Lunar magma ocean

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search

According to the giant impact hypothesis a large amount of energy was liberated in the formation of the Moon and it is inferred that as a result a large portion of the Moon was once completely molten, forming a lunar magma ocean. Evidence for the magma ocean hypothesis comes from the highly anorthositic compositions of the crust in the lunar highlands, as well as the existence of rocks with a high concentration of the geochemical component referred to as KREEP.

Ages of formation and crystallization of the lunar magma ocean have been constrained by studies of isotopes of hafnium, tungsten, samarium, and neodymium. The magma ocean formed about 70 million years after the history of the Solar System began, and most of the ocean had crystallized by about 215 million years after that beginning (Brandon, 2007).


  • Alan Brandon (2007) "Planetary science: A younger moon". Nature 450, 1169-1170. doi:10.1038/4501169a
  • G. Jeffrey Taylor (November 28, 2003). "Hafnium, Tungsten, and the Differentiation of the Moon and Mars". Planetary Science Research Discoveries.

Extended scientific references[edit]

  • Wood, J. A., Dickey, J. S., Jr., Marvin, U. B., and Powell, B. N. (1970) "Lunar Anorthosites". Science, v. 167, no. 3918, p. 602.
  • Wood, J. A. (1972) "Thermal History and Early Magmatism in the Moon". Icarus, v.16(2), p. 229-240.
  • Wood, J. A. (1972) "Fragments of Terra Rock in the Apollo 12 Soil Samples and a Structural Model of the Moon". Icarus, v. 16(3), p. 462-501.