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{{Update|inaccurate=y|date=September 2018|updated=January 2007|data from the [[Clementine (spacecraft)|Clementine]] mission, which has been superseded by [[Lunar Reconnaissance Orbiter]]}} |
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{{one source|date=June 2017}} |
{{one source|date=June 2017}} |
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[[Image:MoonTopoLOLA.png|thumb|right|345px|alt=Topography of the Moon measured from the Lunar Orbiter Laser Altimeter on the mission [[Lunar Reconnaissance Orbiter]], referenced to a sphere of radius 1737.4 km|Topography of the Moon.]] |
[[Image:MoonTopoLOLA.png|thumb|right|345px|alt=Topography of the Moon measured from the Lunar Orbiter Laser Altimeter on the mission [[Lunar Reconnaissance Orbiter]], referenced to a sphere of radius 1737.4 km|Topography of the Moon.]] |
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The '''[[topography]] of the [[Moon]]''' has been measured by the methods of laser altimetry and stereo image analysis, most recently from data obtained during the [[Clementine mission]]. The most visible topographic feature is the giant far side [[South Pole-Aitken basin]], which possesses the lowest [[elevation]]s of the Moon. The highest elevations are found just to the north-east of this basin, and it has been suggested that this area might represent thick [[ejecta]] deposits that were emplaced during an oblique South Pole-Aitken basin impact event. Other large impact basins, such as the [[Lunar mare|maria]] [[Mare Imbrium|Imbrium]], [[Mare Serenitatis|Serenitatis]], [[Mare Crisium|Crisium]], [[Mare Smythii|Smythii]], and [[Mare Orientale|Orientale]], also possess regionally low elevations and elevated [[Rim (craters)|rim]]s. |
The '''[[topography]] of the [[Moon]]''' has been measured by the methods of laser altimetry and stereo image analysis, most recently from data obtained during the [[Clementine mission]]. The most visible topographic feature is the giant far side [[South Pole-Aitken basin]], which possesses the lowest [[elevation]]s of the Moon. The highest elevations are found just to the north-east of this basin, and it has been suggested that this area might represent thick [[ejecta]] deposits that were emplaced during an oblique South Pole-Aitken basin impact event. Other large impact basins, such as the [[Lunar mare|maria]] [[Mare Imbrium|Imbrium]], [[Mare Serenitatis|Serenitatis]], [[Mare Crisium|Crisium]], [[Mare Smythii|Smythii]], and [[Mare Orientale|Orientale]], also possess regionally low elevations and elevated [[Rim (craters)|rim]]s. |
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Another distinguishing feature of the Moon's shape is that the elevations are on average about 1.9 [[Kilometre|km]] higher on the far side than the near side. If it is assumed that the [[Crust (geology)|crust]] is in [[Isostasy|isostatic equilibrium]], and that the density of the crust is everywhere the same, then the higher elevations would be associated with a thicker crust. Using gravity, topography and [[Seismology|seismic]] data, the crust is thought to be on average about {{nowrap|50 ± 15 km}} thick, with the far-side crust being on average thicker than the near side by about 15 km.<ref name="W06">{{cite journal |author=Mark Wieczorek |display-authors=etal |title=The constitution and structure of the lunar interior |journal=Reviews in Mineralogy and Geochemistry |volume=60 |pages=221–364 |date=2006 |doi=10.2138/rmg.2006.60.3 |first1=M. A.|bibcode=2006RvMG...60..221W }}</ref> |
Another distinguishing feature of the Moon's shape is that the elevations are on average about 1.9 [[Kilometre|km]] higher on the far side than the near side. If it is assumed that the [[Crust (geology)|crust]] is in [[Isostasy|isostatic equilibrium]], and that the density of the crust is everywhere the same, then the higher elevations would be associated with a thicker crust. Using gravity, topography and [[Seismology|seismic]] data, the crust is thought to be on average about {{nowrap|50 ± 15 km}} thick, with the far-side crust being on average thicker than the near side by about 15 km.<ref name="W06">{{cite journal |author=Mark Wieczorek |display-authors=etal |title=The constitution and structure of the lunar interior |journal=Reviews in Mineralogy and Geochemistry |volume=60 |pages=221–364 |date=2006 |doi=10.2138/rmg.2006.60.3 |first1=M. A.|bibcode=2006RvMG...60..221W }}</ref>{{Obsolete source|reason=more recent topography data exists from [[Lunar Reconnaissance Orbiter]]|date=September 2018}} |
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{{multiple image|total_width=600|align=center |
{{multiple image|total_width=600|align=center |
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|header=[[Moon|The Moon]]|width1=18000|height1=18000|image1=LRO WAC Nearside Mosaic.jpg |caption1=[[Near side of the Moon|Lunar near side]] |width2=18000 |height2=18000 |image2=Moon Farside LRO.jpg |caption2=[[Far side of the Moon|Lunar far side]]|width3=18622|height3=18622|image3=LRO WAC North Pole Mosaic (PIA14024).jpg|caption3=[[Lunar north pole]]|width4=6082|height4=6082|image4=LRO WAC South Pole Mosaic.jpg|caption4=[[Lunar south pole]] }} |
|header=[[Moon|The Moon]]|width1=18000|height1=18000|image1=LRO WAC Nearside Mosaic.jpg |caption1=[[Near side of the Moon|Lunar near side]] |width2=18000 |height2=18000 |image2=Moon Farside LRO.jpg |caption2=[[Far side of the Moon|Lunar far side]]|width3=18622|height3=18622|image3=LRO WAC North Pole Mosaic (PIA14024).jpg|caption3=[[Lunar north pole]]|width4=6082|height4=6082|image4=LRO WAC South Pole Mosaic.jpg|caption4=[[Lunar south pole]] }} |
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Revision as of 14:38, 28 September 2018
 | The factual accuracy of parts of this article (those related to data from the Clementine mission, which has been superseded by Lunar Reconnaissance Orbiter) may be compromised due to out-of-date information. (September 2018) |
 | This article relies largely or entirely on a single source. (June 2017) |
The topography of the Moon has been measured by the methods of laser altimetry and stereo image analysis, most recently from data obtained during the Clementine mission. The most visible topographic feature is the giant far side South Pole-Aitken basin, which possesses the lowest elevations of the Moon. The highest elevations are found just to the north-east of this basin, and it has been suggested that this area might represent thick ejecta deposits that were emplaced during an oblique South Pole-Aitken basin impact event. Other large impact basins, such as the maria Imbrium, Serenitatis, Crisium, Smythii, and Orientale, also possess regionally low elevations and elevated rims.
Another distinguishing feature of the Moon's shape is that the elevations are on average about 1.9 km higher on the far side than the near side. If it is assumed that the crust is in isostatic equilibrium, and that the density of the crust is everywhere the same, then the higher elevations would be associated with a thicker crust. Using gravity, topography and seismic data, the crust is thought to be on average about 50 ± 15 km thick, with the far-side crust being on average thicker than the near side by about 15 km.[1][obsolete source]
.jpg)
Moon – Oceanus Procellarum ("Ocean of Storms")
Ancient rift valleys – rectangular structure (visible – topography – GRAIL gravity gradients) (October 1, 2014).
Ancient rift valleys – context.
Ancient rift valleys – closeup (artist's concept).
See also
References
- ^ Mark Wieczorek, M. A.; et al. (2006). "The constitution and structure of the lunar interior". Reviews in Mineralogy and Geochemistry. 60: 221–364. Bibcode:2006RvMG...60..221W. doi:10.2138/rmg.2006.60.3.
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