ผลต่างระหว่างรุ่นของ "ผู้ใช้:EZBELLA/กระบะทราย6"

!class=unsortable|หมายเหตุ

|-

| title = Surface

| work = MESSENGER web site

| accessdate = 4 April 2012}}</ref><ref name="OberstPreusker2010">{{cite journal|last1=Oberst|first1=J.|last2=Preusker|first2=F.|last3=Phillips|first3=R. J.|last4=Watters|first4=T. R.|last5=Head|first5=J. W.|last6=Zuber|first6=M. T.|last7=Solomon|first7=S. C.|title=The morphology of Mercury’s Caloris basin as seen in MESSENGER stereo topographic models|journal=Icarus |volume=209|issue=1 |date=2010|pages=230–238 |issn=0019-1035|doi=10.1016/j.icarus.2010.03.009|bibcode = 2010Icar..209..230O }}</ref>

| 0.12

| Formed by the [[Caloris Basin|Caloris impact]]

|-

| rowspan="2" | [[ดาวศุกร์]]

| {{convert|abbr=on|6.4|km|mi|1}} (approx.)<ref name = "planetology">{{cite book| title = Planetology : Unlocking the secrets of the solar system|author1=Jones, Tom |author2=Stofan, Ellen | date = 2008| publisher = National Geographic Society| location = Washington, D.C.| page = 74| isbn = 978-1-4262-0121-9| url = https://books.google.com/books?id=SL-BszT15s0C&pg=PA74}}</ref>

| 0.11

| Has radar-bright slopes due to metallic [[Venus snow]], possibly [[Galena|lead sulfide]]<ref name="wustl-lead-sulfide">{{cite news

|title= 'Heavy metal' snow on Venus is lead sulfide

}}</ref>

|-

| {{convert|abbr=on|4.9|km|mi|1}} (approx.)<ref name = "Maat">{{cite web

| title = PIA00106: Venus - 3D Perspective View of Maat Mons

| accessdate = 30 June 2012}}</ref>

| 0.081

| Highest volcano on Venus

|-

| rowspan="5" | [[โลก]]

| {{convert|abbr=on|10.2|km|mi|1}}<ref name = "Highest_Points">{{cite web |url=http://science.nationalgeographic.com/science/earth/surface-of-the-earth/mountains-article/ |title=Mountains: Highest Points on Earth |publisher=National Geographic Society |accessdate=19 September 2010}}</ref>

| 0.16

| Just {{convert|abbr=on|4.2|km|mi|1}} of this is above sea level

|-

| {{convert|abbr=on|9.1|km|mi|1}}<ref name = "NPS">{{cite web

| title = Haleakala National Park Geology Fieldnotes| last = | first =

| accessdate = 31 January 2017}}</ref>

| 0.14

| Rises 3.1&nbsp;km above sea level<ref name = "NPS" />

|-

| {{convert|abbr=on|7.5|km|mi|1}}<ref name = "UNESCO">{{cite web

| title = Teide National Park | work = UNESCO World Heritage Site list

| accessdate = 2 June 2013}}</ref>

| 0.12

| Rises 3.7&nbsp;km above sea level<ref name = "UNESCO"/>

|-

| {{convert|abbr=on|5.3|to|5.9|km|mi|1}}<ref>{{cite web|url=https://www.pbs.org/wgbh/nova/denali/expedition/mission.html|title=NOVA Online: Surviving Denali, The Mission|publisher=Public Broadcasting Corporation|work=NOVA web site|date=2000|accessdate=7 June 2007}}</ref>

| 0.093

| Tallest mountain base-to-peak on land<ref name="Helman2005">{{cite book|author=Adam Helman|title=The Finest Peaks: Prominence and Other Mountain Measures|url=https://books.google.com/books?id=kr8AM-w8IFQC&printsec=frontcover |accessdate=9 December 2012|date=2005|publisher=Trafford Publishing|isbn=978-1-4120-5995-4}}</ref>{{refn |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 {{convert|18000|feet|meter|abbr=on}}"| group = n }}

|-

| {{convert|abbr=on|3.6|to|4.6|km|mi|1}}<ref name="washburn_map">''Mount Everest'' (1:50,000 scale map), prepared under the direction of [[Bradford Washburn]] for the Boston Museum of Science, the Swiss Foundation for Alpine Research, and the [[National Geographic Society]], 1991, {{ISBN|3-85515-105-9}}</ref>

| 0.072

| 4.6&nbsp;km on north face, 3.6&nbsp;km on south face;{{refn |Peak is {{convert|abbr=on|8.8|km|mi|1}} above sea level, and over {{convert|abbr=on|13|km|mi|1}} above the oceanic [[abyssal plain]].| group = n }} listed only because it has the highest elevation (8.8&nbsp;km) above sea level

<!-- K2 is probably not #4 |-

| {{convert|abbr=on|5.5|km|mi|1}}<ref name="price"/><ref name="moore"/>

| 0.32

| Formed by the [[Mare Imbrium|Imbrium impact]]

|-

| {{convert|abbr=on|4.5|km|mi|1}}<ref name="price">{{cite book | author=Fred W. Price | title=The Moon observer's handbook | publisher=Cambridge University Press | location=London | date=1988 | isbn= 0-521-33500-0}}</ref><ref name="moore">{{cite book | last=Moore | first=Patrick | authorlink = Patrick Moore | title=On the Moon | publisher=Cassell & Co | location=London | date=2001 }}</ref>

| 0.26

| Formed by the [[Mare Imbrium|Imbrium impact]]

|-

| accessdate = 28 August 2007 }}</ref>

| 0.063

| Largest volcanic construct on the Moon<ref name="laps07"/>

|-

| {{convert|abbr=on|21.9|km|mi|0}}<ref name="Plescia2004">{{cite journal|last1=Plescia|first1=J. B.|title=Morphometric properties of Martian volcanoes|journal=Journal of Geophysical Research|volume=109|issue=E3|date=2004|issn=0148-0227|doi=10.1029/2002JE002031|bibcode = 2004JGRE..109.3003P }}</ref><ref name="Carr2007" />

| 0.65

| Rises 26&nbsp;km above northern plains,<ref name="Comins2012">{{cite book|last=Comins|first=Neil F.| title=Discovering the Essential Universe|url=https://books.google.com/books?id=qK_4mNve1DYC&pg=PA148&dq=mons+olympus+height&hl=en&sa=X&ei=YzCQT-GpIcH22AXz852ABQ&ved=0CDoQ6AEwAQ#v=onepage&q=mons%20olympus%20height&f=false|accessdate=23 December 2012|date=4 January 2012|publisher=Macmillan|isbn=978-1-4292-5519-6}}</ref> 1000&nbsp;km away. Summit calderas are 60 x 80&nbsp;km wide, up to 3.2&nbsp;km deep;<ref name="Carr2007">{{cite book|author=Carr, Michael H.|title=The Surface of Mars|url=https://books.google.com/books?id=uLHlJ6sjohwC|date=11 January 2007|publisher=Cambridge University Press|isbn=978-1-139-46124-5|page=51}}</ref> scarp around margin is up to 8&nbsp;km high.<ref name="Lopes1982">{{cite journal|last1=Lopes|first1=R.|last2=Guest|first2=J. E.|last3=Hiller|first3=K.|last4= Neukum|first4= G.|title=Further evidence for a mass movement origin of the Olympus Mons aureole|journal=Journal of Geophysical Research|volume=87|issue= B12|date=January 1982|pages= 9917–9928|doi= 10.1029/JB087iB12p09917|bibcode=1982JGR....87.9917L}}</ref>

|-

|{{convert|abbr=on|14.9|km|mi|1}}<ref name="Plescia2004"/>

| 0.44

| Tallest of the three [[Tharsis Montes]]

|-

|{{convert|abbr=on|12.6|km|mi|1}}<ref name="Plescia2004"/>

| 0.37

| Highest volcano in [[Elysium (volcanic province)|Elysium]]

|-

| {{convert|abbr=on|11.7|km|mi|1}}<ref name="Plescia2004"/>

| 0.35

| Summit [[caldera]] is {{convert|abbr=on|108|to|138|km|mi|0}} across<ref name="Plescia2004"/>

|-

| {{convert|abbr=on|8.4|km|mi|1}}<ref name="Plescia2004"/>

| 0.25

| Summit caldera is {{convert|abbr=on|4.8|km|mi|1}} deep<ref name="Plescia2004"/>

|-

| {{convert|abbr=on|6.2|km|mi|1}}<ref name = "MOLA">JMARS MOLA elevation dataset. Christensen, P.; Gorelick, N.; Anwar, S.; Dickenshied, S.; Edwards, C.; Engle, E. (2007) "[http://adsabs.harvard.edu/abs/2007AGUFM.P11E..01C New Insights About Mars From the Creation and Analysis of Mars Global Datasets];" American Geophysical Union, Fall Meeting, abstract #P11E-01.</ref>

| 0.18

| Among the highest nonvolcanic peaks on Mars, formed by the [[Hellas Planitia|Hellas impact]]

|-

|doi=10.1555/mars.2010.0004}}</ref> | group = n }}

| 0.16

| last = Wall | first = M.

| title = Bizarre Mars Mountain Possibly Built by Wind, Not Water

| accessdate = }}</ref>

| 8.4

| Almost {{convert|200|km|mi|abbr=on}} wide. See also: [[List of largest craters in the Solar System]]

|-

| url = http://dawn.jpl.nasa.gov/news/news-detail.html?id=5745 | accessdate = 2016-03-08}}</ref>

| 0.85

| Isolated steep-sided dome in relatively smooth area; max. height of ~ 5&nbsp;km on steepest side; roughly [[Antipodes|antipodal]] to [[Kerwan (crater)|largest impact basin on Ceres]]

|-

| accessdate = 30 June 2012}}</ref>

| 1.0

| Has a {{convert|abbr=on|15|km|mi|0}} high scarp on its SE margin<ref name="SchenkHargitai2001">{{cite journal|last1=Schenk|first1=P.|last2=Hargitai|first2=H.|last3=Wilson|first3=R.|last4=McEwen|first4=A.|last5=Thomas|first5=P.|title=The mountains of Io: Global and geological perspectives from Voyager and Galileo|journal= Journal of Geophysical Research|volume= 106|issue= E12|date= 2001|pages= 33201|issn=0148-0227|doi=10.1029/2000JE001408|bibcode = 2001JGR...10633201S }}</ref>

|-

| accessdate = 30 June 2012}}</ref>

| 0.70

| Has the form of a curved double ridge

|-

| accessdate = 30 June 2012}}</ref>

| 0.74

| A NW flank landslide left a 25,000&nbsp;km³ debris apron<ref name = "Martel">{{cite web

| last = Martel | first = L. M. V. | title = Big Mountain, Big Landslide on Jupiter's Moon, Io

| accessdate = 6 December 2012}}</ref>

| 0.14

| One of the tallest of Io's many volcanoes, with an atypical conical form<ref name = "unnamed_Io"/>{{refn |Some of [[List of paterae on Io|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.<ref name="Schenk2004">{{cite journal | last=Schenk |first=P. M. |author2=Wilson, R. R. |author3=Davies, R. G. |title=Shield volcano topography and the rheology of lava flows on Io |journal=Icarus |volume=169 |issue= 1|pages=98–110 |date=2004 |url= |doi=10.1016/j.icarus.2004.01.015 |bibcode=2004Icar..169...98S}}</ref> 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.<ref name="Schenk2004"/> | group = n }}

|-

}}</ref>

| 3.5

| See also: [[List of largest craters in the Solar System]]

|-

| {{convert|abbr=on|1.5|km|mi|1}}<ref name = "Hammond2013">{{Cite journal | doi = 10.1016/j.icarus.2012.12.021| title = Flexure on Dione: Investigating subsurface structure and thermal history| journal = [[Icarus (journal)|Icarus]]| volume = 223| issue = 1| pages = 418–422| date = March 2013| last1 = Hammond | first1 = N. P. | last2 = Phillips | first2 = C. B. | last3 = Nimmo | first3 = F.| last4 = Kattenhorn | first4 = S. A. | bibcode = 2013Icar..223..418H}}</ref>

| 0.27

| first1 = C. B. | last1 = Beddingfield | first2 = J. P. | last2 = Emery | first3 = D. M. | last3 = Burr

| title = Testing for a Contractional Origin of Janiculum Dorsa on the Northern, Leading Hemisphere of Saturn's Moon Dione

| ≤ {{convert|abbr=on|3.3|km|mi|1}}<ref name = "PIA20023">{{cite web | url = http://photojournal.jpl.nasa.gov/catalog/PIA20023 | title = PIA20023: Radar View of Titan's Tallest Mountains | date = 2016-03-24 | website = Photojournal.jpl.nasa.gov | publisher = [[Jet Propulsion Laboratory]] | access-date = 2016-03-25}}</ref>

| 0.13

| May have formed due to global contraction<ref name = "Mitri">{{cite journal

| last = Mitri | first = G. | authorlink =

| doi = 10.1002/jgre.20062 | accessdate = 2013-04-10|bibcode = 2013JGRE..118..416L }}</ref>

| 0.056

| Adjacent to [[Sotra Patera]], a {{convert|abbr=on|1.7|km|mi|1}} deep collapse feature<ref name = "Lopes_2013"/>

|-

| {{convert|abbr=on|20|km|mi|0}} (approx.)<ref name="GieseDenk2008">{{cite journal|last=Giese|first=B.|author2=Denk, T. |author3=Neukum, G. |author4=Roatsch, T. |author5=Helfenstein, P. |author6=Thomas, P. C. |author7=Turtle, E. P. |author8=McEwen, A. |author9= Porco, C. C. |title=The topography of Iapetus' leading side|journal=Icarus|volume=193|issue=2|date=2008|pages=359–371|issn=0019-1035|url= http://www.geoinf.fu-berlin.de/publications/denk/2008/GieseEtAl_IapetusTopography_Icarus_2008.pdf |doi=10.1016/j.icarus.2007.06.005|bibcode = 2008Icar..193..359G }}</ref>

| 2.7

|display-authors=etal

|title=Cassini Imaging Science: Initial Results on Phoebe and Iapetus

| {{convert|abbr=on|11|km|mi|0}} (approx.)<ref name="Moore Schenk et al. 2004"/>

| 1.4

| A value of 6&nbsp;km was given shortly after the ''[[Voyager 2]]'' encounter<ref name = "PMoore">{{cite journal

| last = Moore | first = P. | authorlink = Patrick Moore |author2=Henbest, N.

| ~{{convert|abbr=on|5.6|km|mi|1}}<ref name = "cryovolcano_topo"/>

| 0.47

| ~220&nbsp;km across<ref name = "cryovolcano_topo">{{cite web

| url = http://pluto.jhuapl.edu/Multimedia/Science-Photos/image.php?page=&gallery_id=2&image_id=375

| ~{{convert|abbr=on|4.0|km|mi|1}}<ref name = "News2015-11-09"/>

| 0.34

| ~160&nbsp;km across;<ref name = "News2015-11-09"/> summit depression ~56&nbsp;km across<ref name = "Ice_Volcanoes2015-11-09">{{cite web

| url = http://pluto.jhuapl.edu/Multimedia/Science-Photos/image.php?page=&gallery_id=2&image_id=374

| ≤ {{convert|abbr=on|3.5|km|mi|1}}<ref name="HandE_2015a">{{cite journal|last1=Hand|first1=E. | last2 = Kerr | first2 = R. |title=Pluto is alive—but where is the heat coming from?|journal=Science|date=15 July 2015|doi=10.1126/science.aac8860}}</ref>

| 0.30

| Composed of water ice;<ref name = "HandE_2015a"/> named after [[Tenzing Norgay]]<ref name="THT-20150719">{{cite web |last=Pokhrel |first=Rajan |title=Nepal’s mountaineering fraternity happy over Pluto mountains named after Tenzing Norgay Sherpa - Nepal's First Landmark In The Solar System |url=http://thehimalayantimes.com/latest/plutos-mountains-named-after-tenzing-norgay-sherpa |date=19 July 2015 |work=The Himalayan Times |accessdate= 19 July 2015}}</ref>

|-

| {{sort|045| ≥ {{convert|abbr=on|4.5|km|mi|1}}<ref name="Beyer2018" />}}

| {{sort|0743|0.74}}

| [[Vulcan Planitia]], the southern plains, has several isolated peaks, possibly tilted crustal blocks<ref name="Beyer2018" />

|-

| {{sort|040| ~{{convert|abbr=on|4.0|km|mi|1}}<ref name="Beyer2018" />}}

| {{sort|0660|0.66}}

| North polar impact basin Dorothy, Charon's largest, is ∼240 km across and 6 km deep<ref name="Beyer2018" />

|}

 

==Gallery==