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The Arnowitt-Deser-Misner formalism expresses general relativity as constrained Hamiltonian evolution of a spatial metric and its conjugate momentum after a 3+1 decomposition of spacetime. Lapse and shift enforce the Hamiltonian and momentum constraints. For an asymptotically flat spacetime its boundary Hamiltonian gives the Arnowitt-Deser-Misner energy.

A physicist whose work connects special relativity, general relativity, Brownian motion and the photoelectric effect. He worked at the Institute for Advanced Study from 1933 until his death in 1955.^[ref]

In 1905, Albert Einstein used the photoelectric effect to explore quantized light, related Brownian motion to molecular agitation, formulated special relativity, and connected changes in mass and energy. These problems link visible measurements to otherwise inaccessible structure: emitted electron energies, suspended-particle displacements and comparisons of clocks.^[ref]

The Millikan photoelectric experiment follows one of those predictions into the laboratory. Its stopping-voltage measurements test a quantitative relation; the experiment's apparatus, surface preparation and electrical corrections matter to that inference. The Einstein field equations and general relativity lead to a different set of tests involving gravity and spacetime.

The Nobel Prize in Physics in 1921 recognized his theoretical work, particularly the law of the photoelectric effect; the award was presented in 1922.^[ref]

A physicist researching general relativity.^[ref]

Geometric or field data held fixed when a theory's dynamical degrees of freedom vary. The Minkowski metric is background structure in ordinary special relativity; the spacetime metric tensor is dynamical in general relativity. A fixed timelike vector field can introduce a preferred direction even when an equation is written using tensor notation.

A binary pulsar is a pulsar in a binary star: the companion's gravity changes the emitting neutron star's motion and hence its pulse arrival times. The companion need not itself be a detectable pulsar. Pulsar timing turns that motion into a measurable orbit, making the system useful for stellar mass determination and tests of general relativity.

Decreasing orbital period, distinct from spin slowdown. Joseph Hooton Taylor Jr. inferred masses using binary-pulsar periastron advance and binary-pulsar Einstein delay, then tested the independent period derivative against the general relativity quadrupole formula. Correcting differential Galactic acceleration gave indirect gravitational radiation evidence. This was not a terrestrial strain measurement.^[ref]

In particular, the raw measured derivative schematically containsHere $a_{\parallel }^{\mathrm{relative}}$ is positive when the source's recession accelerates. Its contribution follows by differentiating the leading Doppler effect. A decreasing observed orbital period alone therefore does not identify a unique energy-loss mechanism.

For fixed masses, binary orbital energy is $-G{m}_1{m}_2/(2a)$ and Kepler's third law gives $P_b\propto a^{3/2}$. Positive outgoing gravitational radiation predicted by the quadrupole formula makes the orbital energy more negative, reducing $a$ and $P_b$. This sign argument explains shrinking orbits, but a quantitative test also needs the predicted magnitude and orbital eccentricity dependence.

In four-dimensional asymptotically flat general relativity, a regular stationary vacuum black hole is a Kerr black hole under the standard connectedness and analyticity hypotheses. The electrovacuum extension is the Kerr--Newman family.

The Chandrasekhar mass is the limiting mass of a cold nonrotating white dwarf supported by relativistic electron degeneracy pressure, about $1.4M_{\odot }$ for ordinary composition. It bounds the retained remnant's mass, rather than the birth mass of a star that can lose an envelope. The ideal limit assumes fixed mean molecular weight per electron, Newtonian gravity and a noninteracting degenerate electron gas; electron capture, general relativity, stellar rotation and ignition can change the attainable endpoint.

The Chandrasekhar limit belongs to work of the early 1930s. In his 1983 retrospective, Subrahmanyan Chandrasekhar reprints the 1935 mass–radius sequence and then discusses stellar evolution and relativistic stability.^[ref] The 1983 Nobel Prize in Physics recognized his broader theoretical work on stellar structure and stellar evolution; the other half recognized William Alfred Fowler's theoretical and experimental work on nuclear reactions underlying chemical element formation.^[ref]

A congruence in general relativity is a family of curves through an open spacetime region such that each point lies on exactly one member. Its tangent field describes the family locally. A geodesic congruence is the special case in which every member is a geodesic.

Dark energy is a smooth component with sufficiently negative pressure to drive accelerated cosmic expansion. The supernova discovery of accelerating expansion measures an expansion history through luminosity distance; interpreting that history as a component of the stress tensor additionally assumes general relativity. A cosmological constant is one possibility, whereas dynamical dark energy permits a changing equation-of-state parameter.

A physicist researching general relativity.^[ref]

Einstein-Proca theory couples general relativity to a massive vector field governed by the Proca action. Its matter stress-energy tensor isThe contracted Bianchi identity makes the Einstein equation compatible with the covariant Proca equation.

If $D={\bigcap }_{i=1}^q\ker {\alpha }^i$ has constant rank, the Frobenius theorem says that $D$ is integrable exactly when its annihilator is closed under the exterior derivative: equivalently,This is also equivalent to involutivity of $D$.

For a nowhere-zero 1-form $\alpha$, the hyperplane distribution $\ker \alpha$ is tangent to hypersurfaces exactly when $\alpha \wedge d\alpha =0$. In general relativity this characterizes hypersurface-orthogonal vector fields and implies vanishing twist.

The ability to express a theory consistently under arbitrary changes of spacetime coordinates. A tensor equation has this property when all its fields, including any background structures, transform appropriately. It does not by itself say that every active transformation is a dynamical symmetry, or that no preferred background structure exists. General relativity has the additional substantive feature that its metric tensor is dynamical.

General relativity describes gravity through the geometry of spacetime. Its metric tensor specifies distances, proper time measured by clocks, and the causal structure that limits communication. Matter and radiation affect this geometry through the Einstein field equations; freely falling test particles follow geodesics of the resulting geometry. A planet's orbit and a falling apple therefore belong to the same geometric story. The Newtonian limit recovers familiar Newtonian gravity when fields are weak and speeds are small compared with the speed of light. See David Tong's introduction to general relativity.

The most direct way to understand spacetime curvature is to compare neighboring freely falling bodies. Even when each body feels weightless, their separation can change: this is geodesic deviation, observed as a tidal force. Curvature concerns these relative measurements, rather than the shape of a drawing in an imagined surrounding space. A second accessible measurement is gravitational time dilation: identical clocks maintained at different heights accumulate different proper times. Together, tides and clocks turn an abstract geometry into laboratory questions.

In Newtonian gravity, the gravitational field $\mathbf{g}$ specifies the acceleration of a freely falling test particle at each position. A gravitational potential $\Phi$ gives $\mathbf{g}=-\nabla \Phi$, with the gradient taken in the spatial geometry of the model. In general relativity, the metric tensor describes gravitational effects, and tidal forces are encoded by spacetime curvature.

Passive gravitational mass is the coefficient in $\mathbf{F}=m_{\mathrm{g}}\mathbf{g}$ for an imposed Newtonian gravitational field. Active gravitational mass instead measures a body's contribution to the source of that field in Newton's law of universal gravitation. Universality of the ratio of passive gravitational mass to inertial mass is the Newtonian content of the weak equivalence principle. In general relativity, the source is the full stress-energy tensor, rather than a single scalar gravitational mass.

A gravitational wave is a propagating disturbance of spacetime curvature produced by changing mass-energy multipole moments. In general relativity, its two transverse gravitational wave polarizations alternately stretch and squeeze freely falling separations. The leading radiation from a slowly moving source is governed by its mass quadrupole moment, rather than by its total mass alone.

The experimental breakthrough was GW150914: observed on 14 September 2015 and published on 11 February 2016. The LIGO Scientific Collaboration and Virgo Collaboration reported a merging pair of black holes, using the two LIGO detectors at Hanford and Livingston; Virgo was being upgraded and did not observe this event.^[ref]

The 2017 Nobel Prize in Physics recognized Rainer Weiss, Barry C. Barish and Kip S. Thorne for contributions to LIGO and gravitational wave observation. Rainer Weiss developed interferometric detection and its noise analysis; Barry C. Barish led the project into construction and operation; Kip S. Thorne developed its theoretical and astrophysical foundations. The experiment depended on a large collaboration.^[ref]

Gravity governs falling bodies and orbits. Newtonian gravity describes it through a gravitational field acting on masses; general relativity instead relates matter and radiation to the geometry of spacetime through the Einstein field equations.

A gyroscope is a rotating instrument whose rapidly spinning, nearly symmetric rotor provides a direction reference through its angular momentum. In an inertial frame, negligible external torque approximately preserves that direction by conservation of angular momentum. A transverse torque turns the angular momentum instead: the surprising sideways motion of a supported spinning wheel is precession. An ideal freely falling test gyroscope in general relativity has its spin undergo parallel transport along its timelike geodesic. Comparing that direction with distant reference axes measures Lense-Thirring precession; the direction need not remain fixed in arbitrary rotating coordinates.

A gyroscope direction reference is useful precisely because its direction can persist while its housing turns. A spinning-wheel precession experiment deliberately supplies gravitational torque to reveal how that persistence fails. The gyroscope vector geometry explains the direction, and slow steady gyroscope precession gives a numerical prediction with a check on its assumptions.