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A representation of the geodetic effect.
General relativity
G_{\mu \nu} + \Lambda g_{\mu \nu}= {8\pi G\over c^4} T_{\mu \nu}
Einstein field equations
Mathematical formulation
Kepler problem · Lenses · Waves
Frame-dragging · Geodetic effect
Event horizon · Singularity
Black hole

The geodetic effect (also known as geodetic precession, de Sitter precession or de Sitter effect) represents the effect of the curvature of spacetime, predicted by general relativity, on a vector carried along with an orbiting body. For example, the vector could be the angular momentum of a gyroscope orbiting the earth, as carried out by the Gravity Probe B experiment. The geodetic effect was first predicted by Willem de Sitter in 1916, who provided relativistic corrections to the Earth-Moon system's motion. De Sitter's work was extended in 1918 by Jan Schouten and in 1920 by Adriaan Fokker.[1]

It can also be applied to a particular secular precession of astronomical orbits, equivalent to the rotation of the Laplace-Runge-Lenz vector.[2]

The term geodetic effect has two slightly different meanings as the moving body may be spinning or non-spinning. Non-spinning bodies move in geodesics, whereas spinning bodies move in slightly different orbits.[3]

The difference between de Sitter precession and Lense-Thirring precession (frame dragging) is that the de Sitter effect is due simply to the presence of a central mass, whereas Lense-Thirring precession is due to the rotation of the central mass. The total precession is calculated by combining the de Sitter precession with the Lense-Thirring precession.

de Sitter precession consists of the kinematic effect called Thomas precession combined with a geometric effect caused by gravitationally curved spacetime.[4]


Experimental confirmation

The geodetic effect was verified to a precision of better than 0.5% percent by Gravity Probe B, an experiment which measures the tilting of the spin axis of gyroscopes in orbit about the Earth.[5]The first results were announced in April 14, 2007 at the meeting of the American Physical Society.[6]


To derive the precession, assume the system is in a rotating Schwarzschild metric. The nonrotating metric is

\boldsymbol{ds}^{2} = (1-\frac{2m}{r})dt^{2} - (1 - \frac{2m}{r})^{-1}dr^{2} - r^{2}(d\theta^{2} + \sin^{2}\theta d\phi'^{2}) ,

where c = 1.

We introduce a rotating coordinate system, with an angular velocity ω, such that a satellite in a circular orbit in the θ=π/2 plane remains at rest. This gives us

d\phi = d\phi' - \omega dt \frac{}{}.

In this coordinate system, an observer at radial position r sees a vector positioned at r as rotating with angular frequency ω. This observer, however, sees a vector positioned at some other value of r as rotating at a different rate, due to relativistic time dilation. Transforming the Schwarzschild metric into the rotating frame, and assuming that θ is a constant, we find

 \boldsymbol{ds}^{2} = (1-\frac{2m}{r}-r^{2}\beta\omega^{2})(dt-\frac{r^{2}\beta\omega}{1-\frac{2m}{r}-r^{2}\beta\omega^{2}}d\phi)^{2} - (1-\frac{2m}{r})^{-1}dr^{2} - \frac{r^{2}\beta - 2mr\beta}{1-\frac{2m}{r}-r^{2}\beta\omega^{2}}d\phi^{2}

with β = sin(θ)2. For a body orbiting in the θ=π/2 plane, we will have β=1, and the body's world-line will maintain constant spatial coordinates for all time. Now, the metric is in the canonical form

\boldsymbol{ds}^{2} = e^{2\Phi}\left(dt - w_{i} dx^{i}\right)^{2} - k_{ij} dx^{i}dx^{j}.

From this canonical form, we can easily determine the rotational rate of a gyroscope

 \Omega = \frac{\sqrt{2}}{4}e^{\Phi}[k^{ik}k^{jl}(\omega_{i,j}-\omega_{j,i})(\omega_{k,l} - \omega_{l,k})]^{1/2} = -\sqrt{\beta}\omega.

We are at rest in our rotating coordinate system, so there is no acceleration, and thus Φ,i = 0. This leads to

 \Phi,_{i} = \frac{\frac{2m}{r^{2}} - 2r\beta\omega^{2}}{2(1-\frac{2m}{r}-r^{2}\beta\omega^{2})} = 0.

From this, we can distill ω,

 \omega^{2} = \frac{m}{r^{3}\beta}.

This is essentially Kepler's law of periods, which happens to be relativistically exact when expressed in terms of the time coordinate t of this particular rotating coordinate system. In the rotating frame, the satellite remains at rest, but an observer aboard the satellite sees the gyroscope's angular momentum vector precessing at the rate ω. This observer also sees the distant stars as rotating, but they rotate at a slightly different rate due to time dilation. Let τ be the gyroscope's proper time. Then

 \Delta \tau = (1-\frac{2m}{r}-r^{2}\beta\omega^{2})^{1/2}dt = (1-\frac{3m}{r})^{1/2}dt .

The -2m/r term is interpreted as the gravitational time dilation, while the additional -m/r is due to the rotation of this frame of reference. Let α' be the accumulated precession in the rotating frame. Since α' = ΩΔτ, the precession over the course of one orbit, relative to the distant stars, is given by:

 \alpha = \alpha' + 2\pi = -2 \pi \sqrt{\beta}\Bigg( (1-\frac{3m}{r})^{1/2} - 1 \Bigg).

With a first order Taylor series we find

 \alpha \approx \frac{3\pi m}{r}\sqrt{\beta} = \frac{3\pi m}{r}\sin(\theta).

See also


  1. ^ Jean Eisenstaedt, Anne J. Kox (1988). Studies in the History of General Relativity. Birkhäuser. p. 42. ISBN 0817634797.  
  2. ^ de Sitter, W (1916). "On Einstein's Theory of Gravitation and its Astronomical Consequences". Mon. Not. Roy. Astron. Soc. 77: 155–184.  
  3. ^ Rindler Page 254
  4. ^ Rindler, Page 234
  5. ^ Everitt, C.W.F.; Parkinson, B.W. (2009). "Gravity Probe B Science Results—NASA Final Report" (PDF). Retrieved 2009-05-02.  
  6. ^


  • Wolfgang Rindler (2006) Relativity: special, general, and cosmological (2nd Ed.), Oxford University Press, ISBN 9780198567318

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