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C. W. F. Everitt led the Gravity Probe B experiment, which tested general relativity using four cryogenic gyroscopes in Earth orbit. The instrument measured slow changes in spin-axis direction relative to a stellar reference, separating the geodetic effect from frame dragging.

The 2011 final-results paper reported a geodetic drift of $-6601.8\pm 18.3$ milliarcseconds per year and a frame dragging drift of $-37.2\pm 7.2$ milliarcseconds per year, compatible with the predicted values within the reported uncertainties. The latter effect was much smaller, illustrating why identifying and modelling instrument drifts was central to the test.^[ref]

Frame dragging is the influence of mass-energy currents, especially rotation, on local inertial directions in general relativity. In a stationary axisymmetric metric tensor, an observer with zero angular momentum has coordinate angular velocity $\omega =-g_{t\varphi }/g_{\varphi \varphi }$ when the other spatial coordinates are held fixed. Around a rotating source this can be nonzero even without an applied azimuthal torque.

Gravity Probe B tested the effect with four cryogenic gyroscopes in Earth orbit, comparing their spin directions with a guide-star reference. Its analysis separated the much larger geodetic precession from the smaller rotation-dependent drift. This tests a change of inertial orientation, rather than ordinary frictional dragging of the spacecraft.^[ref]

Gravity Probe B was a space experiment that measured the slow drift of orbiting gyroscope axes relative to a distant guide star to test general relativity. It targeted geodetic precession from motion through curved spacetime and frame dragging associated with Earth's rotation.

The apparatus used four nearly spherical gyroscopes operating at cryogenic temperature, a telescope tracking the guide star and superconducting magnetic readout of spin orientation. Drag-free spacecraft control reduced unwanted forces. A crucial challenge was separating the tiny relativistic drift from classical torques, including electrostatic surface-patch effects and changing gyroscope orientation.^[ref]

The 2011 final analysis reported drift components $-6601.8\pm 18.3$ and $-37.2\pm 7.2$ milliarcseconds per year, compared with predicted geodetic and frame-dragging values $-6606.1$ and $-39.2$. The signs depend on the stated sky-coordinate convention. Dividing uncertainty by the measured magnitude shows why the experiment tested the much larger geodetic effect more precisely than the smaller frame-dragging effect.^[ref]

James M. Bardeen developed methods for interpreting motion near rotating black holes. His 1972 paper with William H. Press and Saul Teukolsky introduced a practical local-frame treatment for particle orbits and radiation in the Kerr metric.

Locally nonrotating observers provide an orthonormal frame tied to the rotating geometry. Expressing measurable quantities in that frame clarifies which effects reflect local motion and which involve frame dragging.^[ref]

Saul Teukolsky studied particle orbits and radiation near rotating black holes with James M. Bardeen and William H. Press. Their 1972 work used locally nonrotating orthonormal frames to express physical measurements in the Kerr metric.

This separates locally measured particle speeds from coordinate behavior affected by frame dragging. The paper applied the method to energy extraction and radiation, testing whether a formally allowed process could operate on physically reasonable orbits.^[ref]

Far from an isolated body of mass $M$ and angular momentum $\mathbf{J}$, a weak-field, leading-spin metric can be written in approximately Cartesian spatial coordinates asHere $r=|\mathbf{x}|$, the metric signature is $(-,+,+,+)$, and the retained terms are linear in $GM/(c^{2}r)$ and $GJ/(c^3{r}^2)$. Higher multipole moments and higher-order products are omitted.

For $\mathbf{J}=J\hat{\mathbf{z}}$, the mixed term is $4GJ(ydx-xdy)dt/(c^2{r}^3)$. Equivalently, it is $-4GJ{\sin }^2\theta dtd\phi /(c^{2}r)$. This agrees with the large-radius, leading-spin term of Kerr spacetime. The scalar part also depends on the chosen radial coordinate: the Cartesian form above uses the weak-field isotropic convention.^[ref]

The time-space metric components encode frame dragging, including Lense-Thirring precession. They represent an effect of moving matter that is absent from a description using only a scalar Newtonian gravitational potential.