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南極高原 (火星)：修订间差异

坐标：83°S 160°E / 83°S 160°E / -83; 160
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{{Otheruses|subject=火星的南極高原|other=地球南極的高原|南極高原}}
{{Translating |time=2010-12-07}}

{{MarsGeo-Plains
{{MarsGeo-Plains
|name=南極高原<br>Planum Australe
|name=南極高原<br>Planum Australe
|image=[[Image:CasquetePolarSur.jpg|200px]]
|image=[[Image:Martian south pole during summer by HRSC.jpg|265px]]
|caption=[[火星全球探勘者號]]拍攝的南極高原
|caption=[[火星快車號]]於2015年2月拍攝的火星南極，環繞白色[[火星極冠|極冠]]的區域皆為南極高原
|location=
|location=[[南海區 (火星)|南海區]]
|diameter=1,450 公里
|latitude=83.9
|latitude=83
|N_or_S=S
|N_or_S=S
|longitude=160.0
|longitude=160
|E_or_W=E
|E_or_W=E
|area=
|area=
第14行： 第14行：
|naming=
|naming=
}}
}}
'''南極高原'''([[拉丁語]]：'''Planum Australe'''，南方的平原；'''Planum''' 是指高海拔的平原或高原)是火星[[南極]]的一個高原。延伸範圍的北方界線大約 75°S，中心位置在 {{Coord|-83.9|160.0|globe:Mars}}。[[NASA]]原定以[[火星極地著陸者號]]研究當地地質，但在降落過程中在[[火星大氣層]]內失去聯絡，任務失敗。
'''南極高原'''（{{lang-la|''Planum Australe''}}，南方的平原；Planum 是指高海拔的平原或高原）是火星[[南極]]的一個高原。延伸範圍的北方界線大約 75°S，中心位置在 {{Coord|-83.9|160.0|globe:Mars}}。[[NASA]]原定以[[火星極地著陸者號]]研究當地地質，但在降落過程中在[[火星大氣層]]內失去聯絡，任務失敗。


==冰帽==
==冰帽==
南極高原部份區域被由水冰和乾冰組成的永久冰帽覆蓋，厚度約 3 公里。 A seasonal ice cap forms on top of the permanent one during the Martian winter, extending from 60°S southwards. It is, at the height of winter, approximately 1 metre thick.<ref>{{cite web|title=Mars is Melting| accessdate=2006-10-20| url=http://science.nasa.gov/headlines/y2003/07aug_southpole.htm| first=Tony| last=Phillips| publisher=Science @ NASA}}</ref> It is possible that the area of this ice cap may be shrinking due to localized [[climate change]] or more widespread [[Martian global warming|global warming]].<ref>{{cite web| url=http://www.realclimate.org/index.php?p=192| accessdate=2006-10-20| title=Global warming on Mars?| first= Steinn| last=Sigurdsson| publisher=RealClimate.org}}</ref>
南極高原部份區域被由水冰和乾冰組成的永久冰帽覆蓋，厚度約 3 公里。火星南半球冬季時季節性冰帽會覆蓋在永久冰帽上，最北界線可到達 60°S，厚度約 1 公尺<ref>{{cite web |title=Mars is Melting |accessdate=2006-10-20 |url=http://science.nasa.gov/headlines/y2003/07aug_southpole.htm |first=Tony |last=Phillips |publisher=Science @ NASA |deadurl=yes |archiveurl=https://web.archive.org/web/20070224153145/http://science.nasa.gov/headlines/y2003/07aug_southpole.htm |archivedate=2007-02-24 }}</ref>。冰帽面積的縮小可能是因為地區性的[[氣候變化]]或大範圍的[[火星氣候|全球暖化]]造成<ref>{{cite web| url=http://www.realclimate.org/index.php?p=192| accessdate=2006-10-20| title=Global warming on Mars?| first=Steinn| last=Sigurdsson| publisher=RealClimate.org| archive-date=2007-03-06| archive-url=https://web.archive.org/web/20070306113836/http://www.realclimate.org/index.php?p=192| dead-url=no}}</ref>。
[[Image:TopologicoPoloSurMarte.png|left|thumb|200px|Elevation map of the south pole. Note how Planum Australe rises above the surrounding cratered terrain. Click to enlarge and for more info.]]
[[Image:TopologicoPoloSurMarte.png|left|thumb|200px|火星南極的地形圖。注意南極高原的高程比周圍隕擊高原要高。點選可看大圖。]]
1966年 Leighton 和 Murray 提出火星極區冰帽儲存的二氧化碳含量遠比[[火星大氣層]]中的二氧化碳量多。但現在一般認為火星兩極大部分是水冰。火星兩極都有季節性的薄層固態二氧化碳；而在南極有一個永久性的殘餘二氧化碳冰帽覆蓋在水冰形成的冰帽上，厚度約 8 到 10 公尺。也許關鍵論點是大塊的冰層其實是水冰，因為乾冰的機械強度並不足以使一個厚度 3 公里的冰帽處於長期穩定狀態<ref>
In 1966, Leighton and Murray proposed that the Martian polar caps provided a store of CO<sub>2</sub> much larger than the atmospheric reservoir. However it is now thought that both poles are made mostly of water ice. Both poles have a thin seasonal covering of CO<sub>2</sub>, while in addition the southern pole has a permanent residual CO<sub>2</sub> cap, about 8 to 10 metres thick, that lies on top of the water ice. Perhaps the key argument that the bulk of the ice is water is that CO<sub>2</sub> ice isn't mechanically strong enough to make a 3&nbsp;km thick ice cap stable over long periods of time.<ref>
{{Cite journal
{{Cite journal
| last = Byrne
| last = Byrne
| first = Shane
| first = Shane
| title = A Sublimation Model for Martian South Polar Ice Features
| title = A Sublimation Model for Martian South Polar Ice Features
| url = https://archive.org/details/sim_science_2003-02-14_299_5609/page/1051
| journal = Science
| journal = Science
| volume = 299
| volume = 299
第32行： 第33行：
| last2 = Ingersoll
| last2 = Ingersoll
| first2 = AP
| first2 = AP
| issue = 5609 }}</ref>.
| issue = 5609 }}</ref>。


Data from [[European Space Agency|ESA]]'s [[Mars Express]] indicates that there are three main parts to the ice cap. The most reflective part of the ice cap is approximately 85% [[dry ice]] and 15% water ice. The second part, where the ice cap forms steep slopes at the boundary with the surrounding plain, is almost exclusively water ice. Finally, the ice cap is surrounded by [[permafrost]] fields that extend for tens of [[kilometre]]s north away from the scarps.<ref>{{cite web|url=http://www.esa.int/SPECIALS/Mars_Express/SEMYKEX5WRD_0.html|title=Water at Martian south pole|accessdate=2006-10-22|publisher=[[European Space Agency]]}}</ref>
[[歐洲太空總署]]的[[火星快車號]]探測資料顯示南極高原冰帽可分為三個主要的部份。反照率最高的部份冰帽組成成分約 85% 是[[乾冰]]，15% 是水冰。第二部份則是冰帽與周圍平原交界的邊緣陡坡，幾乎全由水冰組成。最後一部分是環繞冰帽的[[永久凍土]]區，從邊緣的陡坡向北方延伸數十公里<ref>{{cite web|url=http://www.esa.int/SPECIALS/Mars_Express/SEMYKEX5WRD_0.html|title=Water at Martian south pole|accessdate=2006-10-22|publisher=[[European Space Agency]]|archive-date=2004-04-01|archive-url=https://web.archive.org/web/20040401181115/http://www.esa.int/SPECIALS/Mars_Express/SEMYKEX5WRD_0.html|dead-url=no}}</ref>。


永久冰帽的中心並非位於 90°S，而是位於地理南極點北方約 150 公里處。火星西半球的兩個巨大[[撞擊坑]]-[[希臘平原]]和[[阿爾及爾平原]]使火星南極的永久冰帽區產生了永久的[[低氣壓]]。因此造成的氣候模式產生反照率較高的蓬鬆白雪。這是相對於火星南極東半部因為只有少量雪產生的[[黑冰]]（Black ice）<ref>{{cite web|url=http://spaceflightnow.com/news/n0505/14marsmystery/|title=Mars' South Pole mystery|accessdate=2006-10-26|publisher=Spaceflight Now|archive-date=2021-01-25|archive-url=https://web.archive.org/web/20210125025012/https://spaceflightnow.com/news/n0505/14marsmystery/|dead-url=no}}</ref>。
The centre of the permanent ice cap is not located at 90°S but rather approximately 150 kilometres north of the geographical south pole. The presence of two massive [[impact crater|impact basins]] in the western hemisphere - [[Hellas Planitia]] and [[Argyre Planitia]] - creates an immobile [[low pressure area|area of low pressure]] over the permanent ice cap. The resulting weather patterns produce fluffy white [[snow]] which has a high [[albedo]]. This is in contrast to the [[black ice]] that forms in the eastern part of the polar region, which receives little snow.<ref>{{cite web|url=http://spaceflightnow.com/news/n0505/14marsmystery/|title=Mars' South Pole mystery|accessdate=2006-10-26|publisher=Spaceflight Now}}</ref>


==地表特徵==
==地表特徵==
南極高原可分為兩個區域 - 南极舌状地(Australe Lingula)和普罗米修斯舌状地(Promethei Lingula)，這兩個區域由以下數個峽谷分隔：[[普罗米修斯深谷]]、[[乌尔蒂马峡谷]]、[[南極峽谷]]和[[南極槽溝]]。理論上認為這些峽谷是因為[[下降風]]（katabatic wind）造成<ref>
⚫
{{cite journal | first=Eric J. |last = Kolb| coauthors = Kenneth L. Tanaka|title = Accumulation and erosion of south polar layered deposits in the Promethei Lingula region, Planum Australe, Mars|journal = The Mars Journal|volume = 2|pages = 1–9|year = 2006|publisher =Mars Informatics Inc.|doi=10.1555/mars.2006.0001}}</ref>。南極高原內最大的撞擊坑是[[麥克默多撞擊坑]]。


⚫
===火星噴泉===
There are two distinct subregions in Planum Australe - [[Australe Lingula]] and [[Promethei Lingula]]. It is dissected by canyons [[Promethei Chasma]], [[Ultimum Chasma]], [[Chasma Australe]] and [[Australe Sulci]]. It is theorised that these canyons were created by [[katabatic wind]].<ref>
[[File:Geysers on Mars.jpg|thumb|left|150px|藝術家筆下的火星噴泉噴發出含沙的噴流 (NASA出版；[[榮恩米勒 (藝術家和作家)|榮恩·米勒]]繪。]][[Image:Mars Global Surveyor 1.jpg|thumb|150px|由類似噴泉系統產生的「暗色砂丘斑點」（dark dune spots）近距影像。]]
⚫
{{cite journal | first=Eric J. |last = Kolb| coauthors = Kenneth L. Tanaka|title = Accumulation and erosion of south polar layered deposits in the Promethei Lingula region, Planum Australe, Mars|journal = The Mars Journal|volume = 2|pages = 1–9|year = 2006|publisher =Mars Informatics Inc.|doi=10.1555/mars.2006.0001}}</ref> The largest crater in Planum Australe is [[McMurdo Crater]].
⚫
{{Main|火星噴泉}}

⚫
火星南極冰帽的季節性結霜和溶霜產生了類似蜘蛛的放射狀渠道，而這些渠道因為太陽光照射造成其深度約 1 公尺。接著，昇華的乾冰（也可能是水冰）增加了內部壓力，噴出冰冷流體和由[[玄武岩]][[風化]]後形成的暗色的泥沙混和的物質，相當類似噴泉<ref name=2006-100 >{{cite news | first= | last= | coauthors= | authorlink= | title=NASA Findings Suggest Jets Bursting From Martian Ice Cap | date=August 16, 2006 | publisher=NASA | url=http://www.jpl.nasa.gov/news/news.cfm?release=2006-100 | work=Jet Propulsion Laboratory | pages= | accessdate=2009-08-11 | language= | archive-date=2009-10-10 | archive-url=https://web.archive.org/web/20091010164741/http://www.jpl.nasa.gov/news/news.cfm?release=2006-100 | dead-url=no }}</ref><ref name=Kieffer2000 >{{Cite journal| first=H. H.| last=Kieffer| coauthors=| contribution=ANNUAL PUNCTUATED CO2 SLAB-ICE AND JETS ON MARS.| title=Mars Polar Science 2000| editor-first=| editor-last=| coeditors=| publisher=| place=| pages=| date=| year=2000| id=| contribution-url=http://www.lpi.usra.edu/meetings/polar2000/pdf/4095.pdf| format=PDF| accessdate=2009-09-06| postscript=<!--None-->| journal=| archive-date=2011-08-21| archive-url=https://www.webcitation.org/616WmxuWK?url=http://www.lpi.usra.edu/meetings/polar2000/pdf/4095.pdf| dead-url=no}}</ref><ref name=Portyankina >{{Cite journal| first=| last=| coauthors=| contribution=SIMULATIONS OF GEYSER-TYPE ERUPTIONS IN CRYPTIC REGION OF MARTIAN SOUTH| title=Fourth Mars Polar Science Conference| editor-first=G. Portyankina| editor-last=| coeditors=| publisher=| place=| pages=| date=| year=2006| id=| contribution-url=http://www.lpi.usra.edu/meetings/polar2006/pdf/8040.pdf| format=PDF| accessdate=2009-08-11| postscript=<!--None-->| journal=| archive-date=2012-02-17| archive-url=https://web.archive.org/web/20120217023905/http://www.lpi.usra.edu/meetings/polar2006/pdf/8040.pdf| dead-url=no}}</ref><ref name=Hugh2006 >{{cite journal|title=CO2 jets formed by sublimation beneath translucent slab ice in Mars' seasonal south polar ice cap|journal=Nature|date=30 May 2006|first=Hugh H.|last=Kieffer|coauthors=Philip R. Christensen and Timothy N. Titus|volume=442|issue=7104|pages=793–796|doi=10.1038/nature04945|url=http://www.nature.com/nature/journal/v442/n7104/abs/nature04945.html|accessdate=2009-09-02|pmid=16915284|archive-date=2016-03-05|archive-url=https://web.archive.org/web/20160305161549/http://www.nature.com/nature/journal/v442/n7104/abs/nature04945.html|dead-url=no}}</ref>。這樣的過程相當快速，並且觀察到在該區域的地質可能在幾天、幾星期或幾個月內變化，其變化速度不尋常地快，尤其是對火星而言。目前尚無派遣探測器登陸探測「暗色沙丘斑點」（dark dune spots）或「火星蜘蛛」（spider）區域的計畫。
⚫
===火星的噴泉===
[[File:Geysers on Mars.jpg|thumb|left|150px|Artist concept showing sand-laden jets erupt from geysers on Mars. (published by NASA; artist: [[Ron Miller (artist and author)|Ron Miller]].]][[Image:Mars Global Surveyor 1.jpg|thumb|150px|Close up of "dark dune spots" created by geyser-like systems.]]
⚫
{{Main|火星的噴泉}}
⚫
The seasonal frosting and defrosting of the southern ice cap results in the formation of spider-like radial channels carved on 1 meter thick ice by sunlight. Then, sublimed CO<sub>2</sub> -and probably water- increase pressure in their interior producing geyser-like eruptions of cold fluids often mixed with dark basaltic sand or mud.<ref name=2006-100 >{{cite news | first= | last= | coauthors= |authorlink= | title=NASA Findings Suggest Jets Bursting From Martian Ice Cap | date=August 16, 2006 | publisher=NASA | url =http://www.jpl.nasa.gov/news/news.cfm?release=2006-100 | work =Jet Propulsion Laboratory | pages = | accessdate = 2009-08-11 | language = }}</ref><ref name=Kieffer2000 >{{Cite journal| first=H. H. | last=Kieffer| coauthors=| contribution=ANNUAL PUNCTUATED CO2 SLAB-ICE AND JETS ON MARS.| title=Mars Polar Science 2000| editor-first=| editor-last=| coeditors=| publisher=| place=| pages=| date=| year=2000| id= | contribution-url=http://www.lpi.usra.edu/meetings/polar2000/pdf/4095.pdf| format=PDF| accessdate=2009-09-06| postscript=<!--None--> }}</ref><ref name=Portyankina >{{Cite journal| first= | last=| coauthors=| contribution=SIMULATIONS OF GEYSER-TYPE ERUPTIONS IN CRYPTIC REGION OF MARTIAN SOUTH| title=Fourth Mars Polar Science Conference| editor-first=G. Portyankina| editor-last=| coeditors=| publisher=| place=| pages=| date=| year=2006| id= | contribution-url=http://www.lpi.usra.edu/meetings/polar2006/pdf/8040.pdf| format=PDF| accessdate=2009-08-11| postscript= <!--None--> }}</ref><ref name=Hugh2006 >{{cite journal|title=CO2 jets formed by sublimation beneath translucent slab ice in Mars' seasonal south polar ice cap|journal=Nature|date=30 May 2006|first=Hugh H.|last=Kieffer|coauthors=Philip R. Christensen and Timothy N. Titus|volume=442|issue=7104|pages=793–796 |doi= 10.1038/nature04945|url=http://www.nature.com/nature/journal/v442/n7104/abs/nature04945.html|accessdate=2009-09-02|pmid=16915284 }}</ref> This process is rapid, observed happening in the space of a few days, weeks or months, a growth rate rather unusual in geology - especially for Mars. No [[Lander (spacecraft)|lander]] is presently planned to visit the '''dark dune spots''' and '''spider''' areas.


==參見==
==參見==
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* [[火星平原列表]]
* [[火星平原列表]]
* [[火星氣候]]
* [[火星氣候]]
* [[火星水文]]
* [[火星極冠]]


==參考資料==
==參考資料==
第58行： 第60行：


==外部連結==
==外部連結==
* [http://marsjournal.org/contents/2006/0001/ Accumulation and erosion of south polar layered deposits in the Promethei Lingula region, Planum Australe, Mars ]
* [http://marsjournal.org/contents/2006/0001/ Accumulation and erosion of south polar layered deposits in the Promethei Lingula region, Planum Australe, Mars ] {{Wayback|url=http://marsjournal.org/contents/2006/0001/ |date=20181102043321 }}
* [http://www.google.com/mars/#lat=-82.896986&lon=166.113281&q=planum%20australe Planum Australe on Google Mars].
* [http://www.google.com/mars/#lat=-82.896986&lon=166.113281&q=planum%20australe Planum Australe on Google Mars]{{Wayback|url=http://www.google.com/mars/#lat=-82.896986&lon=166.113281&q=planum%20australe |date=20110222180608 }}.
* [http://www.lpi.usra.edu/meetings/polar2000/pdf/4101.pdf Stratigraphy and Topography of McMurdo Crater area, Planum Australe, Mars]
* [http://www.lpi.usra.edu/meetings/polar2000/pdf/4101.pdf Stratigraphy and Topography of McMurdo Crater area, Planum Australe, Mars] {{Wayback|url=http://www.lpi.usra.edu/meetings/polar2000/pdf/4101.pdf |date=20160611110536 }}
* [http://www.lpi.usra.edu/resources/msp/msp.html Topographic maps of the Martian South Pole]
* [http://www.lpi.usra.edu/resources/msp/msp.html Topographic maps of the Martian South Pole] {{Wayback|url=http://www.lpi.usra.edu/resources/msp/msp.html |date=20210213220304 }}
* [http://geopubs.wr.usgs.gov/i-map/i2595/ USGS map of Planum Australe]
* [http://geopubs.wr.usgs.gov/i-map/i2595/ USGS map of Planum Australe] {{Wayback|url=http://geopubs.wr.usgs.gov/i-map/i2595/ |date=20130222044405 }}


{{火星}}
{{火星}}


{{Authority control}}
[[Category:火星平原|A]]
[[Category:火星平原|A]]

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2023年10月18日 (三) 06:15的最新版本

此条目的主題是火星的南極高原。关于地球南極的高原，請見「南極高原」。
南極高原
Planum Australe
火星快車號於2015年2月拍攝的火星南極，環繞白色極冠的區域皆為南極高原
位置南海區
经纬83°S 160°E / 83°S 160°E / -83; 160
直徑1,450 公里

南極高原（拉丁語：Planum Australe，南方的平原；Planum 是指高海拔的平原或高原）是火星南極的一個高原。延伸範圍的北方界線大約 75°S，中心位置在 83°54′S 160°00′E / 83.9°S 160.0°E / -83.9; 160.0。NASA原定以火星極地著陸者號研究當地地質，但在降落過程中在火星大氣層內失去聯絡，任務失敗。

冰帽

[编辑]

南極高原部份區域被由水冰和乾冰組成的永久冰帽覆蓋，厚度約 3 公里。火星南半球冬季時季節性冰帽會覆蓋在永久冰帽上，最北界線可到達 60°S，厚度約 1 公尺[1]。冰帽面積的縮小可能是因為地區性的氣候變化或大範圍的全球暖化造成[2]。

火星南極的地形圖。注意南極高原的高程比周圍隕擊高原要高。點選可看大圖。

1966年 Leighton 和 Murray 提出火星極區冰帽儲存的二氧化碳含量遠比火星大氣層中的二氧化碳量多。但現在一般認為火星兩極大部分是水冰。火星兩極都有季節性的薄層固態二氧化碳；而在南極有一個永久性的殘餘二氧化碳冰帽覆蓋在水冰形成的冰帽上，厚度約 8 到 10 公尺。也許關鍵論點是大塊的冰層其實是水冰，因為乾冰的機械強度並不足以使一個厚度 3 公里的冰帽處於長期穩定狀態[3]。

歐洲太空總署的火星快車號探測資料顯示南極高原冰帽可分為三個主要的部份。反照率最高的部份冰帽組成成分約 85% 是乾冰，15% 是水冰。第二部份則是冰帽與周圍平原交界的邊緣陡坡，幾乎全由水冰組成。最後一部分是環繞冰帽的永久凍土區，從邊緣的陡坡向北方延伸數十公里[4]。

永久冰帽的中心並非位於 90°S，而是位於地理南極點北方約 150 公里處。火星西半球的兩個巨大撞擊坑-希臘平原和阿爾及爾平原使火星南極的永久冰帽區產生了永久的低氣壓。因此造成的氣候模式產生反照率較高的蓬鬆白雪。這是相對於火星南極東半部因為只有少量雪產生的黑冰（Black ice）[5]。

地表特徵

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南極高原可分為兩個區域 - 南极舌状地(Australe Lingula)和普罗米修斯舌状地(Promethei Lingula)，這兩個區域由以下數個峽谷分隔：普罗米修斯深谷、乌尔蒂马峡谷、南極峽谷和南極槽溝。理論上認為這些峽谷是因為下降風（katabatic wind）造成[6]。南極高原內最大的撞擊坑是麥克默多撞擊坑。

火星噴泉

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藝術家筆下的火星噴泉噴發出含沙的噴流 (NASA出版；榮恩·米勒繪。
由類似噴泉系統產生的「暗色砂丘斑點」（dark dune spots）近距影像。
主条目：火星噴泉

火星南極冰帽的季節性結霜和溶霜產生了類似蜘蛛的放射狀渠道，而這些渠道因為太陽光照射造成其深度約 1 公尺。接著，昇華的乾冰（也可能是水冰）增加了內部壓力，噴出冰冷流體和由玄武岩風化後形成的暗色的泥沙混和的物質，相當類似噴泉[7][8][9][10]。這樣的過程相當快速，並且觀察到在該區域的地質可能在幾天、幾星期或幾個月內變化，其變化速度不尋常地快，尤其是對火星而言。目前尚無派遣探測器登陸探測「暗色沙丘斑點」（dark dune spots）或「火星蜘蛛」（spider）區域的計畫。

參見

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维基新闻中的相关報導：Massive ice deposits found on Mars

參考資料

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  1. ^ Phillips, Tony. Mars is Melting. Science @ NASA. [2006-10-20]. （原始内容存档于2007-02-24）. 
  2. ^ Sigurdsson, Steinn. Global warming on Mars?. RealClimate.org. [2006-10-20]. （原始内容存档于2007-03-06）. 
  3. ^ Byrne, Shane; Ingersoll, AP. A Sublimation Model for Martian South Polar Ice Features. Science. 14 February 2003, 299 (5609): 1051–1053. PMID 12586939. doi:10.1126/science.1080148. 
  4. ^ Water at Martian south pole. European Space Agency. [2006-10-22]. （原始内容存档于2004-04-01）. 
  5. ^ Mars' South Pole mystery. Spaceflight Now. [2006-10-26]. （原始内容存档于2021-01-25）. 
  6. ^ Kolb, Eric J.; Kenneth L. Tanaka. Accumulation and erosion of south polar layered deposits in the Promethei Lingula region, Planum Australe, Mars. The Mars Journal (Mars Informatics Inc.). 2006, 2: 1–9. doi:10.1555/mars.2006.0001. 
  7. ^ NASA Findings Suggest Jets Bursting From Martian Ice Cap. Jet Propulsion Laboratory (NASA). August 16, 2006 [2009-08-11]. （原始内容存档于2009-10-10）. 
  8. ^ Kieffer, H. H. Mars Polar Science 2000 (PDF). 2000. （原始内容存档 (PDF)于2011-08-21） 使用|archiveurl=需要含有|url= (帮助).  |contribution=被忽略 (帮助);
  9. ^ Fourth Mars Polar Science Conference (PDF). 2006. （原始内容存档 (PDF)于2012-02-17） 使用|archiveurl=需要含有|url= (帮助).  |contribution=被忽略 (帮助); Editors list列表中的|first1=缺少|last1= (帮助);
  10. ^ Kieffer, Hugh H.; Philip R. Christensen and Timothy N. Titus. CO2 jets formed by sublimation beneath translucent slab ice in Mars' seasonal south polar ice cap. Nature. 30 May 2006, 442 (7104): 793–796 [2009-09-02]. PMID 16915284. doi:10.1038/nature04945. （原始内容存档于2016-03-05）. 

外部連結

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检索自“https://zh.wikipedia.org/zhwiki/w/index.php?title=南極高原_(火星)&oldid=79410977”