Hostname: page-component-cd9895bd7-8ctnn Total loading time: 0 Render date: 2024-12-25T15:51:02.929Z Has data issue: false hasContentIssue false
  • English
  • Français

The Shape of the Moon

Published online by Cambridge University Press:  07 February 2017

S. K. Runcorn  and
S. Hofmann
S. K. Runcorn
Affiliation:
Department of Geophysics and Planetary Physics, School of Physics, University of Newcastle upon Tyne, England
S. Hofmann
Affiliation:
Department of Geophysics and Planetary Physics, School of Physics, University of Newcastle upon Tyne, England

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The determination of the heights of points on the lunar surface by Earth based astronomy using the geometrical librations, although individually of low accuracy, still provides our best method of obtaining the global shape of the Moon. The intrinsic scatter of the results arises from the effects of ‘seeing’ and simple statistical analysis is required to derive valid conclusions about the shape. Baldwin's method of fitting ellipsoidal surfaces to the points on the maria and uplands, separately by the method of least squares proves to be a valuable tool.

Analyses of the ACIC points and of the Pic du Midi studies of G. A. Mills show that good first descriptions of the global shape of the Moon for both the maria and uplands are triaxial ellipsoids with their long axes within 10° of the Earth direction, the major axis of the maria being about 1.3 km smaller than that of the uplands. Of particular significance is that the ellipticity of these surfaces is about 2½ times greater than the dynamical ellipticity; thus the non-hydrostatic figure of the Moon is not simply the result of distortion from a uniform Moon during its early history. The angular variation in density within the Moon cannot be simply a phenomena within the crust but must extend to a great depth. Convection could provide an explanation.

The departures of the lunar surface from the idealised ellipsoids are also of interest. The circular maria are systematically depressed relative to the maria ellipsoid: can the mascons have adjusted isostatically since their formation? Systematic differences in height between the western and eastern southern uplands are also noted.

Type
Part II: Scientific Papers
Information
Symposium - International Astronomical Union , Volume 47: The Moon , 1972 , pp. 22 - 31
Copyright
Copyright © Reidel 1972 

References

Baldwin, R. B.: 1949, The Face of the Moon, Chicago University Press.Google Scholar
Baldwin, R. B.: 1963, The Measure of the Moon, Chicago University Press.Google Scholar
Goudas, C. L.: 1963, Icarus 2, 423.CrossRefGoogle Scholar
Kopal, Z.: 1967, Proc. Roy. Soc. London 296, 254.Google Scholar
Mills, G. A.: 1968, Icarus 8, 90.CrossRefGoogle Scholar
Runcorn, S. K.: 1962, Nature, 195, 1150.CrossRefGoogle Scholar
Runcorn, S. K.: 1967, Proc. Roy. Soc. London A296, 270.Google Scholar
Runcorn, S. K. and Gray, B. M.: 1967, in Mantles of the Earth and Terrestrial Planets, John Wiley, New York.Google Scholar
Runcorn, S. K. and Shrubsall, M. H.: 1968, Phys. Earth Planet. Interiors 1, 317.CrossRefGoogle Scholar