# User:Mpatel/sandbox/General relativity

General relativity (GR) [also called the general theory of relativity (GTR) and general relativity theory (GRT)] is the geometrical theory of gravitation published by Albert Einstein in 1915/16.[1][2] It unifies special relativity and Sir Isaac Newton's law of universal gravitation with the insight that gravitation is not due to a force but rather is a manifestation of curved space and time, with this curvature being produced by the mass-energy and momentum content of the space-time. General relativity is distinguished from other metric theories of gravitation by its use of the Einstein field equations to relate space-time content and space-time curvature.

General relativity is currently the most successful gravitational theory, being almost universally accepted and well supported by observations. The first success of general relativity was in explaining the anomalous perihelion precession of Mercury. Then in 1919, Sir Arthur Eddington announced that observations of stars near the eclipsed Sun confirmed general relativity's prediction that massive objects bend light. Since then, many other observations and experiments have confirmed many of the predictions of general relativity, including gravitational time dilation, the gravitational redshift of light, signal delay, and gravitational radiation. In addition, numerous observations are interpreted as confirming one of general relativity's most mysterious and exotic predictions, the existence of black holes.

In the mathematics of general relativity, the Einstein field equations become a set of simultaneous differential equations which are solved to produce metric tensors of space-time. These metric tensors describe the shape of the space-time, and are used to obtain the predictions of general relativity. The connections of the metric tensors specify the geodesic paths that objects follow when traveling inertially. Important solutions of the Einstein field equations include the Schwarzschild solution (for the space-time surrounding a spherically symmetric uncharged and non-rotating massive object), the Reissner-Nordström solution (for a charged spherically symmetric massive object), and the Kerr metric (for a rotating massive object).

In spite of its overwhelming success, there is discomfort with general relativity in the scientific community due to its being incompatible with quantum mechanics and the reachable singularities of black holes (at which the math of general relativity breaks down). Because of this, numerous other theories have been proposed as alternatives to general relativity. The most successful of these was Brans-Dicke theory, which appeared to have observational support in the 1960s. However, those observations have since been refuted and modern measurements indicate that any Brans-Dicke type of deviation from general relativity must be very small if it exists at all. {{#invoke: Sidebar | collapsible }}

## Overview

### Treatment of gravitation

Two-dimensional analogy of space-time distortion. The presence of matter changes the geometry of spacetime, this (curved) geometry being interpreted as gravity. Note that the white lines do not represent the curvature of space, but instead represent the coordinate system imposed on the curved spacetime which would be rectilinear in a flat spacetime

In this theory, spacetime is treated as a 4-dimensional Lorentzian manifold which is curved by the presence of mass, energy and momentum (or stress-energy) within it. The relationship between stress-energy and the curvature of spacetime is described by the Einstein field equations. The motion of objects being influenced solely by the geometry of spacetime (inertial motion) occurs along special paths called timelike and null geodesics of spacetime.

One of the defining features of general relativity is the idea that gravitational 'force' is replaced by geometry. In general relativity, phenomena that in classical mechanics are ascribed to the action of the force of gravity (such as free-fall, orbital motion, and spacecraft trajectories) are taken in general relativity to represent inertial motion in a curved spacetime. So what people standing on the surface of the Earth perceive as the 'force of gravity' is a result of their undergoing a continuous physical acceleration caused by the mechanical resistance of the surface on which they are standing.

### Justification

The justification for creating general relativity came from the equivalence principle[3], which dictates that free-falling observers are the ones in inertial motion. A consequence of this insight is that inertial observers can accelerate with respect to each other (Think of two balls falling on opposite sides of the Earth, for example). This redefinition is incompatible with Newton's first law of motion, and cannot be accounted for in the Euclidean geometry of special relativity. To quote Einstein himself:

"If all accelerated systems are equivalent, then Euclidean geometry cannot hold in all of them." [4]

Thus the equivalence principle led Einstein to search for a gravitational theory which involves curved space-times.

Another motivating factor was the realization that relativity calls for the gravitational potential to be expressed as a symmetric rank-two tensor, and not just a scalar as was the case in Newtonian physics (An analogy is the electromagnetic four-potential of special relativity). Thus, Einstein sought a rank-two tensor means of describing curved space-times surrounding massive objects.[5] This effort came to fruition with the discovery of the Einstein field equations in 1915.[1]

### Fundamental principles

General relativity is based on the following set of fundamental principles which guided its development.[2][6] These principles are:

(The equivalence principle, which was the starting point for the development of general relativity, ended up being a consequence of the general principle of relativity and the principle that inertial motion is geodesic motion).

### Spacetime as a curved Lorentzian manifold

In general relativity, the spacetime concept introduced by Hermann Minkowski for special relativity is modified. More specifically, general relativity stipulates that spacetime is:

The curvature of spacetime (caused by the presence of stress-energy) can be viewed intuitively in the following way. Placing a heavy object such as a bowling ball on a trampoline will produce a 'dent' in the trampoline. This is analogous to a large mass such as the Earth causing the local spacetime geometry to curve. This is represented by the image at the top of this article. The larger the mass, the bigger the amount of curvature. A relatively light object placed in the vicinity of the 'dent', such as a ping-pong ball, will accelerate towards the bowling ball in a manner governed by the 'dent'. Firing the ping-pong ball at just the right speed towards the 'dent' will result in the ping-pong ball 'orbiting' the bowling ball. This is analogous to the Moon orbiting the Earth, for example.

Similarly, in general relativity massive objects do not directly impart a force on other massive objects as hypothesized in Newton's action at a distance idea. Instead (in a manner analogous to the ping-pong ball's response to the bowling ball's dent rather than the bowling ball itself), other massive objects respond to how the first massive object curves spacetime.

### The mathematics of general relativity

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Due to the expectation that spacetime is curved, Riemannian geometry (a type of non-Euclidean geometry) must be used. In essence, spacetime does not adhere to the "common sense" rules of Euclidean geometry, but instead objects that were initially traveling in parallel paths through spacetime (meaning that their velocities do not differ to first order in their separation) come to travel in a non-parallel fashion. This effect is called geodesic deviation, and it is used in general relativity as an alternative to gravity. For example, two people on the Earth heading due north from different positions on the equator are initially traveling on parallel paths, yet at the north pole those paths will cross. Similarly, two balls initially at rest with respect to and above the surface of the Earth (which are parallel paths by virtue of being at rest with respect to each other) come to have a converging component of relative velocity as both accelerate towards the center of the Earth due to their subsequent free-fall (Another way of looking at this is how a single ball moving in a purely timelike fashion parallel to the center of the Earth comes through geodesic motion to be moving towards the center of the Earth).

The requirements of the mathematics of general relativity are further modified by the other principles. Local Lorentz Invariance requires that the manifolds described in GR be 4-dimensional and Lorentzian instead of Riemannian. In addition, the principle of general covariance forces that mathematics to be expressed using tensor calculus. Tensor calculus permits a manifold as mapped with a coordinate system to be equipped with a metric tensor of spacetime which describes the incremental (spacetime) intervals between coordinates from which both the geodesic equations of motion and the curvature tensor of the spacetime can be ascertained.

### The Einstein field equations

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The Einstein field equations (EFE) describe how stress-energy causes curvature of spacetime and are usually written in tensor form (using abstract index notation) as

${\displaystyle G_{ab}=\kappa \,T_{ab}}$

where Gab is the Einstein tensor, Tab is the stress-energy tensor and ${\displaystyle \kappa }$ is a constant. The tensors Gab and Tab are both rank 2 symmetric tensors, that is, they can each be thought of as 4×4 matrices, each of which contains 10 independent terms.

The EFE reduce to Newton's law of gravity in the limiting cases of a weak gravitational field and slow speed relative to the speed of light. In fact, the value of ${\displaystyle \kappa }$ in the EFE is determined to be ${\displaystyle \kappa =8\pi G/c^{4}\ }$ by making these two approximations.[2]

Einstein introduced an alternative form of the field equations to accommodate a static universe solution in his theory:Template:Fact

${\displaystyle G_{ab}+\Lambda \ g_{ab}=\kappa \,T_{ab}}$

The solutions of the EFE are metrics of spacetime. These metrics describe the structure of spacetime given the stress-energy and coordinate mapping used to obtain that solution. Being non-linear differential equations, the EFE often defy attempts to obtain an exact solution; however, many such solutions are known.

The EFE are the identifying feature of general relativity. Other theories built out of the same premises include additional rules and/or constraints. The result almost invariably is a theory with different field equations (such as Brans-Dicke theory, teleparallelism, Rosen's bimetric theory, and Einstein-Cartan theory).

### Coordinate vs. physical acceleration

One of the greatest sources of confusion about general relativity comes from the need to distinguish between coordinate and physical accelerations.

In classical mechanics, space is preferentially mapped with a Cartesian coordinate system. Inertial motion then occurs as one moves through this space at a constant coordinate rate with respect to time. Any change in this rate of progression must be due to a force, and therefore a physical and coordinate acceleration were in classical mechanics one and the same. It is important to note that in special relativity that same kind of Cartesian coordinate system was used, with time being added as a fourth dimension and defined for an observer using the Einstein synchronization procedure. As a result, physical and coordinate acceleration correspond in special relativity too, although their magnitudes may vary.

In general relativity, the elegance of a flat spacetime and the ability to use a preferred coordinate system are lost (due to stress-energy curving spacetime and the principle of general covariance). Consequently, coordinate and physical accelerations become sundered. For example: Try using a polar coordinate system in classical mechanics. In this case, an inertially moving object which passes by (instead of through) the origin point is found to first be moving mostly inwards, then to be moving tangentially with respect to the origin, and finally to be moving outwards, and yet it is moving in a straight line. This is an example of an inertially moving object undergoing a coordinate acceleration, and the way this coordinate acceleration changes as the object travels is given by the geodesic equations for the manifold and coordinate system in use.

Another more direct example is the case of someone standing on the Earth, where they are at rest with respect to the surface coordinates for the Earth (latitude, longitude, and elevation) but are undergoing a continuous physical acceleration because the mechanical resistance of the Earth's surface keeps them from free-falling.

## Predictions of general relativity

(For more detailed information about tests and predictions of general relativity, see tests of general relativity).

### Gravitational effects

#### Acceleration effects

The acceleration effects are common to all accelerated frames of reference, and were described by Einstein as far back as 1907[3]. As such, they are present even in special relativity.

The first of these effects is the Gravitational redshifting of light. Under this effect, the frequency of light will decrease (shifting visible light towards the red end of the spectrum) as it moves to higher gravitational potentials (out of a gravity well). This is caused by an observer at a higher gravitational potential being accelerated (with respect to the local inertial frames of reference) away from the source of a beam of light as that light is moving towards that observer. Gravitational redshifting has been confirmed by the Pound-Rebka experiment.[7][8][9]

A related effect is gravitational time dilation, under which clocks will run slower at lower gravitational potentials (deeper within a gravity well). It is another way of perceiving that decrease in frequency of the gravitationally redshifted light. This effect has been directly confirmed by the Hafele-Keating experiment[10][11] and GPS.

Gravitational time dilation has as a consequence another effect called the Shapiro effect (also known as gravitational time delay). Shapiro delay occurs when signals take longer to move through a gravitational field than they would in the absence of the gravitational field. This effect was discovered through the observations of signals from spacecraft and pulsars passing behind the Sun as seen from the Earth.[12][13]

#### Bending of light

The most famous early test of the general theory of relativity was made possible by observation of the 1919 solar eclipse. According to Sir Arthur Stanley Eddington, starlight could be seen to bend around the sun as it made its way to the observer on earth.

This bending also occurs in any accelerated frame of reference. However, the details of the bending and therefore the gravitational lensing effects are governed by space-time curvature.

Einstein was aware of this effect by 1911, but at the time he calculated an amount for the bending that was the same as predicted by classical mechanics given that light is accelerated by gravitation. In 1916, Einstein found that the amount of the bending in general relativity was actually twice the Newtonian value[2], and so this became a way of testing general relativity. Since then, this prediction has been confirmed by astronomical observations during eclipses of the Sun and observations of pulsars passing behind the Sun[14].

Gravitational lensing occurs when one distant object is in front of or close to being in front of another much more distant object. In that case, the bending of light by the nearer object can change how the more distant object is seen. The first example of gravitational lensing was the discovery of a case of two nearly images of the same pulsar. Since then many other examples of distant galaxies and quasars being affected by gravitational lensing have been found.

A special type of gravitational lensing occurs in Einstein rings and arcs. The Einstein ring is created when an object is directly behind another object with a uniform gravitational field. In that case, the light from the more distant object becomes a ring around the closer object. If the more distant object is slightly offset to one side and/or the gravitational field is not uniform, partial rings (called arcs) will appear instead.

Finally, in our own galaxy a star can appear to be brightened when compact massive foreground object is sufficiently aligned with it. In that case, the magnified and distorted images of the background star due to the gravitational bending of light cannot be resolved. This effect is called microlensing, and such events are now regularly observed.

#### Orbital effects

General relativity differs from classical mechanics in its predictions for orbiting bodies. The first difference is in the prediction that apsides of orbits will precess on their own. This is not called for by Newton's theory of gravity. Because of this, an early successful test of general relativity was its correctly predicting the anomalous perihelion precession of Mercury. More recently, perihelion precession has been confirmed in the large precessions observed in binary pulsar systems.

A related effect is geodetic precession. This is a precession of the poles of a spinning object due to the effects of parallel transport in a curved space-time. This effect is not expected in Newtonian gravity. The prediction of geodetic precession is being tested by Gravity Probe B.

Another effect is that of orbital decay due to the emission of gravitational radiation by a co-rotating system. It is observable in closely orbiting stars as an ongoing decrease in their orbital period. This effect has been observed in binary pulsar systems.

#### Frame Dragging

Frame dragging is where a rotating massive object "drags" space-time along with its rotation. In essence, an observer who is distant from a rotating massive object and at rest with respect to its center of mass will find that the fastest clocks at a given distance from the object are not those which are at rest (as is the case for a non-rotating massive object). Instead, the fastest clocks will be found to have component of motion around the rotating object in the direction of the rotation. Similarly, it will be found by the distant observer that light moves faster in the direction of the rotation of the object than against it. Frame dragging will also cause the orientation of a gyroscope to change over time. For a spacecraft in a polar orbit, the direction of this effect is perpendicular to the geodetic precession mentioned above. Gravity Probe B is using this feature to test both frame dragging and the geodetic precession predictions.

#### Black holes

Black holes are objects which have gravitationally collapsed behind an event horizon. A black hole is so massive that light cannot escape its gravitational pull. The disappearance of light and matter within a black hole may be thought of as their entering a region where all possible world lines point inwards. Stephen Hawking has predicted that black holes can "leak" mass,[15] a phenomenon called Hawking radiation, a quantum effect not in violation of general relativity. Numerous black hole candidates are known. These include the supermassive object associated with Sagittarius A* at the center of our galaxy[16].

### Cosmology

Although it was created as a theory of gravitation, it was soon realized that general relativity could be used to model the universe, as so gave birth to the field of physical cosmology. The central equations for physical cosmology are the Friedmann-Lemaître-Robertson-Walker metric, which are the cosmological solution of the Einstein field equations. This metric predicts that the universe must be dynamic: It must either be expanding, contracting, or switching between those states.

At the time of the discovery of the Friedmann-Lemaître-Robertson-Walker metric, Einstein could not abide by the idea of a dynamic universe. In an attempt to make general relativity accommodate a static universe, Einstein added a cosmological constant to the field equations as described above. However, the resultant static universe was unstable. Then in 1929 Edwin Hubble showed that the redshifting of light from distant galaxies indicates that they are receding from our own at a rate which is proportional to their distance from us.[17] [18]. This demonstrated that the universe is indeed expanding. Hubble's discovery ended Einstein's objections and his use of the cosmological constant.

The equations for an expanding universe become singular when one goes far enough back in time, and this primordial singularity marks the formation of the universe. That event has come to be called the Big Bang. In 1948, Ralph Asher Alpher and George Gamov published an article describing this event and predicting the existence of the cosmic microwave background radiation left over from the Big Bang. In 1965, Arno Penzias and Robert Wilson first observed the background radiation.[19], confirming the Big Bang theory.

Recently, observations of distant supernovae have indicated that the expansion of the universe is currently accelerating. This was unexpected since Friedmann-Lemaître-Robertson-Walker metric calls for a universe that only contains visible matter to have a decelerating expansion. However, for a universe that is 4% baryonic matter, 26% dark matter, and 70% dark energy, the Friedmann-Lemaître-Robertson-Walker metric takes on a form that is consistent with observation. There is also an irony in that the dark energy can be modeled using Einstein's cosmological constant, but with a value that enhances the dynamic nature of the universe instead of muting it {{ safesubst:#invoke:Unsubst||date=__DATE__ |$B= {{#invoke:Category handler|main}}{{#invoke:Category handler|main}}[citation needed] }}. ### Other predictions • The equivalence of inertial mass and gravitational mass: This follows naturally from free-fall being inertial motion. • Gravitational radiation: Orbiting objects and merging neutron stars and/or black holes are expected to emit gravitational radiation. • Orbital decay (described above). • Binary pulsar mergers: May create gravitational waves strong enough to be observed here on Earth. Several gravitational wave observatories are (or will soon be) in operation. However, there are no confirmed observations of gravitational radiation at this time. • Gravitons: According to quantum mechanics, gravitational radiation must be composed of quanta called gravitons. General relativity predicts that these will be massless spin-2 particles. They have not been observed. • Only quadrupole (and higher order multipole) moments create gravitational radiation. • Dipole gravitational radiation (prohibited by this prediction) is predicted by some alternative theories. It has not been observed. ## Relationship to other physical theories This section will use the Einstein summation convention. ### Classical mechanics and special relativity Classical mechanics and special relativity are lumped together here because special relativity is in many ways intermediate between general relativity and classical mechanics, and shares many attributes with classical mechanics. In the following discussion, the mathematics of general relativity is used heavily. Also, under the principle of minimal coupling, the physical equations of special relativity can be turned into their general relativity counterparts by replacing the Minkowski metric (ηab) with the relevant metric of spacetime (gab) and by replacing any partial derivatives with covariant derivatives. In the discussions that follow, the change of metrics is implied. #### Inertia Inertial motion is motion free of all forces. In Newtonian mechanics, the force F acting on a particle with mass m is given by Newton's second law, ${\displaystyle F=m{\ddot {r}}}$, where the acceleration is given by the second derivative of position r with respect to time t . Zero force means that inertial motion is just motion with zero acceleration: ${\displaystyle {\frac {{\mathrm {d} }^{2}r}{{\mathrm {d} }t^{2}}}=0}$ The idea is the same in special relativity. Using Cartesian coordinates, inertial motion is described mathematically as: ${\displaystyle {\frac {{\mathrm {d} }^{2}x^{a}}{{\mathrm {d} }\tau ^{2}}}=0}$ where xa is the position coordinate and τ is proper time. (In Newtonian mechanics, τ ≡ t, the coordinate time). In both Newtonian mechanics and special relativity, space and then spacetime are assumed to be flat, and we can construct a global Cartesian coordinate system. In general relativity, these restrictions on the shape of spacetime and on the coordinate system to be used are lost. Therefore a different definition of inertial motion is required. In relativity, inertial motion occurs along timelike or null geodesics as parameterized by proper time. This is expressed mathematically by the geodesic equation: ${\displaystyle {\frac {{\mathrm {d} }^{2}x^{a}}{{\mathrm {d} }\tau ^{2}}}+\Gamma _{bc}^{a}\,{\frac {{\mathrm {d} }x^{b}}{{\mathrm {d} }\tau }}\,{\frac {{\mathrm {d} }x^{c}}{{\mathrm {d} }\tau }}=0}$ where ${\displaystyle \Gamma _{bc}^{a}}$ is a Christoffel symbol. Since general relativity describes four-dimensional spacetime, this represents four equations, with each one describing the second derivative of a coordinate with respect to proper time. In the case of flat space in Cartesian coordinates, we have ${\displaystyle \Gamma _{bc}^{a}=0}$, so this equation reduces to the special relativity form. #### Gravitation For gravitation, the relationship between Newton's theory of gravity and general relativity is governed by the correspondence principle: General relativity must produce the same results as gravity does for the cases where Newtonian physics has been shown to be accurate. Around a spherically symmetric object, the Newtonian theory of gravity predicts that objects will be physically accelerated towards the center on the object by the rule ${\displaystyle {\mathbf {\ddot {r}} }=GM{\mathbf {\hat {r}} }/r^{2}}$ where G is Newton's Gravitational constant, M is the mass of the gravitating object, r is the distance to the gravitation object, and ${\displaystyle {\mathbf {\hat {r}} }}$ is a unit vector identifying the direction to the massive object. In the weak-field approximation of general relativity, an identical coordinate acceleration must exist. For the Schwarzschild solution (which is the simplest possible spacetime surrounding a massive object), the same acceleration as that which (in Newtonian physics) is created by gravity is obtained when a constant of integration is set equal to 2MG/c^2). For more information, see Deriving the Schwarzschild solution. #### Transition from Newtonian mechanics to general relativity {{#invoke:main|main}} Some of the basic concepts of general relativity can be outlined outside the relativistic domain. In particular, the idea that mass/energy generates curvature in space and that curvature affects the motion of masses can be illustrated in a Newtonian setting. General relativity generalizes the geodesic equation and the field equation to the relativistic realm in which trajectories in space are replaced with Fermi-Walker transport along world lines in spacetime. The equations are also generalized to more complicated curvatures. #### Transition from special relativity to general relativity {{#invoke:main|main}} The basic structure of general relativity, including the geodesic equation and Einstein field equation, can be obtained from special relativity by examining the kinetics and dynamics of a particle in a circular orbit about the earth. In terms of symmetry, the transition involves replacing global Lorentz covariance with local Lorentz covariance. #### Conservation of energy-momentum In classical mechanics, conservation laws for energy and momentum are handled separately in the two principles of conservation of energy and conservation of momentum. With the advent of special relativity, these two conservation principles were united through the concept of mass-energy equivalence. Mathematically, the general relativity statement of energy-momentum conservation is: ${\displaystyle {T_{a}}^{b}{}_{;b}={T_{a}}^{b}{}_{,b}+{\Gamma ^{b}}_{cb}\,{T_{a}}^{c}-{\Gamma ^{c}}_{ab}\,{T_{c}}^{b}=0}$ where ${\displaystyle {T_{a}}^{b}}$ is the stress-energy tensor, the comma indicates a partial derivative and the semicolon indicates a covariant derivative. The terms involving the Christoffel symbols are absent in the special relativity statement of energy-momentum conservation. Unlike classical mechanics and special relativity, it is not usually possible to unambiguously define the total energy and momentum in general relativity, so the tensorial conservation laws are local statements only (see ADM energy, though). This often causes confusion in time-dependent spacetimes which apparently do not conserve energy, although the local law is always satisfied. Exact formulation of energy-momentum conservation on an arbitrary geometry requires use of a non-unique stress-energy-momentum pseudotensor. ### Electromagnetism {{#invoke:main|main}} General relativity modifies the description of electromagnetic phenomena by employing a new version of Maxwell's equations. These differ from the special relativity form in that the Christoffel symbols make their presence in the equations via the covariant derivative. The source equations of electrodynamics in curved spacetime are (in cgs units) ${\displaystyle F^{\,ab}{}_{;b}={4\pi \over c}\,J^{\,a}}$ where Fab is the electromagnetic field tensor representing the electromagnetic field and Ja is a four-current representing the sources of the electromagnetic field. The source-free equations are the same as their special relativity counterparts. The effect of an electromagnetic field on a charged object is then modified to ${\displaystyle P^{\,a}{}_{\,;\tau }=(q/m)\,F^{\,ab}P_{b}}$, where q is the charge on the object, m is the rest mass of the object and P a is the four-momentum of the charged object. Maxwell's equations in flat spacetime are recovered in rectangular coordinates by reverting the covariant derivatives to partial derivatives. For Maxwell's equations in flat spacetime in curvilinear coordinates see [1] or [2] ### Quantum mechanics Quantum mechanics is viewed as a fundamental theory of physics along with general relativity, but combining the two theories has presented difficulties. #### Quantum field theory in curved spacetime {{#invoke:main|main}} Normally, quantum field theory models are considered in flat Minkowski space (or Euclidean space), which is an excellent approximation for weak gravitational fields like those on Earth. In the presence of strong gravitational fields, the principles of quantum field theory have to be modified. The spacetime is static so the theory is not fully relativistic in the sense of general relativity; it is neither background independent nor generally covariant under the diffeomorphism group. The interpretation of excitations of quantum fields as particles becomes frame dependent. Hawking radiation is a prediction of this semiclassical approximation. #### Einstein gravity is nonrenormalizable  How can the theory of quantum mechanics be merged with the theory of general relativity to produce a so-called "theory of everything"? It is often said that general relativity is incompatible with quantum mechanics. This means that if one attempts to treat the gravitational field using the ordinary rules of quantum field theory, one finds that physical quantities are divergent. Such divergences are common in quantum field theories, and can be cured by adding parameters to the theory known as counterterms. These counterterms are infinities which are equal in magnitude and opposite in sign to the divergent terms. When they are added, the infinities cancel, leaving only finite terms, but modifying the meaning of terms in the equation such as "mass" and "charge" {{ safesubst:#invoke:Unsubst||date=__DATE__ |$B= {{#invoke:Category handler|main}}{{#invoke:Category handler|main}}[citation needed] }}.

Many of the best understood quantum field theories, such as quantum electrodynamics, contain divergences which are canceled by counterterms that have been effectively measured. One needs to say effectively because the counterterms are formally infinite, however it suffices to measure observable quantities, such as physical particle masses and coupling constants, which depend on the counterterms in such a way that the various infinities cancel.

A problem arises, however, when the cancellation of all infinities requires the inclusion of an infinite number of counterterms. In this case the theory is said to be nonrenormalizable. While nonrenormalizable theories are sometimes seen as problematic, the framework of effective field theories presents a way to get low-energy predictions out of non-renormalizable theories. The result is a theory that works correctly at low energies, though such a theory cannot be considered to be a theory of everything because it cannot be self-consistently extended to the high-energy realm.

#### Proposed quantum gravity theories

General relativity fits nicely into the effective field theory formalism and makes sensible predictions at low energies (Donoghue, 1995). However, high enough energies will "break" the theory.

It is generally held that one of the most important unsolved problems in modern physics is the problem of obtaining the true quantum theory of gravitation, that is, the theory chosen by nature, one that will work at all energies. Discarded attempts at obtaining such theories include supergravity, a field theory which unifies general relativity with supersymmetry. In the second superstring revolution, supergravity has come back into fashion, with its quantum completion rebranded with a new name: M-theory.

A very different approach to that described above is employed by loop quantum gravity. In this approach, one does not try to quantize the gravitational field as one quantizes other fields in quantum field theories. Thus the theory is not plagued with divergences and one does not need counterterms. However it has not been demonstrated that the classical limit of loop quantum gravity does in fact contain flat space Einsteinian gravity. This being said, the universe has only one spacetime and it is not flat.

Of these two proposals, M-theory is significantly more ambitious in that it also attempts to incorporate the other known fundamental forces of Nature, whereas loop quantum gravity "merely" attempts to provide a viable quantum theory of gravitation with a well-defined classical limit which agrees with general relativity.

### Alternative theories

{{#invoke:main|main}} Well known classical theories of gravitation other than general relativity include:

• Nordström's theory of gravitation (1913) was one of the earliest metric theories (an aspect brought out by Einstein and Fokker in 1914). Nordström soon abandoned his theory in favor of general relativity on theoretical grounds, but this theory, which is a scalar theory, and which features a notion of prior geometry, does not predict any light bending, so it is solidly incompatible with observation.
• Alfred North Whitehead formulated an alternative theory of gravity that was regarded as a viable contender for several decades, until Clifford Will noticed in 1971 that it predicts grossly incorrect behavior for the ocean tides.
• George David Birkhoff's (1943) yields the same predictions for the classical four solar system tests as general relativity, but unfortunately requires sound waves to travel at the speed of light. Thus, like Whitehead's theory, it was never a viable theory after all, despite making an initially good impression on many experts.
• Like Nordström's theory, the gravitation theory of Wei-Tou Ni (1971) features a notion of prior geometry, but Will soon showed that it is not fully compatible with observation and experiment.
• The Brans-Dicke theory and the Rosen bimetric theory are two alternatives to general relativity which have been around for a very long time and which have also withstood many tests. However, they are less elegant and more complicated than general relativity, in several senses.
• There have been many attempts to formulate consistent theories which combine gravity and electromagnetism. The first of these, Weyl's gauge theory of gravitation, was immediately shot down (on a postcard) by Einstein himself,Template:Fact who pointed out to Hermann Weyl that in his theory, hydrogen atoms would have variable size, which they do not. Another early attempt, the original Kaluza-Klein theory, at first seemed to unify general relativity with classical electromagnetism, but is no longer regarded as successful for that purpose. Both these theories have turned out to be historically important for other reasons: Weyl's idea of gauge invariance survived and in fact is omnipresent in modern physics, while Kaluza's idea of compact extra dimensions has been resurrected in the modern notion of a braneworld.
• The Fierz-Pauli spin-two theory was an optimistic attempt to quantize general relativity, but it turns out to be internally inconsistent. Pascual Jordan's work toward fixing these problems eventually motivated the Brans-Dicke theory, and also influenced Richard Feynman's unsuccessful attempts to quantize gravity.
• Einstein-Cartan theory includes torsion terms, so it is not a metric theory in the strict sense.
• Teleparallel gravity goes further and replaces connections with nonzero curvature (but vanishing torsion) by ones with nonzero torsion (but vanishing curvature).
• The Nonsymmetric Gravitational Theory (NGT) of John W. Moffat is a dark horse in the race.

Even for "weak field" observations confined to our Solar system, various alternative theories of gravity predict quantitatively distinct deviations from Newtonian gravity. In the weak-field, slow-motion limit, it is possible to define 10 experimentally measurable parameters which completely characterize predictions of any such theory. This system of these parameters, which can be roughly thought of as describing a kind of ten dimensional "superspace" made from a certain class of classical gravitation theories, is known as PPN formalism (Parametric Post-Newtonian formalism). [3] Current bounds on the PPN parameters [4] are compatible with GR.

See in particular confrontation between Theory and Experiment in Gravitational Physics, a review paper by Clifford Will.

## History

General relativity was developed by Einstein in a process that began in 1907 with the publication of an article on the influence of gravity and acceleration on the behavior of light in special relativity. Most of this work was done in the years 1911–1915, beginning with the publication of a second article on the effect of gravitation on light. By 1912, Einstein was actively seeking a theory in which gravitation was explained as a geometric phenomenon. In December of 1915, these efforts culminated in Einstein's submission of a paper presenting the Einstein field equations, which are a set of differential equations. This paper was subsequently published in 1916.[2] Since 1915, the development of general relativity has focused on solving the field equations for various cases. This generally means finding metrics which correspond to realistic physical scenarios. The interpretation of the solutions and their possible experimental and observational testing also constitutes a large part of research in GR.

The expansion of the universe created an interesting episode for general relativity. Starting in 1922, researchers found that cosmological solutions of the Einstein field equations call for an expanding universe. Einstein did not believe in an expanding universe, and so he added a cosmological constant to the field equations to permit the creation of static universe solutions. In 1929, Edwin Hubble found evidence that the universe is expanding. This resulted in Einstein dropping the cosmological constant, referring to it as "the biggest blunder in my career".

Progress in solving the field equations and understanding the solutions has been ongoing. Notable solutions have included the Schwarzschild solution (1916), the Reissner-Nordström solution, the Friedmann-Robertson-Walker solution and the Kerr solution.

Observationally, general relativity has a history too. Einstein's showing that general relativity could account for the discrepancy between the Newtonian prediction for the perihelion precession of Mercury and the observed was the first evidence that general relativity is correct. In 1919, Eddington's announcement that his observations of stars near the eclipsed Sun confirmed Einstein's prediction for the deflection of light by the Sun helped to cement the status of general relativity as a likely true theory. Since then, many observations have confirmed the predictions of general relativity. These include observations of gravitational red shift, studies of binary pulsars, observations of radio signals passing the limb of the Sun, and even the GPS system.

## Status

The status of general relativity is decidedly mixed.

On the one hand, general relativity is a highly successful model of gravitation and cosmology. It has passed every unambiguous test to which it has been subjected so far, both observationally and experimentally. It is therefore almost universally accepted by the scientific community.

On the other hand, general relativity is inconsistent with quantum mechanics, and the singularities of black holes also raise some disconcerting issues. So while it is accepted, there is also a sense that something beyond general relativity may yet be found.

Currently, better tests of general relativity are needed. Even the most recent binary pulsar discoveries only test general relativity to the first order of deviation from Newtonian projections in the post-Newtonian parameterizations. Some way of testing second and higher order terms is needed, and may shed light on how reality differs from general relativity (if it does).

## Quotes

Spacetime grips mass, telling it how to move, and mass grips spacetime, telling it how to curveJohn Archibald Wheeler.
The theory appeared to me then, and still does, the greatest feat of human thinking about nature, the most amazing combination of philosophical penetration, physical intuition, and mathematical skill. But its connections with experience were slender. It appealed to me like a great work of art, to be enjoyed and admired from a distance.Max Born

## References

For a more complete list of available publications on general relativity, please see general relativity resources.
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## Bibliography

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• Template:Cite web Lectures presented at the Advanced School on Effective Field Theories (Almunecar, Spain, June 1995), to be published in the proceedings.