List of tallest mountains in the Solar System

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Olympus Mons, the tallest planetary mountain in the Solar System, compared to Mount Everest and Mauna Kea on Earth (heights shown are above datum or sea level, which differ from the base-to-peak heights given in the list). Olympus Mons Side View.svg
Olympus Mons, the tallest planetary mountain in the Solar System, compared to Mount Everest and Mauna Kea on Earth (heights shown are above datum or sea level, which differ from the base-to-peak heights given in the list).

This is a list of the tallest mountains in the Solar System. This list includes peaks on all celestial bodies where significant mountains have been detected. For some celestial bodies, different peaks are given across different types of measurement. The solar system's tallest mountain is possibly the Olympus Mons on Mars with an altitude of 21.9 to 26 km. The central peak of Rheasilvia on the asteroid Vesta is also a candidate to be the tallest, with an estimated at up to between 20 and 25 km from peak to base.

Contents

List

Heights are given from base to peak (although a precise definition for mean base level is lacking). Peak elevations above sea level are only available on Earth, and possibly Titan. [1] On other planets, peak elevations above an equipotential surface or a reference ellipsoid could be used if enough data is available for the calculation, but this is often not the case.

PlanetTallest peak(s)Base-to-peak height% of radius [n 1] OriginNotes
Mercury Caloris Montes ≤ 3 km (1.9 mi) [2] [3] 0.12 impact [4] Formed by the Caloris impact
Venus Skadi Mons (Maxwell Montes massif)6.4 km (4.0 mi) [5] (11 km above mean)0.11 tectonic [6] Has radar-bright slopes due to metallic Venus snow, possibly lead sulfide [7]
Maat Mons 4.9 km (3.0 mi) (approx.) [8] 0.081 volcanic [9] Highest volcano on Venus
Mauna Kea and Mauna Loa 10.2 km (6.3 mi) [11] 0.16 volcanic 4.2 km (2.6 mi) of this is above sea level
Haleakalā 9.1 km (5.7 mi) [12] 0.14 volcanic Rises 3.1 km above sea level [12]
Pico del Teide 7.5 km (4.7 mi) [13] 0.12 volcanic Rises 3.7 km above sea level [13]
Denali 5.3 to 5.9 km (3.3 to 3.7 mi) [14] 0.093 tectonic Tallest mountain base-to-peak on land [15] [n 3]
Mount Everest 3.6 to 4.6 km (2.2 to 2.9 mi) [16] 0.072 tectonic 4.6 km on north face, 3.6 km on south face; [n 4] highest elevation (8.8 km) above sea level, as well as by wet and dry prominence (but not among the tallest from base to peak, and in distance to Earth's center Mt Chimborazo rises highest).
Moon [n 5] Mons Huygens 5.5 km (3.4 mi) [19] [20] 0.32 impact Formed by the Imbrium impact. Not highest lunar peak by prominence, which would be Selenean summit.
Mons Hadley 4.5 km (2.8 mi) [19] [20] 0.26 impact Formed by the Imbrium impact
Mons Rümker 1.3 km (0.81 mi) [21] 0.063 volcanic Largest volcanic construct on the Moon [21]
Mars Olympus Mons 21.9–26 km (13.6–16.2 mi; 72,000–85,000 ft) [n 6] [22] [23] [24] 0.65 volcanic Tallest mountain in the Solar System. Rises 26 km above northern plains, [25] (dry prominence) 1000 km away. Summit calderas are 60 x 80 km wide, up to 3.2 km deep; [24] scarp around margin is up to 8 km high. [26] A shield volcano, the mean flank slope is a modest 5.2 degrees. [23]
Ascraeus Mons 14.9 km (9.3 mi) [23] 0.44 volcanic Tallest of the three Tharsis Montes
Elysium Mons 12.6 km (7.8 mi) [23] 0.37 volcanic Highest volcano in Elysium
Arsia Mons 11.7 km (7.3 mi) [23] 0.35 volcanic Summit caldera is 108 to 138 km (67 to 86 mi) across [23]
Pavonis Mons 8.4 km (5.2 mi) [23] 0.25 volcanic Summit caldera is 4.8 km (3.0 mi) deep [23]
Anseris Mons 6.2 km (3.9 mi) [27] 0.18 impact Among the highest nonvolcanic peaks on Mars, formed by the Hellas impact
Aeolis Mons ("Mount Sharp")4.5 to 5.5 km (2.8 to 3.4 mi) [28] [n 7] 0.16 deposition and erosion [n 8] Formed from deposits in Gale crater; [33] the MSL rover has been ascending it since November 2014. [34]
Vesta Rheasilvia central peak 20–25 km (12–16 mi; 66,000–82,000 ft) [n 9] [35] [36] 8.4 impact Almost 200 km (120 mi) wide. See also: List of largest craters in the Solar System
Ceres Ahuna Mons 4 km (2.5 mi) [37] 0.85 cryovolcanic [38] Isolated steep-sided dome in relatively smooth area; max. height of ~ 5 km on steepest side; roughly antipodal to largest impact basin on Ceres
Io Boösaule Montes "South" [39] 17.5 to 18.2 km (10.9 to 11.3 mi) [40] 1.0 tectonic Has a 15 km (9 mi) high scarp on its SE margin [41]
Ionian Mons east ridge12.7 km (7.9 mi) (approx.) [41] [42] 0.70 tectonic Has the form of a curved double ridge
Euboea Montes 10.5 to 13.4 km (6.5 to 8.3 mi) [43] 0.74 tectonic A NW flank landslide left a 25,000 km3 debris apron [44] [n 10]
unnamed (245° W, 30° S)2.5 km (1.6 mi) (approx.) [45] [46] 0.14 volcanic One of the tallest of Io's many volcanoes, with an atypical conical form [46] [n 11]
Mimas Herschel central peak 7 km (4 mi) (approx.) [48] 3.5 impact See also: List of largest craters in the Solar System
Dione Janiculum Dorsa 1.5 km (0.9 mi) [49] 0.27 tectonic [n 12] Surrounding crust depressed ca. 0.3 km.
Titan Mithrim Montes ≤ 3.3 km (2.1 mi) [52] 0.13 tectonic [52] May have formed due to global contraction [53]
Doom Mons 1.45 km (0.90 mi) [54] 0.056 cryovolcanic [54] Adjacent to Sotra Patera, a 1.7 km (1.1 mi) deep collapse feature [54]
Iapetus equatorial ridge 20 km (12 mi) (approx.) [55] 2.7 uncertain [n 13] Individual peaks have not been measured
Oberon unnamed ("limb mountain")11 km (7 mi) (approx.) [48] 1.4 impact (?)A value of 6 km was given shortly after the Voyager 2 encounter [59]
Pluto Tenzing Montes, peak "T2"~6.2 km (3.9 mi) [60] 0.52 tectonic [61] (?)Composed of water ice; [61] named after Tenzing Norgay [62]
Piccard Mons [63] [64] ~5.5 km (3.4 mi) [60] 0.46 cryovolcanic (?)~220 km across; [65] central depression is 11 km deep [60]
Wright Mons [63] [64] ~4.7 km (2.9 mi) [60] 0.40 cryovolcanic (?)~160 km across; [63] summit depression ~56 km across [66] and 4.5 km deep [60]
Charon Butler Mons [67] ≥ 4.5 km (2.8 mi) [67] 0.74 tectonic (?) Vulcan Planitia, the southern plains, has several isolated peaks, possibly tilted crustal blocks [67]
Dorothy central peak [67] ~4.0 km (2.5 mi) [67] 0.66 impact North polar impact basin Dorothy, Charon's largest, is ~240 km across and 6 km deep [67]
2002 MS4 unnamed20–29 km (12–18 mi)6.3 ?Discovered by stellar occultation; it is unclear whether this feature may be a genuine topographic peak or a transiting/occulting satellite. [68]

Tallest mountains by elevation

The following images are shown in order of decreasing base-to-peak height.

See also

Notes

  1. ↑ 100 × ratio of peak height to radius of the parent world
  2. ↑ On Earth, mountain heights are constrained by glaciation; peaks are usually limited to elevations not more than 1500 m above the snow line (which varies with latitude). Exceptions to this trend tend to be rapidly forming volcanoes. [10]
  3. ↑ On p. 20 of Helman (2005): "the base to peak rise of Mount McKinley is the largest of any mountain that lies entirely above sea level, some 18,000 ft (5,500 m)"
  4. ↑ Peak is 8.8 km (5.5 mi) above sea level, and over 13 km (8.1 mi) above the oceanic abyssal plain.
  5. ↑ Prominences in crater rims are not typically viewed as peaks and have not been listed here. A notable example is an (officially) unnamed massif on the rim of the farside crater Zeeman that rises about 4.0 km above adjacent parts of the rim and about 7.57 km above the crater floor. [17] The formation of the massif does not appear to be explainable simply on the basis of the impact event. [18]
  6. ↑ Due to limitations in the accuracy of the measurements and the lack of a precise definition of "base", it is difficult to say whether this peak or the central peak of Vesta's crater Rheasilvia is the tallest mountain in the Solar System.
  7. ↑ About 5.25 km (3.26 mi) high from the perspective of the landing site of Curiosity. [29]
  8. ↑ A crater central peak may sit below the mound of sediment. If that sediment was deposited while the crater was flooded, the crater may have once been entirely filled before erosional processes gained the upper hand. [28] However, if the deposition was due to katabatic winds that descend the crater walls, as suggested by reported 3 degree radial slopes of the mound's layers, the role of erosion would have been to place an upper limit on the mound's growth. [30] [31] Gravity measurements by Curiosity suggest the crater was never buried by sediment, consistent with the latter scenario. [32]
  9. ↑ Due to limitations in the accuracy of the measurements and the lack of a precise definition of "base", it is difficult to say whether this peak or the volcano Olympus Mons on Mars is the tallest mountain in the Solar System.
  10. ↑ Among the Solar System's largest [44]
  11. ↑ Some of Io's paterae are surrounded by radial patterns of lava flows, indicating they are on a topographic high point, making them shield volcanoes. Most of these volcanoes exhibit relief of less than 1 km. A few have more relief; Ruwa Patera rises 2.5 to 3 km over its 300 km width. However, its slopes are only on the order of a degree. [47] A handful of Io's smaller shield volcanoes have steeper, conical profiles; the example listed is 60 km across and has slopes averaging 4° and reaching 6-7° approaching the small summit depression. [47]
  12. ↑ Was apparently formed via contraction. [50] [51]
  13. ↑ Hypotheses of origin include crustal readjustment associated with a decrease in oblateness due to tidal locking, [56] [57] and deposition of deorbiting material from a former ring around the moon. [58]
  14. ↑ A linearized wide-angle hazcam image that makes the mountain look steeper than it actually is. The highest peak is not visible in this view.

Related Research Articles

<span class="mw-page-title-main">Olympus Mons</span> Martian volcano, tallest point on Mars

Olympus Mons is a shield volcano on Mars. It is over 21.9 km high as measured by the Mars Orbiter Laser Altimeter (MOLA), and is about two and a half times Mount Everest's height above sea level. It is Mars's tallest volcano, its tallest planetary mountain, and is approximately tied with Rheasilvia on Vesta as the tallest mountain currently discovered in the Solar System. It is associated with the volcanic region of Tharsis Montes. It last erupted 25 million years ago.

<span class="mw-page-title-main">Ascraeus Mons</span> Martian volcano

Ascraeus Mons is a large shield volcano located in the Tharsis region of the planet Mars. It is the northernmost and tallest of three shield volcanoes collectively known as the Tharsis Montes.

<span class="mw-page-title-main">Arsia Mons</span> Martian volcano

Arsia Mons is the southernmost of three volcanoes on the Tharsis bulge near the equator of the planet Mars. To its north is Pavonis Mons, and north of that is Ascraeus Mons. The tallest volcano in the Solar System, Olympus Mons, is to its northwest. Its name comes from a corresponding albedo feature on a map by Giovanni Schiaparelli, which he named in turn after the legendary Roman forest of Arsia Silva. Historically, it was known as Nodus Gordii before being renamed.

<span class="mw-page-title-main">Io (moon)</span> Innermost of the four Galilean moons of Jupiter

Io, or Jupiter I, is the innermost and second-smallest of the four Galilean moons of the planet Jupiter. Slightly larger than Earth's moon, Io is the fourth-largest moon in the Solar System, has the highest density of any moon, the strongest surface gravity of any moon, and the lowest amount of water by atomic ratio of any known astronomical object in the Solar System. It was discovered in 1610 by Galileo Galilei and was named after the mythological character Io, a priestess of Hera who became one of Zeus's lovers.

<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 gasses and volatile material such as liquid water, ammonia, and hydrocarbons, collectively referred to as cryolava, from a reservoir of subsurface cryomagma. These 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">Hecates Tholus</span> Martian volcano

Hecates Tholus is a Martian volcano, notable for results from the European Space Agency's Mars Express mission which indicate a major eruption took place 350 million years ago. The eruption created a caldera 10 km in diameter on the volcano's western flank.

<span class="mw-page-title-main">Elysium (volcanic province)</span> 2nd-largest volcanic region of Mars

Elysium, located in the Elysium and Cebrenia quadrangles, is the second largest volcanic region on Mars, after Tharsis. The region includes the volcanoes Hecates Tholus, Elysium Mons and Albor Tholus. The province is centered roughly on Elysium Mons at 24.7°N 150°E. Elysium Planitia is a broad plain to the south of Elysium, centered at 3.0°N 154.7°E. Another large volcano, Apollinaris Mons, lies south of Elysium Planitia and is not part of the province. Besides having large volcanoes, Elysium has several areas with long trenches, called fossa or fossae (plural) on Mars. They include the Cerberus Fossae, Elysium Fossae, Galaxias Fossae, Hephaestus Fossae, Hyblaeus Fossae, Stygis Fossae and Zephyrus Fossae.

<span class="mw-page-title-main">Elysium Mons</span> Martian volcano

Elysium Mons is a volcano on Mars located in the volcanic province Elysium, at 25.02°N 147.21°E, in the Martian eastern hemisphere. It stands about 12.6 km (41,000 ft) above its base, and about 14.1 km (46,000 ft) above the Martian datum, making it the third tallest Martian mountain in terms of relief and the fourth highest in elevation. Its diameter is about 240 km (150 mi), with a summit caldera about 14 km (8.7 mi) across. It is flanked by the smaller volcanoes Hecates Tholus to the northeast, and Albor Tholus to the southeast.

<span class="mw-page-title-main">Geology of Mars</span> Scientific study of the surface, crust, and interior of the planet Mars

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<span class="mw-page-title-main">Tooting (crater)</span> Volcanic crater on Mars

Tooting is an impact crater with volcanic features at 23.1°N, 207.1°E, in Amazonis Planitia, due west of the volcano Olympus Mons, on Mars. It was identified by planetary geologist Peter Mouginis-Mark in September 2004. Scientists estimate that its age is on the order of hundreds of thousands of years, which is relatively young for a Martian crater. A later study confirms this order of magnitude estimate. A preliminary paper describing the geology and geometry of Tooting was published in 2007 by the journal Meteoritics and Planetary Science, vol. 42, pages 1615–1625. Further papers have been published, including a 2010 analysis of flows on the walls of Tooting crater by A. R. Morris et al., and a 2012 review paper by P.J. Mouginis-Mark and J.M. Boyce in Chemie der Erde Geochemistry, vol. 72, p. 1–23. A geologic map has also been submitted in 2012 to the U.S. Geological Survey for consideration and future publication.

<span class="mw-page-title-main">Volcanism on Mars</span> Overview of volcanism in the geological history of Mars

Volcanic activity, or volcanism, has played a significant role in the geologic evolution of Mars. Scientists have known since the Mariner 9 mission in 1972 that volcanic features cover large portions of the Martian surface. These features include extensive lava flows, vast lava plains, and the largest known volcanoes in the Solar System. Martian volcanic features range in age from Noachian to late Amazonian, indicating that the planet has been volcanically active throughout its history, and some speculate it probably still is so today. Both Earth and Mars are large, differentiated planets built from similar chondritic materials. Many of the same magmatic processes that occur on Earth also occurred on Mars, and both planets are similar enough compositionally that the same names can be applied to their igneous rocks and minerals.

<span class="mw-page-title-main">Tharsis quadrangle</span> Map of Mars

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<span class="mw-page-title-main">Ceraunius Tholus</span> Martian volcano

Ceraunius Tholus is a volcano on Mars located in the Tharsis quadrangle at 24.25° north latitude and 262.75° east longitude, part of the Uranius group of volcanoes. It is 130 kilometres (81 mi) across, approximately 8,500 metres (27,887 ft) high and is named after a classical albedo feature name.

<span class="mw-page-title-main">Mount Sharp</span> Martian mountain

Mount Sharp, officially Aeolis Mons, is a mountain on Mars. It forms the central peak within Gale crater and is located around 5.08°S 137.85°E, rising 5.5 km (18,000 ft) high from the valley floor. Its ID in the United States Geological Survey's Gazetteer of Planetary Nomenclature is 15000.

<span class="mw-page-title-main">Mons (planetary nomenclature)</span>

Mons is a mountain on a celestial body. The term is used in planetary nomenclature: it is a part of the international names of such features. It is capitalized and usually stands after the proper given name, but stands before it in the case of lunar mountains.

<span class="mw-page-title-main">Geology of Ceres</span>

The geology of Ceres consists of the characteristics of the surface, the crust and the interior of the dwarf planet Ceres. The surface of Ceres is comparable to the surfaces of Saturn's moons Rhea and Tethys, and Uranus's moons Umbriel and Oberon.

<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">Volcanism on the Moon</span> Volcanic processes and landforms on the Moon

Volcanism on the Moon is represented by the presence of volcanoes, pyroclastic deposits and vast lava plains on the lunar surface. The volcanoes are typically in the form of small domes and cones that form large volcanic complexes and isolated edifices. Calderas, large-scale collapse features generally formed late in a volcanic eruptive episode, are exceptionally rare on the Moon. Lunar pyroclastic deposits are the result of lava fountain eruptions from volatile-laden basaltic magmas rapidly ascending from deep mantle sources and erupting as a spray of magma, forming tiny glass beads. However, pyroclastic deposits formed by less common non-basaltic explosive eruptions are also thought to exist on the Moon. Lunar lava plains cover large swaths of the Moon's surface and consist mainly of voluminous basaltic flows. They contain a number of volcanic features related to the cooling of lava, including lava tubes, rilles and wrinkle ridges.

References

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