Internal structure of the Moon - Revision history

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			{{Short description\|none}} <!-- This short description is INTENTIONALLY "none" - please see WP:SDNONE before you consider changing it! -->
	{{see also\|Geology of the Moon}}		{{see also\|Geology of the Moon}}
	[[File:Return of the moon diagram.svg\|thumb\|400px\|Moon's internal structure]]		[[File:Return of the moon diagram.svg\|thumb\|400px\|Moon's internal structure.]]
	[[File:Lunar Olivine Basalt 15555 from Apollo 15 in National Museum of Natural History.jpg\|thumb\|350px\|[[Olivine]] [[basalt]] collected by [[Apollo 15]].]]		[[File:Lunar Olivine Basalt 15555 from Apollo 15 in National Museum of Natural History.jpg\|thumb\|350px\|[[Olivine]] [[basalt]] collected by [[Apollo 15]].]]
	[[File:Thermal state of the Moon at age 100 Ma.jpg\|thumb\|300px\|Thermal state of the Moon at age 100 Ma.<ref>{{cite journal \|last1=Maurice \|first1=M. \|last2=Tosi \|first2=N. \|last3=Schwinger \|first3=S. \|last4=Breuer \|first4=D. \|last5=Kleine \|first5=T. \|title=A long-lived magma ocean on a young Moon \|journal=Science Advances \|date=1 July 2020 \|volume=6 \|issue=28 \|~~pages~~=eaba8949 \|doi=10.1126/sciadv.aba8949\|pmid=32695879 \|pmc=7351470 \|bibcode=2020SciA....6.8949M \|language=en \|issn=2375-2548\|doi-access=free }} [[File:CC-BY icon.svg\|50px]] Text and images are available under a [https://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International License].</ref>]]		[[File:Thermal state of the Moon at age 100 Ma.jpg\|thumb\|300px\|Thermal state of the Moon at age 100 Ma.<ref>{{cite journal \|last1=Maurice \|first1=M. \|last2=Tosi \|first2=N. \|last3=Schwinger \|first3=S. \|last4=Breuer \|first4=D. \|last5=Kleine \|first5=T. \|title=A long-lived magma ocean on a young Moon \|journal=Science Advances \|date=1 July 2020 \|volume=6 \|issue=28 \|article-number=eaba8949 \|doi=10.1126/sciadv.aba8949\|pmid=32695879 \|pmc=7351470 \|bibcode=2020SciA....6.8949M \|language=en \|issn=2375-2548\|doi-access=free }} [[File:CC-BY icon.svg\|50px]] Text and images are available under a [https://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International License].</ref>]]
	Having a ~~[[Arithmetic mean\|~~mean]] density of 3,346.4 [[Kilogram per metre cubed\|kg/m<sup>3</sup>]],<ref>Making it the second densest satellite in the [[Solar System]] after [[Io (moon)\|Io]]</ref> the [[Moon]] is a [[Planetary differentiation\|differentiated]] body, being composed of a [[Geochemistry\|geochemically]] distinct [[Crust (geology)\|crust]], [[Mantle (geology)\|mantle]], and [[planetary core]]. This structure is believed to have resulted from the [[Fractional crystallization (geology)\|fractional crystallization]] of a [[Lunar magma ocean\|magma ocean]] shortly after its formation about 4.5 billion years ago. The energy required to melt the outer portion of the Moon is commonly attributed to a [[~~giant~~ impact hypothesis\|giant impact]] event that is postulated to have formed the Earth-Moon system, and the subsequent [[Accretion_(astrophysics)\|reaccretion]] of material in Earth orbit. Crystallization of this magma ocean would have given rise to a [[mafic]] mantle and a [[plagioclase]]-rich crust.		Having a mean density of 3,346.4 [[Kilogram per metre cubed\|kg/m<sup>3</sup>]],<ref>Making it the second densest satellite in the [[Solar System]] after [[Io (moon)\|Io]]</ref> the [[Moon]] is a [[Planetary differentiation\|differentiated]] body, being composed of a [[Geochemistry\|geochemically]] distinct [[Crust (geology)\|crust]], [[Mantle (geology)\|mantle]], and [[planetary core]]. This structure is believed to have resulted from the [[Fractional crystallization (geology)\|fractional crystallization]] of a [[Lunar magma ocean\|magma ocean]] shortly after its formation about 4.5 billion years ago. The energy required to melt the outer portion of the Moon is commonly attributed to a [[Giant-impact hypothesis\|giant impact]] event that is postulated to have formed the Earth-Moon system, and the subsequent [[Accretion_(astrophysics)\|reaccretion]] of material in Earth orbit. Crystallization of this magma ocean would have given rise to a [[mafic]] mantle and a [[plagioclase]]-rich crust.

	Geochemical mapping from orbit implies that the crust of the Moon is largely [[Anorthosite\|anorthositic]] in composition,<ref name="L06">{{cite journal \|last1=P. Lucey and 12 coauthors \|title=Understanding the lunar surface and space-Moon interactions \|journal=Reviews in Mineralogy and Geochemistry \|volume=60 \|issue=1 \|pages=83–219 \|date=2006 \|doi=10.2138/rmg.2006.60.2 \|first1=P.\|bibcode=2006RvMG...60...83L }}</ref> consistent with the magma ocean hypothesis. In terms of elements, the lunar crust is composed primarily of [[oxygen]], [[silicon]], [[magnesium]], [[iron]], [[calcium]], and [[aluminium]], but important minor and trace elements such as [[titanium]], [[uranium]], [[thorium]], [[potassium]], and [[hydrogen]] are present as well. Based on geophysical techniques, the crust is estimated to be on average about 50~~ ~~km thick.<ref name="W06">{{cite journal \|url=http://scripts.mit.edu/~paleomag/articles/60_03_Wieczorek_etal.pdf \|last1=Mark Wieczorek and 15 coauthors \|title=The constitution and structure of the lunar interior \|journal=Reviews in Mineralogy and Geochemistry \|volume=60 \|issue=1 \|pages=221–364 \|date=2006 \|doi=10.2138/rmg.2006.60.3 \|first1=M. A. ~~\|url-status=dead~~ \|archive-url=https://web.archive.org/web/20141221063318/http://scripts.mit.edu/~paleomag/articles/60_03_Wieczorek_etal.pdf \|archive-date=2014-12-21 \|bibcode=2006RvMG...60..221W }}</ref>		Geochemical mapping from orbit implies that the crust of the Moon is largely [[Anorthosite\|anorthositic]] in composition,<ref name="L06">{{cite journal \|last1=P. Lucey and 12 coauthors \|title=Understanding the lunar surface and space-Moon interactions \|journal=Reviews in Mineralogy and Geochemistry \|volume=60 \|issue=1 \|pages=83–219 \|date=2006 \|doi=10.2138/rmg.2006.60.2 \|first1=P.\|bibcode=2006RvMG...60...83L }}</ref> consistent with the magma ocean hypothesis. In terms of elements, the lunar crust is composed primarily of [[oxygen]], [[silicon]], [[magnesium]], [[iron]], [[calcium]], and [[aluminium]], but important minor and trace elements such as [[titanium]], [[uranium]], [[thorium]], [[potassium]], [[Sulfur\|sulphur]], [[manganese]], [[chromium]],<ref>{{Cite web \|date=2023-08-30 \|title=What Chandrayaan 3 has found on moon so far: Oxygen, sulphur, iron, silicon \|url=https://www.hindustantimes.com/india-news/what-chandrayaan-3-has-found-on-moon-so-far-oxygen-sulphur-iron-silicon-101693360903346.html \|access-date=2023-11-15 \|website=Hindustan Times \|language=en}}</ref> and [[hydrogen]] are present as well. Based on geophysical techniques, the crust is estimated to be on average about 50 km thick.<ref name="W06">{{cite journal \|url=http://scripts.mit.edu/~paleomag/articles/60_03_Wieczorek_etal.pdf \|last1=Mark Wieczorek and 15 coauthors \|title=The constitution and structure of the lunar interior \|journal=Reviews in Mineralogy and Geochemistry \|volume=60 \|issue=1 \|pages=221–364 \|date=2006 \|doi=10.2138/rmg.2006.60.3 \|first1=M. A. \|archive-url=https://web.archive.org/web/20141221063318/http://scripts.mit.edu/~paleomag/articles/60_03_Wieczorek_etal.pdf \|archive-date=2014-12-21 \|bibcode=2006RvMG...60..221W }}</ref>

	Partial melting within the mantle of the Moon gave rise to the eruption of mare basalts on the lunar surface. Analyses of these basalts indicate that the mantle is composed predominantly of the minerals [[olivine]], [[orthopyroxene]] and [[clinopyroxene]], and that the lunar mantle is more iron-rich than that of the Earth. Some lunar basalts contain high abundances of titanium (present in the mineral [[ilmenite]]), suggesting that the mantle is highly heterogeneous in composition. [[~~Moonquake~~]]s have been found to occur deep within the mantle of the Moon about 1,000 km below the surface. These occur with monthly periodicities and are related to tidal stresses caused by the eccentric orbit of the Moon about the Earth. A few shallow moonquakes with hypocenters located about 100 km below the surface have also been detected, but these occur more infrequently and appear to be unrelated to the lunar tides.<ref name="W06"/>		Partial melting within the mantle of the Moon gave rise to the eruption of mare basalts on the lunar surface. Analyses of these basalts indicate that the mantle is composed predominantly of the minerals [[olivine]], [[orthopyroxene]] and [[clinopyroxene]], and that the lunar mantle is more iron-rich than that of the Earth. Some lunar basalts contain high abundances of titanium (present in the mineral [[ilmenite]]), suggesting that the mantle is highly heterogeneous in composition. [[Quake (natural phenomenon)\|Moonquakes]] have been found to occur deep within the mantle of the Moon about 1,000 km below the surface. These occur with monthly periodicities and are related to tidal stresses caused by the eccentric orbit of the Moon about the Earth. A few shallow moonquakes with hypocenters located about 100 km below the surface have also been detected, but these occur more infrequently and appear to be unrelated to the lunar tides.<ref name="W06"/>

	==Core==		==Core==
	[[File:Moon Schematic Cross Section.svg\|right\|thumb\|350px\|Schematic illustration of the internal structure of the Moon]]		[[File:Moon Schematic Cross Section.svg\|right\|thumb\|350px\|Schematic illustration of the internal structure of the Moon.]]
	Several lines of evidence imply that the lunar core is small, with a radius of about 350 km or less.<ref name="W06"/> The ~~size~~ of the lunar core is only about 20% the ~~size~~ of the Moon itself, in contrast to about 50% as is the case for most other terrestrial bodies. The composition of the lunar core is not well constrained, but most believe that it is composed of metallic iron alloy with a small amount of [[sulfur]] and [[nickel]]. Analyses of the Moon's time-variable rotations indicate that the core is at least partly molten.<ref>{{cite journal \|author1=J. G. Williams \|author2=S. G. Turyshev \|author3=D. H. Boggs \|author4=J. T. Ratcliff \|title=Lunar laser ranging science: Gravitational physics and lunar interior and geodesy \|journal=Advances in Space Research \|date=2006 \|volume=37 \|issue=1 \|pages=67–71 \|doi=10.1016/j.asr.2005.05.013\|arxiv = gr-qc/0412049 \|bibcode=2006AdSpR..37...67W \|s2cid=14801321 }}</ref> Within the giant-impact formation scenario, the core formation of Moon could have occurred within the initial 100–1000 years from the commencement of its accretion from its moonlets. <ref>{{cite journal \|author1=S. Sahijpal \|author2=V. Goyal \|title=Thermal evolution of the early Moon \|journal=Meteoritics and Planetary Science Journal \|date=2018 \|volume=53 \|issue=10 \|pages=2193–2211 \|doi=10.1111/maps.13119\| arxiv=2001.07123 \|bibcode=2018M&PS...53.2193S \|s2cid=134291699 }}</ref>		Several lines of evidence imply that the lunar core is small, with a radius of about 350 km or less.<ref name="W06"/> The diameter of the lunar core is only about 20% the diameter of the Moon itself, in contrast to about 50% as is the case for most other terrestrial bodies. The composition of the lunar core is not well constrained, but most believe that it is composed of metallic iron alloy with a small amount of [[sulfur]] and [[nickel]]. Analyses of the Moon's time-variable rotations indicate that the core is at least partly molten.<ref>{{cite journal \|author1=J. G. Williams \|author2=S. G. Turyshev \|author3=D. H. Boggs \|author4=J. T. Ratcliff \|title=Lunar laser ranging science: Gravitational physics and lunar interior and geodesy \|journal=Advances in Space Research \|date=2006 \|volume=37 \|issue=1 \|pages=67–71 \|doi=10.1016/j.asr.2005.05.013\|arxiv = gr-qc/0412049 \|bibcode=2006AdSpR..37...67W \|s2cid=14801321 }}</ref> Within the giant-impact formation scenario, the core formation of Moon could have occurred within the initial 100–1000 years from the commencement of its accretion from its moonlets.<ref>{{cite journal \|author1=S. Sahijpal \|author2=V. Goyal \|title=Thermal evolution of the early Moon \|journal=Meteoritics and Planetary Science Journal \|date=2018 \|volume=53 \|issue=10 \|pages=2193–2211 \|doi=10.1111/maps.13119\| arxiv=2001.07123 \|bibcode=2018M&PS...53.2193S \|s2cid=134291699 }}</ref>

	In 2010, a reanalysis of the old [[Apollo Lunar Surface Experiments Package\|Apollo]] seismic data on the deep ~~[[moonquake]]s~~ using modern processing methods confirmed that the Moon has an iron rich core with a radius of {{nowrap\|330 ± 20 km}}. The same reanalysis established that the solid inner core made of pure iron has a radius of {{nowrap\|240 ± 10 km}}. The core is surrounded by the partially (10 to 30%) melted layer of the lower mantle with a radius of {{nowrap\|480 ± 20 km}} (thickness ~150 km). These results imply that 40% of the core by volume has solidified. The density of the liquid outer core is about 5 g/cm<sup>3</sup> and it could contain as much as 6% [[sulfur]] by weight. The temperature in the core is probably about 1600–1700 K (1330–1430 °C).<ref name=Weber2010/>		In 2010, a reanalysis of the old [[Apollo Lunar Surface Experiments Package\|Apollo]] seismic data on the deep moonquakes using modern processing methods confirmed that the Moon has an iron rich core with a radius of {{nowrap\|330 ± 20 km}}. The same reanalysis established that the solid inner core made of pure iron has a radius of {{nowrap\|240 ± 10 km}}. The core is surrounded by the partially (10 to 30%) melted layer of the lower mantle with a radius of {{nowrap\|480 ± 20 km}} (thickness ~150 km). These results imply that 40% of the core by volume has solidified. The density of the liquid outer core is about 5 g/cm<sup>3</sup> and it could contain as much as 6% [[sulfur]] by weight. The temperature in the core is probably about 1600–1700 K (1330–1430 °C).<ref name=Weber2010/>
	{{multiple image\|total_width=600\|align=center		{{multiple image\|total_width=600\|align=center
	\|header=Moon – [[Oceanus Procellarum]] ("Ocean of Storms")\|width1=614 \|height1=228 \|image1=14-236-LunarGrailMission-OceanusProcellarum-Rifts-Overall-20141001.jpg\|caption1=Ancient [[rift valley]]s – rectangular structure (visible – topography – [[Gravity Recovery and Interior Laboratory\|GRAIL gravity gradients]]) (October 1, 2014).\|width2=1500 \|height2=1500 \|image2=PIA18822-LunarGrailMission-OceanusProcellarum-Rifts-Overall-20141001.jpg\|caption2=Ancient [[rift valley]]s – context.\|width3=1546 \|height3=905 \|image3=PIA18821-LunarGrailMission-OceanusProcellarum-Rifts-Closeup-20141001.jpg\|caption3=Ancient [[rift valley]]s – closeup (artist's concept).}}		\|header=Moon – [[Oceanus Procellarum]] ("Ocean of Storms")\|width1=614 \|height1=228 \|image1=14-236-LunarGrailMission-OceanusProcellarum-Rifts-Overall-20141001.jpg\|caption1=Ancient [[rift valley]]s – rectangular structure (visible – topography – [[Gravity Recovery and Interior Laboratory\|GRAIL gravity gradients]]) (October 1, 2014).\|width2=1500 \|height2=1500 \|image2=PIA18822-LunarGrailMission-OceanusProcellarum-Rifts-Overall-20141001.jpg\|caption2=Ancient [[rift valley]]s – context.\|width3=1546 \|height3=905 \|image3=PIA18821-LunarGrailMission-OceanusProcellarum-Rifts-Closeup-20141001.jpg\|caption3=Ancient [[rift valley]]s – closeup (artist's concept).}}
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	==References==		==References==
	~~{{reflist\|refs=~~		<references>
	<ref name=Weber2010>{{Cite journal \| last1 = Weber \| first1 = R. C. \| last2 = Lin \| first2 = P.-Y. \| last3 = Garnero \| first3 = E. J. \| last4 = Williams \| first4 = Q. \| last5 = Lognonne \| first5 = P. \| title = Seismic Detection of the Lunar Core \| doi = 10.1126/science.1199375 \| journal = Science \| volume = 331 \| issue = 6015 \| pages = 309–312 \| year = 2011 \| pmid = 21212323\|bibcode = 2011Sci...331..309W \| s2cid = 206530647 \| url = https://zenodo.org/record/1230912 }}</ref>}}		<ref name=Weber2010>{{Cite journal \| last1 = Weber \| first1 = R. C. \| last2 = Lin \| first2 = P.-Y. \| last3 = Garnero \| first3 = E. J. \| last4 = Williams \| first4 = Q. \| last5 = Lognonne \| first5 = P. \| title = Seismic Detection of the Lunar Core \| doi = 10.1126/science.1199375 \| journal = Science \| volume = 331 \| issue = 6015 \| pages = 309–312 \| year = 2011 \| pmid = 21212323\|bibcode = 2011Sci...331..309W \| s2cid = 206530647 \| url = https://zenodo.org/record/1230912 }}</ref>
			</references>

	==External links==		==External links==
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	{{Planetary Geology}}		{{Planetary Geology}}

	[[Category:~~Lunar science~~]]		[[Category:Geology of the Moon]]

Ajay Kumar: Created a new article

2023-08-23T13:17:01Z

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New page

{{see also|Geology of the Moon}}
[[File:Return of the moon diagram.svg|thumb|400px|Moon's internal structure]]
[[File:Lunar Olivine Basalt 15555 from Apollo 15 in National Museum of Natural History.jpg|thumb|350px|[[Olivine]] [[basalt]] collected by [[Apollo 15]].]]
[[File:Thermal state of the Moon at age 100 Ma.jpg|thumb|300px|Thermal state of the Moon at age 100 Ma.<ref>{{cite journal |last1=Maurice |first1=M. |last2=Tosi |first2=N. |last3=Schwinger |first3=S. |last4=Breuer |first4=D. |last5=Kleine |first5=T. |title=A long-lived magma ocean on a young Moon |journal=Science Advances |date=1 July 2020 |volume=6 |issue=28 |pages=eaba8949 |doi=10.1126/sciadv.aba8949|pmid=32695879 |pmc=7351470 |bibcode=2020SciA....6.8949M |language=en |issn=2375-2548|doi-access=free }} [[File:CC-BY icon.svg|50px]] Text and images are available under a [https://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International License].</ref>]]
Having a [[Arithmetic mean|mean]] density of 3,346.4 [[Kilogram per metre cubed|kg/m<sup>3</sup>]],<ref>Making it the second densest satellite in the [[Solar System]] after [[Io (moon)|Io]]</ref> the [[Moon]] is a [[Planetary differentiation|differentiated]] body, being composed of a [[Geochemistry|geochemically]] distinct [[Crust (geology)|crust]], [[Mantle (geology)|mantle]], and [[planetary core]]. This structure is believed to have resulted from the [[Fractional crystallization (geology)|fractional crystallization]] of a [[Lunar magma ocean|magma ocean]] shortly after its formation about 4.5 billion years ago. The energy required to melt the outer portion of the Moon is commonly attributed to a [[giant impact hypothesis|giant impact]] event that is postulated to have formed the Earth-Moon system, and the subsequent [[Accretion_(astrophysics)|reaccretion]] of material in Earth orbit. Crystallization of this magma ocean would have given rise to a [[mafic]] mantle and a [[plagioclase]]-rich crust.

Geochemical mapping from orbit implies that the crust of the Moon is largely [[Anorthosite|anorthositic]] in composition,<ref name="L06">{{cite journal |last1=P. Lucey and 12 coauthors |title=Understanding the lunar surface and space-Moon interactions |journal=Reviews in Mineralogy and Geochemistry |volume=60 |issue=1 |pages=83–219 |date=2006 |doi=10.2138/rmg.2006.60.2 |first1=P.|bibcode=2006RvMG...60...83L }}</ref> consistent with the magma ocean hypothesis. In terms of elements, the lunar crust is composed primarily of [[oxygen]], [[silicon]], [[magnesium]], [[iron]], [[calcium]], and [[aluminium]], but important minor and trace elements such as [[titanium]], [[uranium]], [[thorium]], [[potassium]], and [[hydrogen]] are present as well. Based on geophysical techniques, the crust is estimated to be on average about 50 km thick.<ref name="W06">{{cite journal |url=http://scripts.mit.edu/~paleomag/articles/60_03_Wieczorek_etal.pdf |last1=Mark Wieczorek and 15 coauthors |title=The constitution and structure of the lunar interior |journal=Reviews in Mineralogy and Geochemistry |volume=60 |issue=1 |pages=221–364 |date=2006 |doi=10.2138/rmg.2006.60.3 |first1=M. A. |url-status=dead |archive-url=https://web.archive.org/web/20141221063318/http://scripts.mit.edu/~paleomag/articles/60_03_Wieczorek_etal.pdf |archive-date=2014-12-21 |bibcode=2006RvMG...60..221W }}</ref>

Partial melting within the mantle of the Moon gave rise to the eruption of mare basalts on the lunar surface. Analyses of these basalts indicate that the mantle is composed predominantly of the minerals [[olivine]], [[orthopyroxene]] and [[clinopyroxene]], and that the lunar mantle is more iron-rich than that of the Earth. Some lunar basalts contain high abundances of titanium (present in the mineral [[ilmenite]]), suggesting that the mantle is highly heterogeneous in composition. [[Moonquake]]s have been found to occur deep within the mantle of the Moon about 1,000 km below the surface. These occur with monthly periodicities and are related to tidal stresses caused by the eccentric orbit of the Moon about the Earth. A few shallow moonquakes with hypocenters located about 100 km below the surface have also been detected, but these occur more infrequently and appear to be unrelated to the lunar tides.<ref name="W06"/>

==Core==
[[File:Moon Schematic Cross Section.svg|right|thumb|350px|Schematic illustration of the internal structure of the Moon]]
Several lines of evidence imply that the lunar core is small, with a radius of about 350 km or less.<ref name="W06"/> The size of the lunar core is only about 20% the size of the Moon itself, in contrast to about 50% as is the case for most other terrestrial bodies. The composition of the lunar core is not well constrained, but most believe that it is composed of metallic iron alloy with a small amount of [[sulfur]] and [[nickel]]. Analyses of the Moon's time-variable rotations indicate that the core is at least partly molten.<ref>{{cite journal |author1=J. G. Williams |author2=S. G. Turyshev |author3=D. H. Boggs |author4=J. T. Ratcliff |title=Lunar laser ranging science: Gravitational physics and lunar interior and geodesy |journal=Advances in Space Research |date=2006 |volume=37 |issue=1 |pages=67–71 |doi=10.1016/j.asr.2005.05.013|arxiv = gr-qc/0412049 |bibcode=2006AdSpR..37...67W |s2cid=14801321 }}</ref> Within the giant-impact formation scenario, the core formation of Moon could have occurred within the initial 100–1000 years from the commencement of its accretion from its moonlets. <ref>{{cite journal |author1=S. Sahijpal |author2=V. Goyal |title=Thermal evolution of the early Moon |journal=Meteoritics and Planetary Science Journal |date=2018 |volume=53 |issue=10 |pages=2193–2211 |doi=10.1111/maps.13119| arxiv=2001.07123 |bibcode=2018M&PS...53.2193S |s2cid=134291699 }}</ref>

In 2010, a reanalysis of the old [[Apollo Lunar Surface Experiments Package|Apollo]] seismic data on the deep [[moonquake]]s using modern processing methods confirmed that the Moon has an iron rich core with a radius of {{nowrap|330 ± 20 km}}. The same reanalysis established that the solid inner core made of pure iron has a radius of {{nowrap|240 ± 10 km}}. The core is surrounded by the partially (10 to 30%) melted layer of the lower mantle with a radius of {{nowrap|480 ± 20 km}} (thickness ~150 km). These results imply that 40% of the core by volume has solidified. The density of the liquid outer core is about 5 g/cm<sup>3</sup> and it could contain as much as 6% [[sulfur]] by weight. The temperature in the core is probably about 1600–1700 K (1330–1430 °C).<ref name=Weber2010/>
{{multiple image|total_width=600|align=center
|header=Moon – [[Oceanus Procellarum]] ("Ocean of Storms")|width1=614 |height1=228 |image1=14-236-LunarGrailMission-OceanusProcellarum-Rifts-Overall-20141001.jpg|caption1=Ancient [[rift valley]]s – rectangular structure (visible – topography – [[Gravity Recovery and Interior Laboratory|GRAIL gravity gradients]]) (October 1, 2014).|width2=1500 |height2=1500 |image2=PIA18822-LunarGrailMission-OceanusProcellarum-Rifts-Overall-20141001.jpg|caption2=Ancient [[rift valley]]s – context.|width3=1546 |height3=905 |image3=PIA18821-LunarGrailMission-OceanusProcellarum-Rifts-Closeup-20141001.jpg|caption3=Ancient [[rift valley]]s – closeup (artist's concept).}}

In 2019, a reanalysis of nearly 50 years of data collected from the [[Lunar Laser Ranging experiment]] with lunar gravity field data from the [[GRAIL]] mission, shows that for a relaxed lunar fluid core with non-hydrostatic lithospheres, the core [[flattening]] is determined as {{val|2.2|0.6|e=-4}} with the radii of its core-mantle boundary as {{val|381|12|u=km}}.<ref>{{cite journal |last1=Viswanathan |first1=V. |last2=Rambaux |first2=N. |last3=Fienga |first3=A. |last4=Laskar |first4=J. |last5=Gastineau |first5=M. |title=Observational Constraint on the Radius and Oblateness of the Lunar Core-Mantle Boundary |journal=[[Geophysical Research Letters]]|volume=46 |date=9 July 2019 |issue=13 |pages=7295–7303 |doi=10.1029/2019GL082677|arxiv=1903.07205 |bibcode=2019GeoRL..46.7295V |s2cid=119508748 }}</ref>

==See also==
{{Portal|Solar System}}
*[[Lunar resources]]
*[[Structure of the Earth]]

==References==
{{reflist|refs=
<ref name=Weber2010>{{Cite journal | last1 = Weber | first1 = R. C. | last2 = Lin | first2 = P.-Y. | last3 = Garnero | first3 = E. J. | last4 = Williams | first4 = Q. | last5 = Lognonne | first5 = P. | title = Seismic Detection of the Lunar Core | doi = 10.1126/science.1199375 | journal = Science | volume = 331 | issue = 6015 | pages = 309–312 | year = 2011 | pmid = 21212323|bibcode = 2011Sci...331..309W | s2cid = 206530647 | url = https://zenodo.org/record/1230912 }}</ref>}}

==External links==
*[http://www.psrd.hawaii.edu/Archive/Archive-Moon.html Moon articles in Planetary Science Research Discoveries], including articles about internal structure of the Moon

{{The Moon}}
{{Planetary Geology}}

[[Category:Lunar science]]