## Abstract

Energy is dissipated in the Earth-Moon system at the. rate of 2.7 × 10
where

^{19}ergs/sec. We here consider the friction in the solid parts of the Earth and the Moon, first as a sink for tidal energy and secondly as a possible significant geophysical source of thermal energy. As a tidal sink this friction may account for that part of the energy dissipation which is not accounted for by the friction in the shallow seas. As a source of thermal energy, considerations of the work done by the Moon in varying its distance from the Earth give a limitation of roughly 8 × 10^{16}*Q*^{−1}ergs/sec on the amount of energy available. The specific dissipation function*Q*^{−1}is defined by Munk and MacDonald (1960, Sec. 4.3):$$\frac{1}{Q}~=~\frac{1}{2\pi E}~\oint{\frac{dE}{dt}}~dt$$

*E*is the peak energy stored in the system. This function is a dimensionless measure of the rate at which energy is dissipated in a vibrating system, and it does not depend on the detailed mechanisms of the dissipative process.## Keywords

Energy Dissipation Thermal Effect Tidal Effect Tidal Energy Deviatoric Strain
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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## References

- Alterman, Z., Jarosch, H., and Pekeris, C. L. (1959),
*Proc. Roy. Soc. (London) Ser*. A 252: 80Google Scholar - Gutenberg, B. (1959),
*The Physics of the Earth’s Interior*, Academic Press, New York and London.Google Scholar - Munk, W. H., and MacDonald, G. J. F. (1960),
*The Rotation of the Earth*, Cambridge University Press, London.Google Scholar

## Copyright information

© Plenum Press 1966