt, a ring of bodies beyond the orbit of Neptune. It is the ninth-largest and tenth-most-massive known object to directly orbit the Sun. It is the largest known trans-Neptunian object by volume, by a small margin, but is less massive than Eris. Like other Kuiper belt objects, Pluto is made primarily of ice and rock and is much smaller than the inner planets. Pluto has roughly one-sixth the mass of Earth's moon, and one-third its volume.

<span class="mw-page-title-main">Charon (moon)</span> Largest natural satellite of Pluto

Charon, known as (134340) Pluto I, is the largest of the five known natural satellites of the dwarf planet Pluto. It has a mean radius of 606 km (377 mi). Charon is the sixth-largest known trans-Neptunian object after Pluto, Eris, Haumea, Makemake, and Gonggong. It was discovered in 1978 at the United States Naval Observatory in Washington, D.C., using photographic plates taken at the United States Naval Observatory Flagstaff Station (NOFS).

<span class="mw-page-title-main">Hellas Planitia</span> Plantia on Mars

Hellas Planitia is a plain located within the huge, roughly circular impact basin Hellas located in the southern hemisphere of the planet Mars. Hellas is the third- or fourth-largest known impact crater in the Solar System. The basin floor is about 7,152 m (23,465 ft) deep, 3,000 m (9,800 ft) deeper than the Moon's South Pole-Aitken basin, and extends about 2,300 km (1,400 mi) east to west. It is centered at 42.4°S 70.5°E. Hellas Planitia spans the boundary between the Hellas quadrangle and the Noachis quadrangle.

<span class="mw-page-title-main">Cryovolcano</span> Type of volcano that erupts volatiles such as water, ammonia or methane, instead of molten rock

A cryovolcano 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.

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

The geology of Pluto consists of the characteristics of the surface, crust, and interior of Pluto. Because of Pluto's distance from Earth, in-depth study from Earth is difficult. Many details about Pluto remained unknown until 14 July 2015, when New Horizons flew through the Pluto system and began transmitting data back to Earth. When it did, Pluto was found to have remarkable geologic diversity, with New Horizons team member Jeff Moore saying that it "is every bit as complex as that of Mars". The final New Horizons Pluto data transmission was received on 25 October 2016. In June 2020, astronomers reported evidence that Pluto may have had a subsurface ocean, and consequently may have been habitable, when it was first formed.

<span class="mw-page-title-main">Moons of Pluto</span> Natural satellites orbiting Pluto

The dwarf planet Pluto has five natural satellites. In order of distance from Pluto, they are Charon, Styx, Nix, Kerberos, and Hydra. Charon, the largest, is mutually tidally locked with Pluto, and is massive enough that Pluto and Charon are sometimes considered a binary dwarf planet.

<span class="mw-page-title-main">Acidalia Planitia</span> Planitia on Mars

Acidalia Planitia is a plain on Mars, between the Tharsis volcanic province and Arabia Terra to the north of Valles Marineris, centered at 49.8°N 339.3°E. Most of this region is found in the Mare Acidalium quadrangle, but a small part is in the Ismenius Lacus quadrangle. The plain contains the famous Cydonia region at the contact with the heavily cratered highland terrain.

<span class="mw-page-title-main">Tombaugh Regio</span> Bright region on Pluto

Tombaugh Regio, sometimes nicknamed "Pluto's heart" after its shape, is the largest bright surface feature of the dwarf planet Pluto. It lies just north of Pluto's equator, to the northeast of Belton Regio and to the northwest of Safronov Regio, which are both dark features. Its western lobe, a 1,000 km (620 mi)-wide plain of nitrogen and other ices lying within a basin, is named Sputnik Planitia. The eastern lobe consists of high-albedo uplands thought to be coated by nitrogen transported through the atmosphere from Sputnik Planitia, and then deposited as ice. Some of this nitrogen ice then returns to Sputnik Planitia via glacial flow. The region is named after Clyde Tombaugh, the discoverer of Pluto.

<span class="mw-page-title-main">Belton Regio</span> Equatorial dark region on Pluto

Belton Regio is a prominent surface feature of the dwarf planet Pluto. It is an elongated dark region along Pluto's equator, 2,990 km (1,860 mi) long and one of the darkest features on its surface.

<span class="mw-page-title-main">Mordor Macula</span> North polar dark region on Charon

Mordor Macula is the informal name for a large dark area about 475 km in diameter near the north pole of Charon, Pluto's largest moon. It is named after the black land called Mordor in J.R.R. Tolkien's The Lord of the Rings.

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

The geology of Charon encompasses the characteristics of the surface, crust, and interior of Pluto's moon Charon. Like the geology of Pluto, almost nothing was known of Charon's geology until the New Horizons of the Pluto system on 14 July 2015. Charon's diameter is 1,208 km (751 mi)—just over half that of Pluto. Charon is sufficiently massive to have collapsed into a spheroid under its own gravity.

<span class="mw-page-title-main">Geography of Pluto</span>

The geography of Pluto refers to the study and mapping of physical features across the dwarf planet Pluto. On 14 July 2015, the New Horizons spacecraft became the first spacecraft to fly by Pluto. During its brief flyby, New Horizons made detailed geographical measurements and observations of Pluto and its moons.

<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.

Challenger Colles is a range of hills on Pluto near the eastern edge of Sputnik Planitia. Discovered by the New Horizons team in July 2015, It is named in honor of the Space Shuttle Challenger, which was destroyed with all seven crew lost on January 28, 1986. The name Challenger Colles was officially approved by the International Astronomical Union on May 27, 2022.

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

Vulcan Planitia, or Vulcan Planum, is the unofficial name given to a large plain on the southern hemisphere of Pluto's moon Charon. It discovered by New Horizons during its flyby of Pluto in July 2015. It is named after the fictional planet Vulcan in the science-fiction series Star Trek. The name is not approved by International Astronomical Union (IAU) as of 2024.

<span class="mw-page-title-main">Coleta de Dados Colles</span> Range of hills on Pluto

The Coleta de Dados Colles are a cluster of hills ("colles") on the smooth plains of Sputnik Planitia on Pluto. The hills are over 100 km from the major mountain ranges to the west, and appear to be blocks of water ice floating in the denser nitrogen ice of Sputnik Planitia. The hills were informally named on July 28, 2015, by the research team of the New Horizons mission after the first Brazilian satellite, the Satélite de Coleta de Dados. The ridge's name has yet to be recognized officially by the IAU.

<span class="mw-page-title-main">Wright Mons</span> Mountain on Pluto

Wright Mons is a large, roughly circular mountain and likely cryovolcano on the dwarf planet Pluto. Discovered by the New Horizons spacecraft in 2015, it is located southwest of Sputnik Planitia within Hyecho Palus, adjacent to the Tenzing Montes and Belton Regio. A relatively young geological feature, Wright Mons has attracted attention as one of the most apparent examples of recent geological activity on Pluto and borders numerous other similarly young features. Numerous semi-regular hills surround and partially construct the flanks of Wright Mons. Their nature remains unexplained, with few, if any, direct analogs elsewhere in the Solar System.

<span class="mw-page-title-main">Dorothy (Charonian crater)</span> Largest crater on Charon

Dorothy is the largest known impact basin on Pluto's moon Charon. The crater was discovered by the New Horizons space probe in 2015 during its flyby of Pluto and its moons. It was named after Dorothy Gale from the novel The Wonderful Wizard of Oz. The crater is located near Charon's north pole, and overlaps the edge of Mordor Macula.

<span class="mw-page-title-main">Climate of Pluto</span> Types of climate on the dwarf planet Pluto

The climate of Pluto concerns the atmospheric dynamics, weather, and long-term trends on the dwarf planet Pluto. Five climate zones are assigned on the dwarf planet: tropics, arctic, tropical arctic, diurnal, and polar. These climate zones are delineated based on astronomically defined boundaries or sub-solar latitudes, which are not associated with the atmospheric circulations on the dwarf planet. Charon, the largest moon of Pluto, is tidally locked with it, and thus has the same climate zone structure as Pluto itself.

References

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