General Relativity is the common name for the theory of gravitation published by Albert Einstein in 1915. According to general relativity the force of gravity is a manifestation of the local geometry of spacetime. Although the modern theory is due to Einstein, its origins go back to the axioms of Euclidean geometry and the many attempts over the centuries to prove Euclid's fifth postulate, that parallel lines remain always equidistant, culminating with the realisation by Bolyai and Gauss that this axiom need not be true. The general mathematics of nonEuclidean geometries was developed by Gauss' student, Riemann, but these were thought to be wholly inapplicable to the real world until Einstein had developed his theory of relativity.
The special theory of relativity (1905) modified the equations used in comparing the measurements made by differently moving bodies, in view of the constant value of the speed of light: this had the consequence that physics could no longer treat space and time separately, but only as a single fourdimensional system, "spacetime," which was divided into "timelike" and "spacelike" directions differently depending on the observer's motion. The general theory added to this that the presence of matter "warped" the local spacetime environment, so that apparently "straight" lines through space and time have the properties we think of "curved" lines as having.
On May 29, 1919 observations by Arthur Eddington of shifted star positions during a solar eclipse confirmed the theory.
Foundations of Relativity and Special Relativity
This section outlines the major experimental results and mathematical advances that led to the formulation of General Relativity, and also sketches the more limited Special Theory of Relativity.
Gauss had realised that there is no prior reason that the geometry of space should be Euclidean. What this means is that if a physicist holds up a stick, and a cartographer stands some distance away and measures its length by a triangulation technique based on Euclidean geometry, then he is not guaranteed to get the same answer as if the physicist brings the stick to him and he measures its length directly. Of course for a stick he could not in practice measure the difference between the two measurements, but there are equivalent measurements which do detect the nonEuclidean geometry of spacetime directly; for example the PoundRebka experiment (1959) detected the change in wavelength of light from a cobalt source rising 22.5 meters against gravity in a shaft in the Jefferson Physical Laboratory at Harvard, and the rate of atomic clocks in GPS satellites orbiting the Earth has to be corrected for the effect of gravity.
Newton's theory of gravity had assumed that objects did in fact have absolute velocities: that some things really were at rest while others really were in motion. He realized, and made clear, that there was no way these absolutes could be measured. All the measurements one can make provide only velocities relative to one's own velocity (positions relative to one's own position, and so forth), and all the laws of mechanics would appear to operate identically no matter how one was moving. Newton believed, however, that the theory could not be made sense of without presupposing that there are absolute values, even if they cannot be determined. In fact, Newtonian mechanics can be made to work without this assumption: the outcome is rather innocuous, and should not be confused with Einstein's relativity which further requires the constancy of the speed of light.
In the nineteenth century Maxwell formulated a set of equationsMaxwell's field equationsthat demonstrated that light should behave as a wave emitted by electromagnetic fields which would travel at a fixed velocity through space. This appeared to provide a way around Newton's relativity: by comparing one's own speed with the speed of light in one's vicinity, one should be able to measure one's absolute speedor, what is practically the same, one's speed relative to a frame of reference that would be the same for all observers.
The assumption was whatever medium light was travelling throughwhatever it was waves ofcould be treated as a background against which to make other measurements. This inspired a search to determine the earth's velocity through this cosmic backdrop or "ether"the "ether drift." The speed of light measured from the surface of the earth should appear to be greater when the earth was moving against the ether, slower when they were moving in the same direction. (Since the earth was hurtling through space and spinning, there should be at least some regularly changing mesurements here.) A test made by Michelson and Morley toward the end of the century had the astonishing result that the speed of light appeared to be the same in every direction.
(To get a sense of how strange this was, imagine a car is driving down the highway. You want to see how fast it is going, so you and a bunch of friends get in cars and drive after it at different speeds. You talk on cell phones and each keep an eye on your speedometer and the other car. Some of you will get closer to the other car; some will fall further behind. When one of your friendsBillnotices that he is neither gaining nor losing distance on the other car, you can judge that the strange car's speed is the same as Bill's. Michelson and Morley's result would be like you and all of your friends discovering that you are each neither gaining nor losing time on the strange car, even though you are all going different speeds.)
Einstein synthesized these various results in his 1905 paper "On the Electrodynamics of Moving Bodies."
The fundamental idea in relativity is that we cannot talk of the physical quantities of velocity or acceleration without first defining a reference frame, and that a reference frame is defined by choosing particular matter as the basis for its definition. Thus all motion is defined and quantified relative to other matter. In the special theory of relativity it is assumed that reference frames can be extended indefinitely in all directions in space and time. The theory of special relativity concerns itself with inertial (nonaccelerating) frames while general relativity deals with all frames of reference. In the general theory it is recognised that we can only define local frames to given accuracy for finite time periods and finite regions of space (similarly we can draw flat maps of regions of the surface of the earth but we cannot extend them to cover the whole surface without distortion). In general relativity Newton's laws are assumed to hold in local reference frames. In particular free particles travel in straight lines in local inertial (Lorentz) frames. When these lines are extended they do not appear straight, and are known as geodesics. Thus Newton's first law is replaced by the law of geodesic motion.
We distinguish inertial reference frames, in which bodies maintain a uniform state of motion unless acted upon by another body, from noninertial frames in which freely moving bodies have an acceleration deriving from the reference frame itself. In noninertial frames there is a perceived force which is accounted for by the acceleration of the frame, not by the direct influence of other matter. Thus we feel gforces when cornering on the roads when we use a car as the physical base of our reference frame. Similarly there are coriolis and centrifugal forces when we define reference frames based on rotating matter (such as the Earth or a child's roundabout). The principle of equivalence in general relativity states that there is no local experiment to distinguish nonrotating free fall in a gravitational field from uniform motion in the absence of a gravitational field. In short there is no gravity in a reference frame in free fall. From this perspective the observed gravity at the surface of the Earth is the force observed in a reference frame defined from matter at the surface which is not free, but is acted on from below by the matter within the Earth, and is analogous to the gforces felt in a car.
Mathematically, Einstein models spacetime by a fourdimensional pseudoRiemannian manifold, and his field equation states that the manifold's curvature at a point is directly related to the stress energy tensor at that point; the latter tensor being a measure of the density of matter and energy. Curvature tells matter how to move, and matter tells space how to curve. The field equation is not uniquely proven, and there is room for other models, provided that they do not contradict observation. General relativity is distinguished from other theories of gravity by the simplicity of the coupling between matter and curvature, although we still await the unification of general relativity and quantum mechanics and the replacement of the field equation with a deeper quantum law. Few physicists doubt that such a theory of everything will give general relativity in the appropriate limit, just as general relativity predicts Newton's law of gravity in the nonrelativistic limit.
Einstein's field equation contains a parameter called the "cosmological constant" <math>\Lambda</math> which was originally introduced by Einstein to allow for a static universe (ie one that is not expanding or contracting). This effort was unsuccessful for two reasons: the static universe described by this theory was unstable, and observations by Hubble a decade later confirmed that our universe is in fact not static but expanding. So Λ was abandoned, but quite recently, improved astronomical techniques have found that a nonzero value of Λ is needed to explain some observations.
The field equation reads as follows:
where <math>R_{ik}</math> is the Ricci curvature tensor[?], <math>R</math> is the Ricci curvature scalar[?], <math>g_{ik}</math> is the metric tensor, <math>\Lambda</math> is the cosmological constant, <math>T_{ik}</math> is the stressenergy tensor, <math>\pi</math> is pi, <math>c</math> is the speed of light and <math>G</math> is the gravitational constant which also occurs in Newton's law of gravity. <math>g_{ik}</math> describes the metric of the manifold and is a symmetric 4 x 4 tensor, so it has 10 independent components. Given the freedom of choice of the four spacetime coordinates, the independent equations reduce to 6.
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