List of tallest mountains in the Solar System

Olympus Mons on Mars, the tallest planetary mountain in the Solar System, compared to Mount Everest and Mauna Kea on Earth (both elevations are sea-level-to-peak).

This is a list of the tallest mountains in the Solar System. The tallest peak or peaks on worlds where significant mountains have been measured are given; in some cases, the tallest peaks of different classes on a world are also listed. At 21.9 km, the enormous shield volcano Olympus Mons on Mars is the tallest mountain on any planet. For 40 years, following its discovery in 1971, it was the tallest mountain known in the Solar System. However, in 2011, the central peak of the crater Rheasilvia on the asteroid and protoplanet Vesta was found to be of comparable height.[lower-alpha 1]


The heights are given as base-to-peak, because there is no nonarbitrary equivalent to height above sea level on other worlds.

World Tallest peak(s) Height % of radius[lower-alpha 2] Origin Notes
01 Mercury Caloris Montes 0303 km (1.9 mi)[1][2] 0123 0.12 impact[3] Formed by the Caloris impact
02 Venus Skadi Mons 0646.4 km (4.0 mi) (approx.)[4] 0106 0.11 tectonic[5] Has radar-bright slopes due to metallic Venus snow, possibly lead sulfide[6]
Maat Mons 0494.9 km (3.0 mi) (approx.)[7] 0081 0.081 volcanic[8] Highest volcano on Venus
03 Earth Mauna Kea and Mauna Loa 10210.2 km (6.3 mi)[9] 0160 0.16 volcanic Just 4.2 km (2.6 mi) of this is above sea level
Pico del Teide 0757.5 km (4.7 mi)[10] 0118 0.12 volcanic Rises 3.7 km above sea level[10]
Denali 0565.3 to 5.9 km (3.3 to 3.7 mi)[11] 0093 0.093 tectonic Tallest mountain base-to-peak on land[12][lower-alpha 3]
Mount Everest 0413.6 to 4.6 km (2.2 to 2.9 mi)[13] 0072 0.072 tectonic 4.6 km on north face, 3.6 km on south face.[lower-alpha 4]
04 Moon Mons Huygens 0555.5 km (3.4 mi)[14][15] 0317 0.32 impact Formed by the Imbrium impact
Mons Hadley 0454.5 km (2.8 mi)[14][15] 0259 0.26 impact Formed by the Imbrium impact
Mons Rümker 0111.1 km (0.68 mi)[16] 0063 0.063 volcanic Largest volcanic construct on the Moon[16]
05 Mars Olympus Mons 219 21.9 km (14 mi)[17][18] 0646 0.65 volcanic Rises 26 km above northern plains,[19] 1000 km away. Summit calderas are 60 x 80 km wide, up to 3.2 km deep;[18] scarp around margin is up to 8 km high.[20]
Ascraeus Mons 14914.9 km (9.3 mi)[17] 0440 0.44 volcanic Tallest of the three Tharsis Montes
Elysium Mons 12612.6 km (7.8 mi)[17] 0372 0.37 volcanic Highest volcano in Elysium
Arsia Mons 117 11.7 km (7.3 mi)[17] 0345 0.35 volcanic Summit caldera is 108 to 138 km (67 to 86 mi) across[17]
Pavonis Mons 084 8.4 km (5.2 mi)[17] 0248 0.25 volcanic Summit caldera is 4.8 km (3.0 mi) deep[17]
Anseris Mons 062 6.2 km (3.9 mi)[21] 0183 0.18 impact Among the highest nonvolcanic peaks on Mars, formed by the Hellas impact
Aeolis Mons ("Mount Sharp") 050 4.5 to 5.5 km (2.8 to 3.4 mi)[22][lower-alpha 5] 0162 0.16 depositional[lower-alpha 6] Formed from deposits in Gale crater; MSL rover's long-term prime destination,[26] reached in November 2014.[27]
06 Vesta Rheasilvia central peak 22022 km (14 mi)[28][29] 8370 8.4 impact Almost 200 km (120 mi) wide. See also: List of largest craters in the Solar System
07 Ceres Ahuna Mons 0404 km (2.5 mi)[30] 0853 0.85 cryovolcanic[31] Isolated steep-sided dome in relatively smooth area; max. height of ~ 5 km on steepest side; roughly antipodal to largest impact basin on Ceres
08 Io Boösaule Montes "South"[32] 17817.5 to 18.2 km (10.9 to 11.3 mi)[33] 0999 1.0 tectonic Has a 15 km (9 mi) high scarp on its SE margin[34]
Ionian Mons east ridge 12712.7 km (7.9 mi) (approx.)[34][35] 0697 0.70 tectonic Has the form of a curved double ridge
Euboea Montes 11810.3 to 13.4 km (6.4 to 8.3 mi)[36] 0736 0.74 tectonic A NW flank landslide left a 25,000 km3 debris apron[37][lower-alpha 7]
unnamed (245° W, 30° S) 0202.5 km (1.6 mi) (approx.)[38][39] 013 0.14 volcanic One of the tallest of Io's many volcanoes, with an atypical conical form[39][lower-alpha 8]
09 Mimas Herschel central peak 0707 km (4 mi) (approx.)[41] 3530 3.5 impact See also: List of largest craters in the Solar System
10 Dione Janiculum Dorsa 0151.5 km (0.9 mi)[42] 0267 0.27 tectonic[lower-alpha 9] Surrounding crust depressed ca. 0.3 km.
11 Titan Mithrim Montes 033373.3 km (2.1 mi)[44] 013 0.13 tectonic[44] May have formed due to global contraction[45]
Doom Mons 01451.45 km (0.90 mi)[46] 0056 0.056 cryovolcanic[46] Adjacent to Sotra Patera, a 1.7 km (1.1 mi) deep collapse feature[46]
12 Iapetus equatorial ridge 20020 km (12 mi) (approx.)[47] 2720 2.7 uncertain[lower-alpha 10] Individual peaks have not been measured
13 Oberon unnamed ("limb mountain") 11011 km (7 mi) (approx.)[41] 1440 1.4 impact (?) A value of 6 km was given shortly after the Voyager 2 encounter[51]
14 Pluto Piccard Mons[lower-alpha 11][52][53] 056 ~5.6 km (3.5 mi)[54] 0473 0.47 cryovolcanic (?) ~220 km across[54]
Wright Mons[lower-alpha 11][52][53] 040 ~4.0 km (2.5 mi)[52] 0330 0.34 cryovolcanic (?) ~160 km across;[52] summit depression ~56 km across[55]
Norgay Montes[lower-alpha 11][56] 0353.5 km (2.2 mi)[57] 0295 0.30 tectonic[57] (?) Composed of water ice;[57] named after Tenzing Norgay[58]

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

See also


  1. Olympus Mons, however, is a much broader peak; its diameter is similar to that of Vesta itself.
  2. 100 x ratio of peak height to radius of the parent world
  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. About 5.25 km (3.26 mi) high from the perspective of the landing site of Curiosity.[23]
  6. 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.[22] However, if the deposition was due to katabatic winds, 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.[24][25]
  7. Among the Solar System's largest[37]
  8. 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.[40] 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.[40]
  9. Was apparently formed via contraction.[43]
  10. Hypotheses of origin include crustal readjustment associated with a decrease in oblateness due to tidal locking,[48][49] and deposition of deorbiting material from a former ring around the moon.[50]
  11. 1 2 3 Name not yet approved by the IAU
  12. 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.


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