# Clairaut's theorem

Not to be confused with Clairaut's relation.
For the theorem concerning symmetry of second derivatives of a mapping $f \colon \mathbb{R}^n \to \mathbb{R}$, see Symmetry of second derivatives.
Figure 1: An ellipsoid
Figure 2: Wireframe rendering of an ellipsoid (oblate spheroid)

Clairaut's theorem is a general mathematical law applying to spheroids of revolution. Published in 1743 by Alexis Claude Clairaut in his Théorie de la figure de la terre, tirée des principes de l'hydrostatique,[1] which synthesized physical and geodetic evidence that the Earth is an oblate rotational ellipsoid,[2][3] it was initially used to relate the gravity at any point on the Earth's surface to the position of that point, allowing the ellipticity of the Earth to be calculated from measurements of gravity at different latitudes.

## Formula

Clairaut's formula for the acceleration due to gravity g on the surface of a spheroid at latitude φ, was:[4][5]

$g(\varphi) = \mathbb{G}_e \left[ 1 + \left(\frac{5}{2} m - f\right) \sin^2 \varphi \right] \ ,$

where $\mathbb{G}_e$ is the value of the acceleration of gravity at the equator, m the ratio of the centrifugal force to gravity at the equator, and f the flattening of a meridian section of the earth, defined as:

$f = \frac {a-b}{a} \ ,$

(where a = semimajor axis, b = semiminor axis).

Clairaut derived the formula under the assumption that the body was composed of concentric coaxial spheroidal layers of constant density.[6] This work was subsequently pursued by Laplace, who relaxed the initial assumption that surfaces of equal density were spheroids.[7] Stokes showed in 1849 that the theorem applied to any law of density so long as the external surface is a spheroid of equilibrium.[8][9] A history of the subject, and more detailed equations for g can be found in Khan.[10]

### Somigliana equation

The above expression for g has been supplanted by the Somigliana equation (after Carlo Somigliana):

$g(\varphi) = G_e \left[ \frac{1+k\sin^2 \varphi}{\sqrt{1-e^2 \sin^2 \varphi }} \right],\,\!$

where,

• $e^2=\frac{a^2-b^2}{a^2}$ is the spheroid's eccentricity, squared;
• $\mathbb{G}_e,\mathbb{G}_p$ is the defined gravity at the equator and poles, respectively;
• $k=\frac{b\mathbb{G}_p-a\mathbb{G}_e}{a\mathbb{G}_e}$ (formula constant);

For Earth, $\mathbb{G}_e$ = 9.7803253359 ms−2; $\mathbb{G}_p$ = 9.8321849378 ms−2; k = 0.00193185265241 ; e2 = 0.00669437999013:[11] [12]

$g(\varphi)=9.7803253359\left[\frac{1+0.00193185265241\sin^2\varphi}{\sqrt{1-0.00669437999013\sin^2\varphi}}\right] \,\mathrm{ms}^{-2}.$

## Geodesy

The spheroidal shape of the Earth is the result of the interplay between gravity and centrifugal force caused by the Earth's rotation about its axis.[13][14] In his Principia, Newton proposed the equilibrium shape of a homogeneous rotating Earth was a rotational ellipsoid with a flattening f given by 1/230.[15][16] As a result gravity increases from the equator to the poles. By applying Clairaut's theorem, Laplace was able to deduce from 15 gravity values that f = 1/330. A modern estimate is 1/298.25642.[17] See Figure of the Earth for more detail.

For a detailed account of the construction of the reference Earth model of geodesy, see Chatfield.[18]

## References

1. ^ From the catalogue of the scientific books in the library of the Royal Society.
2. ^ Wolfgang Torge (2001). Geodesy: An Introduction (3rd ed.). Walter de Gruyter. p. 10. ISBN 3-11-017072-8.
3. ^ Edward John Routh (2001). A Treatise on Analytical Statics with Numerous Examples. Vol. 2. Adamant Media Corporation. p. 154. ISBN 1-4021-7320-2. A reprint of the original work published in 1908 by Cambridge University Press.
4. ^ W. W. Rouse Ball A Short Account of the History of Mathematics (4th edition, 1908)
5. ^ Walter William Rouse Ball (1901). A short account of the history of mathematics (3rd ed.). Macmillan. p. 384.
6. ^ Poynting, John Henry; Joseph John Thompson (1907). A Textbook of Physics, 4th Ed. London: Charles Griffin & Co. pp. 22–23.
7. ^ Isaac Todhunter. A History of the Mathematical Theories of Attraction and the Figure of the Earth from the Time of Newton to that of Laplace. Vol. 2. Elibron Classics. ISBN 1-4021-1717-5. Reprint of the original edition of 1873 published by Macmillan and Co.
8. ^ Osmond Fisher (1889). Physics of the Earth's Crust. Macmillan and Co. p. 27.
9. ^ John Henry Poynting & Joseph John Thomson (1907). A Textbook of Physics. C. Griffin. p. 22.
10. ^ NASA case file On the equilibrium figure of the earth by Mohammad A. Khan (1968)
11. ^ Department of Defense World Geodetic System 1984 ― Its Definition and Relationships with Local Geodetic Systems,NIMA TR8350.2, 3rd ed., Tbl. 3.4, Eq. 4-1
12. ^ Eq. 2.57 in MIT Essentials of Geophysics OpenCourseWare notes
13. ^ John P. Vinti, Gim J. Der, Nino L. Bonavito (1998). Orbital and Celestial Mechanics. Progress in astronautics and aeronautics, v. 177. American Institute of Aeronautics and Astronautics. p. 171. ISBN 1-56347-256-2.
14. ^ Arthur Gordon Webster (1904). The Dynamics of Particles and of Rigid, Elastic, and Fluid Bodies: being lectures on mathematical physics. B.G. Teubner. p. 468.
15. ^ Isaac Newton: Principia Book III Proposition XIX Problem III, p. 407 in Andrew Motte translation.
16. ^ See the Principia on line at Andrew Motte Translation
17. ^
18. ^ Averil B. Chatfield (1997). Fundamentals of High Accuracy Inertial Navigation. Volume 174 in Progress in Astronautics and Aeronautics. American Institute of Aeronautics and Astronautics. Chapter 1, Part VIII p. 7. ISBN 1-56347-243-0.