Movatterモバイル変換

[0]ホーム
URL:

Jump to content
WikipediaThe Free Encyclopedia
Search

List of tallest mountains in the Solar System

From Wikipedia, the free encyclopedia

Olympus Mons, the tallest planetary mountain in the Solar System, compared toMount Everest andMauna Kea on Earth (heights shown are abovedatum orsea level, which differ from the base-to-peak heights given in the list).

This is alist of the tallest mountains in the Solar System. This list includes peaks on allcelestial 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 theOlympus Mons onMars with an altitude of 21.9 to 26 km. The central peak ofRheasilvia on the asteroidVesta is also a candidate to be the tallest, with an estimated at up to between 19 and 22 km from peak to base.

List

[edit]

Heights are given from base to peak (although a precise definition for mean base level is lacking). Peak elevations abovesea level are only available on Earth, and possiblyTitan.[1] On other planets, peak elevations above anequipotential surface or areference 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
MercuryCaloris Montes≤ 3 km (1.9 mi)[2][3]0.12impact[4]Formed by theCaloris impact
VenusSkadi Mons (Maxwell Montes massif)6.4 km (4.0 mi)[5] (11 km above mean)0.11tectonic[6]Has radar-bright slopes due to metallicVenus snow, possiblylead sulfide[7]
Maat Mons4.9 km (3.0 mi) (approx.)[8]0.081volcanic[9]Highest volcano on Venus
Earth[n 2]Mauna Kea andMauna Loa10.2 km (6.3 mi)[11]0.16volcanic4.2 km (2.6 mi) of this is above sea level
Haleakalā9.1 km (5.7 mi)[12]0.14volcanicRises 3.1 km above sea level[12]
Pico del Teide7.5 km (4.7 mi)[13]0.12volcanicRises 3.7 km above sea level[13]
Denali (Mount McKinley)5.3 to 5.9 km (3.3 to 3.7 mi)[14]0.093tectonicTallest mountain base-to-peak on land[15][n 3]
Mount Everest3.6 to 4.6 km (2.2 to 2.9 mi)[16]0.072tectonic4.6 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 dryprominence (but not among the tallest from base to peak, nor in distance to Earth's center, asMt Chimborazo rises highest).
Moon[n 5]Mons Huygens5.3 km (3.3 mi)[20]0.31impactFormed by theImbrium impact.
Mons Mouton6 km (3.7 mi)[20]0.35impactPossibly formed by the South Pole-Aitken basin impact.
Southern Farside Mountain7 km (4.3 mi)[20]0.40impactInformal name of the Moon's tallest free-standing mountain. Possibly formed by the South Pole-Aitken basin impact. Not highest lunar peak byprominence, which would beSelenean summit.
Mons Hadley4.5 km (2.8 mi)[21][22]0.26impactFormed by theImbrium impact
Mons Rümker1.3 km (0.81 mi)[23]0.063volcanicLargest volcanic construct on the Moon[23]
MarsOlympus Mons21.9–26 km (13.6–16.2 mi; 72,000–85,000 ft)[n 6][24][25][26]0.65volcanicTallest mountain in theSolar System. Rises 26 km above northern plains,[27] (dryprominence) 1000 km away. Summit calderas are 60×80 km wide, up to 3.2 km deep;[26] scarp around margin is up to 8 km high.[28] Ashield volcano, the mean flank slope is a modest 5.2 degrees.[25]
Ascraeus Mons14.9 km (9.3 mi)[25]0.44volcanicTallest of the threeTharsis Montes
Elysium Mons12.6 km (7.8 mi)[25]0.37volcanicHighest volcano inElysium
Arsia Mons11.7 km (7.3 mi)[25]0.35volcanicSummitcaldera is 108 to 138 km (67 to 86 mi) across[25]
Pavonis Mons8.4 km (5.2 mi)[25]0.25volcanicSummit caldera is 4.8 km (3.0 mi) deep[25]
Anseris Mons6.2 km (3.9 mi)[29]0.18impactAmong the highest nonvolcanic peaks on Mars, formed by theHellas impact
Aeolis Mons ("Mount Sharp")4.5 to 5.5 km (2.8 to 3.4 mi)[30][n 7]0.16deposition anderosion[n 8]Formed from deposits inGale crater;[35] theMSL rover has been ascending it since November 2014.[36]
VestaRheasilviacentral peak[37]20–22 km (12–14 mi; 66,000–72,000 ft)[n 9][38][39]8.4impactAlmost 200 km (120 mi) wide. See also:List of largest craters in the Solar System
CeresAhuna Mons4 km (2.5 mi)[40]0.85cryovolcanic[41]Isolated steep-sided dome in relatively smooth area; max. height of ~ 5 km on steepest side; roughlyantipodal tolargest impact basin on Ceres
IoBoösaule Montes "South"[42]17.5 to 18.2 km (10.9 to 11.3 mi)[43]1.0tectonicHas a 15 km (9 mi) high scarp on its SE margin[44]
Ionian Mons east ridge12.7 km (7.9 mi) (approx.)[44][45]0.70tectonicHas the form of a curved double ridge
Euboea Montes10.5 to 13.4 km (6.5 to 8.3 mi)[46]0.74tectonicA NW flank landslide left a 25,000 km3 debris apron[47][n 10]
unnamed (245° W, 30° S)2.5 km (1.6 mi) (approx.)[48][49]0.14volcanicOne of the tallest of Io's many volcanoes, with an atypical conical form[49][n 11]
MimasHerschelcentral peak7 km (4 mi) (approx.)[51]3.5impactSee also:List of largest craters in the Solar System
DioneJaniculum Dorsa1.5 km (0.9 mi)[52]0.27tectonic[n 12]Surrounding crust depressed ca. 0.3 km.
TitanMithrim Montes≤ 3.3 km (2.1 mi)[55]0.13tectonic[55]May have formed due to global contraction[56]
Doom Mons1.45 km (0.90 mi)[57]0.056cryovolcanic[57]Adjacent toSotra Patera, a 1.7 km (1.1 mi) deep collapse feature[57]
Iapetusequatorial ridge20 km (12 mi) (approx.)[58]2.7uncertain[n 13]Individual peaks have not been measured
Oberonunnamed ("limb mountain")11 km (7 mi) (approx.)[51]1.4impact (?)A value of 6 km was given shortly after theVoyager 2 encounter[62]
PlutoTenzing Montes, peak "T2"~6.2 km (3.9 mi)[63]0.52tectonic[64] (?)Composed of water ice;[64] named afterTenzing Norgay[65]
Piccard Mons[66][67]~5.5 km (3.4 mi)[63]0.46cryovolcanic (?)~220 km across;[68] central depression is 11 km deep[63]
Wright Mons[66][67]~4.7 km (2.9 mi)[63]0.40cryovolcanic (?)~160 km across;[66] summit depression ~56 km across[69] and 4.5 km deep[63]
CharonButler Mons[70]≥ 4.5 km (2.8 mi)[70]0.74tectonic (?)Vulcan Planitia, the southern plains, has several isolated peaks, possibly tilted crustal blocks[70]
Dorothycentral peak[70]~4.0 km (2.5 mi)[70]0.66impactNorth polar impact basin Dorothy, Charon's largest, is ~240 km across and 6 km deep[70]
Mániunnamed25 km (16 mi)[71]6.3impact[71]Discovered bystellar occultation; it is unclear whether this feature is a genuine topographic peak or atransiting/occulting satellite.[71]

Tallest mountains by elevation

[edit]

Gallery

[edit]

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

See also

[edit]

Notes

[edit]
  1. ^100 × ratio of peak height toradius of the parent world
  2. ^On Earth, mountain heights are constrained byglaciation; peaks are usually limited to elevations not more than 1500 m above thesnow line (which varies withlatitude). 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 oceanicabyssal plain.
  5. ^Prominences in crater rims are not typically viewed as peaks[citation needed] and have not been listed here. The highest point on the Moon is the so-calledSelenean summit at5°26′28″N158°39′22″W / 5.441°N 158.656°W /5.441; -158.656, a crater rim on the lunar highland, having an elevation of 10.629 kilometres (6.605 mi).[17] A notable example is an (officially) unnamed massif on the rim of the farside craterZeeman that rises about 4.0 km above adjacent parts of the rim and about 7.57 km above the crater floor.[18] The formation of the massif does not appear to be explainable simply on the basis of the impact event.[19]
  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 ofCuriosity.[31]
  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 beforeerosional processes gained the upper hand.[30] However, if the deposition was due tokatabatic 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.[32][33] Gravity measurements byCuriosity suggest the crater was never buried by sediment, consistent with the latter scenario.[34]
  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[47]
  11. ^Some ofIo'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.[50] 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.[50]
  12. ^Was apparently formed via contraction.[53][54]
  13. ^Hypotheses of origin include crustal readjustment associated with a decrease inoblateness due totidal locking,[59][60] and deposition of deorbiting material from a formerring around the moon.[61]
  14. ^A linearized wide-anglehazcam image that makes the mountain look steeper than it actually is. The highest peak is not visible in this view.

References

[edit]
  1. ^Hayes, A.G.; Birch, S.P.D.; Dietrich, W.E.; Howard, A.D.; Kirk, R.L.; Poggiali, V.; Mastrogiuseppe, M.; Michaelides, R.J.; Corlies, P.M.; Moore, J.M.; Malaska, M.J.; Mitchell, K.L.; Lorenz, R.D.; Wood, C.A. (2017)."Topographic Constraints on the Evolution and Connectivity of Titan's Lacustrine Basins".Geophysical Research Letters.44 (23): 11,745–11, 753.Bibcode:2017GeoRL..4411745H.doi:10.1002/2017GL075468.hdl:11573/1560393.
  2. ^"Surface".MESSENGER web site.Johns Hopkins University/Applied Physics Lab. Archived from the original on 30 September 2016. Retrieved4 April 2012.
  3. ^Oberst, J.; Preusker, F.; Phillips, R. J.; Watters, T. R.; Head, J. W.; Zuber, M. T.; Solomon, S. C. (2010). "The morphology of Mercury's Caloris basin as seen in MESSENGER stereo topographic models".Icarus.209 (1):230–238.Bibcode:2010Icar..209..230O.doi:10.1016/j.icarus.2010.03.009.ISSN 0019-1035.
  4. ^Fassett, C. I.; Head, J. W.; Blewett, D. T.; Chapman, C. R.; Dickson, J. L.; Murchie, S. L.; Solomon, S. C.; Watters, T. R. (2009). "Caloris impact basin: Exterior geomorphology, stratigraphy, morphometry, radial sculpture, and smooth plains deposits".Earth and Planetary Science Letters.285 (3–4):297–308.Bibcode:2009E&PSL.285..297F.doi:10.1016/j.epsl.2009.05.022.ISSN 0012-821X.
  5. ^Jones, Tom; Stofan, Ellen (2008).Planetology: Unlocking the secrets of the solar system. Washington, D.C.: National Geographic Society. p. 74.ISBN 978-1-4262-0121-9.Archived from the original on 16 July 2017. Retrieved25 October 2016.
  6. ^Keep, M.; Hansen, V. L. (1994). "Structural history of Maxwell Montes, Venus: Implications for Venusian mountain belt formation".Journal of Geophysical Research.99 (E12): 26015.Bibcode:1994JGR....9926015K.doi:10.1029/94JE02636.ISSN 0148-0227.
  7. ^Otten, Carolyn Jones (10 February 2004)."'Heavy metal' snow on Venus is lead sulfide".Newsroom.Washington University in St. Louis.Archived from the original on 29 January 2016. Retrieved10 December 2012.
  8. ^"PIA00106: Venus - 3D Perspective View of Maat Mons".Planetary Photojournal.Jet Propulsion Lab. 1 August 1996.Archived from the original on 8 March 2016. Retrieved30 June 2012.
  9. ^Robinson, C. A.; Thornhill, G. D.; Parfitt, E. A. (January 1995)."Large-scale volcanic activity at Maat Mons: Can this explain fluctuations in atmospheric chemistry observed by Pioneer Venus?".Journal of Geophysical Research.100 (E6):11755–11764.Bibcode:1995JGR...10011755R.doi:10.1029/95JE00147.Archived from the original on 1 March 2012. Retrieved11 February 2013.
  10. ^Egholm, D. L.; Nielsen, S. B.; Pedersen, V. K.; Lesemann, J.-E. (2009). "Glacial effects limiting mountain height".Nature.460 (7257):884–887.Bibcode:2009Natur.460..884E.doi:10.1038/nature08263.PMID 19675651.S2CID 205217746.
  11. ^"Mountains: Highest Points on Earth". National Geographic Society. Archived fromthe original on 6 March 2012. Retrieved19 September 2010.
  12. ^ab"Haleakala National Park Geology Fieldnotes". U.S. National Park Service.Archived from the original on 2 February 2017. Retrieved31 January 2017.
  13. ^ab"Teide National Park".UNESCO World Heritage Site list.UNESCO.Archived from the original on 12 June 2022. Retrieved2 June 2013.
  14. ^"NOVA Online: Surviving Denali, The Mission".NOVA web site. Public Broadcasting Corporation. 2000.Archived from the original on 20 November 2010. Retrieved7 June 2007.
  15. ^Adam Helman (2005).The Finest Peaks: Prominence and Other Mountain Measures. Trafford Publishing.ISBN 978-1-4120-5995-4.Archived from the original on 31 October 2020. Retrieved9 December 2012.
  16. ^Mount Everest (1:50,000 scale map), prepared under the direction ofBradford Washburn for the Boston Museum of Science, the Swiss Foundation for Alpine Research, and theNational Geographic Society, 1991,ISBN 3-85515-105-9
  17. ^Li, ChunLai; Ren, Xin; Liu, JianJun; Zou, XiaoDuan; Mu, LingLi; Wang, JianYu; Shu, Rong; Zou, YongLiao; Zhang, HongBo; Lü, Chang; Liu, JianZhong; Zuo, Wei; Su, Yan; Wen, WeiBin; Bian, Wei; Wang, Min; Xu, Chun; Kong, DeQing; Wang, XiaoQian; Wang, Fang; Geng, Liang; Zhang, ZhouBin; Zheng, Lei; Zhu, XinYing; Li, JunDuo; Ouyang, ZiYuan (2010). "Laser altimetry data of Chang'E-1 and the global lunar DEM model".Science China Earth Sciences.53 (11):1582–1593.doi:10.1007/s11430-010-4020-1.ISSN 1674-7313.
  18. ^Robinson, M. (20 November 2017)."Mountains of the Moon: Zeeman Mons".LROC.sese.asu. Arizona State University.Archived from the original on 12 November 2021. Retrieved5 September 2020.
  19. ^Ruefer, A.C.; James, P.B. (March 2020).Zeeman Crater's Anomalous Massif(PDF). 51st Lunar and Planetary Science Conference. p. 2673.Bibcode:2020LPI....51.2673R.Archived(PDF) from the original on 9 September 2021. Retrieved5 September 2020.
  20. ^abcThe Moon's Highs and Lows
  21. ^Fred W. Price (1988).The Moon observer's handbook. London: Cambridge University Press.ISBN 978-0-521-33500-3.
  22. ^Moore, Patrick (2001).On the Moon. London: Cassell & Co.ISBN 978-0-304-35469-6.
  23. ^abWöhler, C.; Lena, R.; Pau, K. C. (16 March 2007).The Lunar Dome Complex Mons Rümker: Morphometry, Rheology, and Mode of Emplacement. 38th Lunar and Planetary Science Conference. p. 1091.Bibcode:2007LPI....38.1091W.
  24. ^Neil F. Comins (2012).Discovering the Essential Universe. W. H. Freeman. p. 148.ISBN 978-1-4292-5519-6.
  25. ^abcdefghPlescia, J. B. (2004)."Morphometric properties of Martian volcanoes".Journal of Geophysical Research.109 (E3): E03003.Bibcode:2004JGRE..109.3003P.doi:10.1029/2002JE002031.ISSN 0148-0227.
  26. ^abCarr, Michael H. (11 January 2007).The Surface of Mars. Cambridge University Press. p. 51.ISBN 978-1-139-46124-5.Archived from the original on 24 June 2021. Retrieved25 October 2016.
  27. ^Comins, Neil F. (4 January 2012).Discovering the Essential Universe. Macmillan.ISBN 978-1-4292-5519-6.Archived from the original on 9 November 2021. Retrieved23 December 2012.
  28. ^Lopes, R.; Guest, J. E.; Hiller, K.; Neukum, G. (January 1982)."Further evidence for a mass movement origin of the Olympus Mons aureole".Journal of Geophysical Research.87 (B12):9917–9928.Bibcode:1982JGR....87.9917L.doi:10.1029/JB087iB12p09917.
  29. ^JMARS MOLA elevation dataset. Christensen, P.; Gorelick, N.; Anwar, S.; Dickenshied, S.; Edwards, C.; Engle, E. (2007) "New Insights About Mars From the Creation and Analysis of Mars Global DatasetsArchived 5 October 2018 at theWayback Machine;" American Geophysical Union, Fall Meeting, abstract #P11E-01.
  30. ^ab"Gale Crater's History Book".Mars Odyssey THEMIS web site.Arizona State University.Archived from the original on 4 November 2008. Retrieved7 December 2012.
  31. ^Anderson, R. B.; Bell III, J. F. (2010). "Geologic mapping and characterization of Gale Crater and implications for its potential as a Mars Science Laboratory landing site".International Journal of Mars Science and Exploration.5:76–128.Bibcode:2010IJMSE...5...76A.doi:10.1555/mars.2010.0004.
  32. ^Wall, M. (6 May 2013)."Bizarre Mars Mountain Possibly Built by Wind, Not Water".Space.com.Archived from the original on 7 November 2016. Retrieved13 May 2013.
  33. ^Kite, E. S.; Lewis, K. W.; Lamb, M. P.; Newman, C. E.; Richardson, M. I. (2013). "Growth and form of the mound in Gale Crater, Mars: Slope wind enhanced erosion and transport".Geology.41 (5):543–546.arXiv:1205.6840.Bibcode:2013Geo....41..543K.doi:10.1130/G33909.1.ISSN 0091-7613.S2CID 119249853.
  34. ^Lewis, K. W.; Peters, S.; Gonter, K.; Morrison, S.; Schmerr, N.; Vasavada, A. R.; Gabriel, T. (2019)."A surface gravity traverse on Mars indicates low bedrock density at Gale crater".Science.363 (6426):535–537.Bibcode:2019Sci...363..535L.doi:10.1126/science.aat0738.PMID 30705193.S2CID 59567599.
  35. ^Agle, D. C. (28 March 2012)."'Mount Sharp' On Mars Links Geology's Past and Future".NASA.Archived from the original on 6 March 2017. Retrieved31 March 2012.
  36. ^Webster, Gay; Brown, Dwayne (9 November 2014)."Curiosity Arrives at Mount Sharp".NASA Jet Propulsion Laboratory. Archived fromthe original on 2 December 2014. Retrieved16 October 2016.
  37. ^Mid-continent Research for Education and Learning: McREL."Dawn Mission: News & Events > New View of Vesta Mountain from NASA's Dawn Mission".dawn.jpl.nasa.gov. Archived fromthe original on 17 October 2013. Retrieved9 October 2025.
  38. ^Vega, P. (11 October 2011)."New View of Vesta Mountain From NASA's Dawn Mission".Jet Propulsion Lab's Dawn mission web site.NASA. Archived fromthe original on 22 October 2011. Retrieved29 March 2012.
  39. ^Schenk, P.; Marchi, S.; O'Brien, D. P.; Buczkowski, D.; Jaumann, R.; Yingst, A.; McCord, T.; Gaskell, R.; Roatsch, T.; Keller, H. E.; Raymond, C.A.; Russell, C. T. (1 March 2012). "Mega-Impacts into Planetary Bodies: Global Effects of the Giant Rheasilvia Impact Basin on Vesta".43rd Lunar and Planetary Science Conference.Lunar and Planetary Science Conference. No. 1659. p. 2757.Bibcode:2012LPI....43.2757S. contribution 1659, id.2757.
  40. ^"Dawn's First Year at Ceres: A Mountain Emerges".JPL Dawn website.Jet Propulsion Lab. 7 March 2016.Archived from the original on 8 March 2016. Retrieved8 March 2016.
  41. ^Ruesch, O.; Platz, T.; Schenk, P.; McFadden, L. A.; Castillo-Rogez, J. C.; Quick, L. C.; Byrne, S.; Preusker, F.; OBrien, D. P.; Schmedemann, N.; Williams, D. A.; Li, J.- Y.; Bland, M. T.; Hiesinger, H.; Kneissl, T.; Neesemann, A.; Schaefer, M.; Pasckert, J. H.; Schmidt, B. E.; Buczkowski, D. L.; Sykes, M. V.; Nathues, A.; Roatsch, T.; Hoffmann, M.; Raymond, C. A.; Russell, C. T. (2 September 2016)."Cryovolcanism on Ceres".Science.353 (6303) aaf4286.Bibcode:2016Sci...353.4286R.doi:10.1126/science.aaf4286.PMID 27701087.
  42. ^Perry, Jason (27 January 2009)."Boösaule Montes".Gish Bar Times blog.Archived from the original on 23 March 2016. Retrieved30 June 2012.
  43. ^Schenk, P.; Hargitai, H."Boösaule Montes".Io Mountain Database.Archived from the original on 4 March 2016. Retrieved30 June 2012.
  44. ^abSchenk, P.; Hargitai, H.; Wilson, R.; McEwen, A.; Thomas, P. (2001)."The mountains of Io: Global and geological perspectives from Voyager and Galileo".Journal of Geophysical Research.106 (E12): 33201.Bibcode:2001JGR...10633201S.doi:10.1029/2000JE001408.ISSN 0148-0227.
  45. ^Schenk, P.; Hargitai, H."Ionian Mons".Io Mountain Database.Archived from the original on 4 March 2016. Retrieved30 June 2012.
  46. ^Schenk, P.; Hargitai, H."Euboea Montes".Io Mountain Database.Archived from the original on 4 March 2016. Retrieved30 June 2012.
  47. ^abMartel, L. M. V. (16 February 2011)."Big Mountain, Big Landslide on Jupiter's Moon, Io".NASA Solar System Exploration web site. Archived fromthe original on 13 January 2011. Retrieved30 June 2012.
  48. ^Moore, J. M.; McEwen, A. S.; Albin, E. F.; Greeley, R. (1986). "Topographic evidence for shield volcanism on Io".Icarus.67 (1):181–183.Bibcode:1986Icar...67..181M.doi:10.1016/0019-1035(86)90183-1.ISSN 0019-1035.
  49. ^abSchenk, P.; Hargitai, H."Unnamed volcanic mountain".Io Mountain Database.Archived from the original on 4 March 2016. Retrieved6 December 2012.
  50. ^abSchenk, P. M.; Wilson, R. R.; Davies, R. G. (2004). "Shield volcano topography and the rheology of lava flows on Io".Icarus.169 (1):98–110.Bibcode:2004Icar..169...98S.doi:10.1016/j.icarus.2004.01.015.
  51. ^abMoore, Jeffrey M.; Schenk, Paul M.; Bruesch, Lindsey S.; Asphaug, Erik; McKinnon, William B. (October 2004)."Large impact features on middle-sized icy satellites"(PDF).Icarus.171 (2):421–443.Bibcode:2004Icar..171..421M.doi:10.1016/j.icarus.2004.05.009.Archived(PDF) from the original on 2 October 2018. Retrieved4 September 2015.
  52. ^Hammond, N. P.;Phillips, C. B.; Nimmo, F.; Kattenhorn, S. A. (March 2013). "Flexure on Dione: Investigating subsurface structure and thermal history".Icarus.223 (1):418–422.Bibcode:2013Icar..223..418H.doi:10.1016/j.icarus.2012.12.021.
  53. ^Beddingfield, C. B.; Emery, J. P.; Burr, D. M. (March 2013). "Testing for a Contractional Origin of Janiculum Dorsa on the Northern, Leading Hemisphere of Saturn's Moon Dione".44th Lunar and Planetary Science Conference, LPI Contribution No. 1719. Lunar and Planetary Science Conference. p. 1301.Bibcode:2013LPI....44.1301B.
  54. ^Overlooked Ocean Worlds Fill the Outer Solar SystemArchived 26 December 2018 at theWayback Machine. John Wenz,Scientific American. 4 October 2017.
  55. ^ab"PIA20023: Radar View of Titan's Tallest Mountains".Photojournal.jpl.nasa.gov.Jet Propulsion Laboratory. 24 March 2016.Archived from the original on 25 August 2017. Retrieved25 March 2016.
  56. ^Mitri, G.; Bland, M. T.; Showman, A. P.; Radebaugh, J.; Stiles, B.; Lopes, R. M. C.; Lunine, Jonathan I.; Pappalardo, R. T. (2010)."Mountains on Titan: Modeling and observations".Journal of Geophysical Research.115 (E10002): E10002.Bibcode:2010JGRE..11510002M.doi:10.1029/2010JE003592.Archived from the original on 26 January 2020. Retrieved5 July 2012.
  57. ^abcLopes, 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.Bibcode:2013JGRE..118..416L.doi:10.1002/jgre.20062.Archived(PDF) from the original on 1 September 2019. Retrieved1 September 2019.
  58. ^Giese, B.; Denk, T.; Neukum, G.; Roatsch, T.; Helfenstein, P.; Thomas, P. C.; Turtle, E. P.; McEwen, A.; Porco, C. C. (2008)."The topography of Iapetus' leading side"(PDF).Icarus.193 (2):359–371.Bibcode:2008Icar..193..359G.doi:10.1016/j.icarus.2007.06.005.ISSN 0019-1035.Archived from the original on 13 March 2020. Retrieved9 December 2012.
  59. ^Porco, C. C.; et al. (2005)."Cassini Imaging Science: Initial Results on Phoebe and Iapetus"(PDF).Science.307 (5713):1237–1242.Bibcode:2005Sci...307.1237P.doi:10.1126/science.1107981.ISSN 0036-8075.PMID 15731440.S2CID 20749556. 2005Sci...307.1237P.Archived(PDF) from the original on 19 July 2018. Retrieved13 January 2019.
  60. ^Kerr, Richard A. (6 January 2006)."How Saturn's Icy Moons Get a (Geologic) Life".Science.311 (5757): 29.doi:10.1126/science.311.5757.29.PMID 16400121.S2CID 28074320.
  61. ^Ip, W.-H. (2006)."On a ring origin of the equatorial ridge of Iapetus"(PDF).Geophysical Research Letters.33 (16): L16203.Bibcode:2006GeoRL..3316203I.doi:10.1029/2005GL025386.ISSN 0094-8276.Archived(PDF) from the original on 26 June 2019. Retrieved9 December 2012.
  62. ^Moore, P.; Henbest, N. (April 1986). "Uranus - the View from Voyager".Journal of the British Astronomical Association.96 (3):131–137.Bibcode:1986JBAA...96..131M.
  63. ^abcdeSchenk, 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. (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.
  64. ^abHand, E.; Kerr, R. (15 July 2015). "Pluto is alive—but where is the heat coming from?".Science.doi:10.1126/science.aac8860.
  65. ^Pokhrel, Rajan (19 July 2015)."Nepal's mountaineering fraternity happy over Pluto mountains named after Tenzing Norgay Sherpa - Nepal's First Landmark In The Solar System".The Himalayan Times.Archived from the original on 13 August 2015. Retrieved19 July 2015.
  66. ^abc"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 10 November 2015. Retrieved9 November 2015.
  67. ^abWitze, A. (9 November 2015)."Icy volcanoes may dot Pluto's surface".Nature.doi:10.1038/nature.2015.18756.S2CID 182698872.Archived from the original on 10 November 2015. Retrieved9 November 2015.
  68. ^"Ice Volcanoes and Topography".New Horizons Multimedia. The Johns Hopkins University Applied Physics Laboratory LLC. 9 November 2015. Archived fromthe original on 13 November 2015. Retrieved9 November 2015.
  69. ^"Ice Volcanoes on Pluto?".New Horizons Multimedia. The Johns Hopkins University Applied Physics Laboratory LLC. 9 November 2015. Archived fromthe original on 11 September 2017. Retrieved9 November 2015.
  70. ^abcdefSchenk, P. M.; Beyer, R. A.; McKinnon, W. B.; Moore, J. M.; Spencer, J. R.; White, O. L.; Singer, K.; Umurhan, O. M.; Nimmo, F.; Lauer, T. R.; Grundy, W. M.; Robbins, S.; Stern, S. A.; Weaver, H. A.; Young, L. A.; Smith, K. E.; Olkin, C. (2018). "Breaking up is hard to do: Global cartography and topography of Pluto's mid-sized icy Moon Charon from New Horizons".Icarus.315:124–145.Bibcode:2018Icar..315..124S.doi:10.1016/j.icarus.2018.06.010.S2CID 125833113.
  71. ^abcRommel, F. L.; Braga-Ribas, F.; Ortiz, J. L.; Sicardy, B.; Santos-Sanz, P.; Desmars, J.; et al. (October 2023)."A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations".Astronomy & Astrophysics.678: 25.arXiv:2308.08062.Bibcode:2023A&A...678A.167R.doi:10.1051/0004-6361/202346892.S2CID 260926329. A167.

External links

[edit]
Wikimedia Commons has media related toList of tallest mountains in the Solar System.
The Sun, the planets, their moons, and several trans-Neptunian objects
Minor
planets
Dwarf planets
Asteroids
(Small Solar
System bodies)
Notable asteroids
Groups and families
Naming
Trans-Neptunian
(Distant minor
planets)
Kuiper belt
Other
Comets
Lists
Hypothetical
Retrieved from "https://en.wikipedia.org/w/index.php?title=List_of_tallest_mountains_in_the_Solar_System&oldid=1322354556"
Categories:
Hidden categories:
[8]ページ先頭
©2009-2025 Movatter.jp