The moon and the planets

, Volume 22, Issue 3, pp 367–382 | Cite as

The moon as the origin of the Earth's continents

  • Tovy Grjebine
Article

Abstract

Paleontological data and celestial mechanics suggest that the Moon may have stayed in a geosynchronous corotation around the Earth as a geostationary satellite. Excess energy may have slowly been released as heat, transferred as movement around the Sund or lost with matter ejected into space.

The radial segregation process which was responsible for the formation of the Earth's iron core also brought water and lithophile elements dissolved in the water towards the surface. These elements were deposited in the area facing the Moon for several reasons, and a single continent was formed. Its level continuously matched the sea level, so the continent was formed under shallow water. When the geosynchronous corotation of the Moon became impossible, the tides become important, the Moon receded and the Earth slowed down and became more and more spherical; the variation of its oblateness from about 8% to 0.3% was incompatible with the shape of the continent, that broke into pieces.

Almost all the data were have on the Earth's age, the composition of the continents, sea water and the atmosphere fit this approach as does lunar data.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. Alfvén, H. and Arrhenius, G.: 1969),Science 165, 11–17.Google Scholar
  2. Alfvén, H. and Arrhenius, G.: 1972,The Moon 5, 210–230.Google Scholar
  3. Arnorsson, S. and Sigurdsson, S.: (1974),Geothermics 3, 127–141.Google Scholar
  4. Berry, W. and Baker, R. M.: 1968),Nature 217, 938–939.Google Scholar
  5. Collinson, D. W., Stephenson, A., and Runcorn, S. K.: (1977),Phil. Trans. Roy. Soc. London A285, 241–247.Google Scholar
  6. Daillet, S.: (1978),Ann. Geophys. 34, fasc. 2, 79–87.Google Scholar
  7. Gerstenkorn, H.: (1955),H. Z. Astrophys. 26, 245.Google Scholar
  8. Grjebine, T. and Marchal, Ch.: (1980a) ‘Fission and geosynchronous release of the Moon’,The Moon and the Planets 22, 347–358.Google Scholar
  9. Grjebine, T. and Marchal, Ch.: (1980b), ‘Consequences of a geosynchronous phase for the Moon’,The Moon and the Planets 22, 359–366.Google Scholar
  10. Hunten, D. M.: (1973),Jour. Atmos. Sci. 31, 305–317.Google Scholar
  11. Ingersoll, A. P.: (1969),Jour. Atmos. Sci. 26, 1191–1198.Google Scholar
  12. Kahn, G. K. and Pompea, S. M.: (1978),Nature 275, 606–611.Google Scholar
  13. Lyttleton, R. A.: (1953),Monthly Notices Roy. Astron. Soc. 97, 108–115.Google Scholar
  14. MacDonald, G. J. F.: (1964),Review Geophys. 2, 467–541.Google Scholar
  15. Nordmann, D.: (1978) Personal Communication.Google Scholar
  16. O'Keefe, J. A.: (1969),Jour. Geophys. Research 74, 2758–2767.Google Scholar
  17. Pannella, G.: (1972),Astrophysics and Space Sci. 16, 212–239.Google Scholar
  18. Petren, O. and Walin, G.: 1976),Tellus 28, 74–87.Google Scholar
  19. Ringwood, A. E.: (1970),Earth Plan. Sci. Letter 8, 131–140.Google Scholar
  20. Runcorn, S. K.: (1968),Nature 218, 459.Google Scholar
  21. Runcorn, S. K.: (1977)Phil. Trans. Roy. Soc. Lond. A285, 507–516.Google Scholar
  22. Turcotte, D. L., Nordmann, J. C., and Cisne, J. L.: (1974),Nature 251, 124–125.Google Scholar
  23. Walker, J. C. G.: (1976),Evolution of the Atmosphere, Hafner, New York.Google Scholar
  24. Walker, J. C. G.: (1975) in B. F. Windley (Ed.),The Early History of the Earth J. Wiley, London.Google Scholar
  25. Wasserburg, G. J., Papanastassiou, D. A., and Tera, F.: (1977),Phil. Trans. Roy. Soc. London A285, 7–22.Google Scholar
  26. Well, J. W.: (1963),Nature 197, 948–950.Google Scholar

Copyright information

© D. R. Reidel Publishing Co 1980

Authors and Affiliations

  • Tovy Grjebine
    • 1
  1. 1.Intergroupe Energie de la MajoritéAssemblée NationaleParisFrance

Personalised recommendations