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Internal structure of the Moon

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See also: Geology of the Moon
Moon's internal structure
Olivine basalt collected by Apollo 15.
Thermal state of the Moon at age 100 Ma.[1]

Having a mean density of 3,346.4 kg/m3,[2] the Moon is a differentiated body, being composed of a geochemically distinct crust, mantle, and planetary core. This structure is believed to have resulted from the fractional crystallization of a 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 event that is postulated to have formed the Earth-Moon system, and the subsequent 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 anorthositic in composition,[3] 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, sulphur, manganese, chromium[4] and hydrogen are present as well. Based on geophysical techniques, the crust is estimated to be on average about 50 km thick.[5]

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. 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.[5]

Core

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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.[5] 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.[6] 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. [7]

In 2010, a reanalysis of the old Apollo seismic data on the deep moonquakes using modern processing methods confirmed that the Moon has an iron rich core with a radius of 330 ± 20 km. The same reanalysis established that the solid inner core made of pure iron has a radius of 240 ± 10 km. The core is surrounded by the partially (10 to 30%) melted layer of the lower mantle with a radius of 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/cm3 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).[8]

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).

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 (2.2±0.6)×10−4 with the radii of its core-mantle boundary as 381±12 km.[9]

See also

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References

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  1. ^ Maurice, M.; Tosi, N.; Schwinger, S.; Breuer, D.; Kleine, T. (1 July 2020). "A long-lived magma ocean on a young Moon". Science Advances. 6 (28): eaba8949. Bibcode:2020SciA....6.8949M. doi:10.1126/sciadv.aba8949. ISSN 2375-2548. PMC 7351470. PMID 32695879. Text and images are available under a Creative Commons Attribution 4.0 International License.
  2. ^ Making it the second densest satellite in the Solar System after Io
  3. ^ P. Lucey and 12 coauthors, P. (2006). "Understanding the lunar surface and space-Moon interactions". Reviews in Mineralogy and Geochemistry. 60 (1): 83–219. Bibcode:2006RvMG...60...83L. doi:10.2138/rmg.2006.60.2.{{cite journal}}: CS1 maint: numeric names: authors list (link)
  4. ^ "What Chandrayaan 3 has found on moon so far: Oxygen, sulphur, iron, silicon". Hindustan Times. 2023-08-30. Retrieved 2023-11-15.
  5. ^ a b c Mark Wieczorek and 15 coauthors, M. A. (2006). "The constitution and structure of the lunar interior" (PDF). Reviews in Mineralogy and Geochemistry. 60 (1): 221–364. Bibcode:2006RvMG...60..221W. doi:10.2138/rmg.2006.60.3. Archived from the original (PDF) on 2014-12-21.{{cite journal}}: CS1 maint: numeric names: authors list (link)
  6. ^ J. G. Williams; S. G. Turyshev; D. H. Boggs; J. T. Ratcliff (2006). "Lunar laser ranging science: Gravitational physics and lunar interior and geodesy". Advances in Space Research. 37 (1): 67–71. arXiv:gr-qc/0412049. Bibcode:2006AdSpR..37...67W. doi:10.1016/j.asr.2005.05.013. S2CID 14801321.
  7. ^ S. Sahijpal; V. Goyal (2018). "Thermal evolution of the early Moon". Meteoritics and Planetary Science Journal. 53 (10): 2193–2211. arXiv:2001.07123. Bibcode:2018M&PS...53.2193S. doi:10.1111/maps.13119. S2CID 134291699.
  8. ^ Weber, R. C.; Lin, P.-Y.; Garnero, E. J.; Williams, Q.; Lognonne, P. (2011). "Seismic Detection of the Lunar Core". Science. 331 (6015): 309–312. Bibcode:2011Sci...331..309W. doi:10.1126/science.1199375. PMID 21212323. S2CID 206530647.
  9. ^ Viswanathan, V.; Rambaux, N.; Fienga, A.; Laskar, J.; Gastineau, M. (9 July 2019). "Observational Constraint on the Radius and Oblateness of the Lunar Core-Mantle Boundary". Geophysical Research Letters. 46 (13): 7295–7303. arXiv:1903.07205. Bibcode:2019GeoRL..46.7295V. doi:10.1029/2019GL082677. S2CID 119508748.
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