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. We use circular orbits as our prototype. This has the advantage that we know the kinetics of circular orbits. This allows us to calculate curvature of orbits in space directly and compare the results with dynamical forces.



The equivalence of gravitational and inertial mass

A unique feature of the gravitational force is that all massive objects accelerate in the same manner in a gravitational field. This is often expressed as "The gravitational mass is equal to the inertial mass." This allows us to think of gravity as a curvature of spacetime.

Test for flatness in spacetime

If initially parallel paths of two particles on nearby geodesics remain parallel within some accuracy, then spacetime is flat to within that accuracy. [Ref. 2, p. 30]

Two nearby particles in a radial gravitational field

Newtonian mechanics for circular orbits

The geodesic and field equations for circular orbits

Consider the situation in which there are two particles in nearby circular polar orbits of the Earth at radius  and speed . Since the orbits are circular, the gravitational force on the particles must equal the centripetal force,

where G is the gravitational constant and  is the mass of the earth.

The particles execute simple harmonic motion about the earth and with respect to each other. They are at their maximum distance from each other as they cross the equator. Their trajectories intersect at the poles.

From Newton's Law of Gravitation the separation vector  can be shown to be given by the "geodesic equation"

where  is the curvature of the trajectory and  is the speed of light c times the time.

The curvature of the trajectory is generated by the mass of the earth . This is represented by the "field equation"

In this example, the field equation is simply a statement of the Newtonian concept that centripetal force is equal to gravitational force for circular orbits. We refer to this expression as a field equation in order to highlight the similarities with the Einstein field equation. This equation is in a much different form than Gauss's law, which is the usual characterization of the field equation in Newtonian mechanics.

Relationship between curvature and mass density
Mass can be written in terms of the average mass density  inside a sphere of radius  by the expression

.

The field equation becomes

.

The curvature of the particle trajectories is proportional to mass density.

Local measurements

A requirement of General Relativity is that all measurements must be made locally. Imagine that the particles are inside a windowless spacecraft co-orbiting the Earth with the center of mass of the spacecraft coincident with one of the particles. That particle would be at rest with respect to the spacecraft. An observer in the spacecraft would have no indication that the craft was orbiting Earth. The observer is only allowed to measure the behavior of the particles in the frame of the craft.

In this example, we can define a local coordinate system such that the -direction is toward the ceiling of the craft and this is directed along . The -direction is toward the front of the craft and is in the direction of . The -direction is toward the left side of the craft.

In this frame, the vector  is the position vector for the second particle. An observer in the craft would think the second particle was oscillating in a potential well generated by a gravitational field. This is an example of a coordinate acceleration due to the choice of frames as opposed to a physical acceleration due to actual forces.

General motion in the earth's gravitational field

Elliptic and hyberbolic trajectories

More generally, particles move in elliptic or hyberbolic trajectories in a plane that contains the earth center. The orbits need not be circular. One can obtain intuitive geodesic and field equations in those situations as well [Ref 2, Chapter 1]. Unlike circular orbits, however, the speed of the particles in elliptic or hyperbolic trajectories is not constant. We therefore do not have a constant speed with which to scale the curvature. Therefore, in anticipation of the transition to relativistic mechanics, the trajectories and curvatures are scaled with the speed of light .

From Newton's Law of Gravitation

one can obtain the geodesic equation for the separation of two particles in nearby trajectories

and the field equation

if the particle separation is perpendicular to  and

if the separation is parallel to . In the calculation of  the radius was expanded in terms of . Only the linear term was retained.

In the case that the separation of the particle is radial, the curvature is negative. This will cause the particles to separate rather than to be drawn toward each other as in the case in which they have the same radius. This is easy to understand. Outer orbits travel slower than inner orbits. This leads to particle separation.

Local coordinate system

A local coordinate system for a space craft co-moving with one of the particles can again be defined. The -direction, toward the ceiling, is in the direction of . The -direction, toward the front of the craft, is perpendicular to  but still in the plane of the trajectory. Unlike in a circular orbit, this craft no longer necessarily points in the direction of the velocity. The -direction is toward the left side of the craft.

Tensor description

Simple diagonal frame

The geodesic equation in a radial gravitational field can be described succinctly in tensor notation [Ref. 2, p. 37] in the co-moving frame in which the ceiling of the space craft is in the  direction

where the Latin indices are over the spatial directions in the co-moving system, and we have used the Einstein summation convention in which repeated indices are summed. The curvature tensor  is given by

and the separation vector is given by

where  is the component of  in the  direction,  is the component in the  direction, and  is the component in the  direction.

In this co-moving coordinate system the curvature tensor is diagonal. This is not true in general.

Arbitrary orientation of the local frame

The co-moving spacecraft has no windows. An observer is not able to tell which direction is the  direction, nor can he/she know which direction is the velocity with respect to earth. The orientation of the spacecraft may be quite different from the simple coordinate system in which the ceiling is in the  direction and the front of the craft is in a direction coplanar with the radius and the velocity. We can transform our simple coordinates to an arbitrarily oriented coordinate system through rotations. This, however, destroys the diagonal nature of the curvature matrix.

Rotations are performed with a rotation matrix  such that the separation vector  is related to the separation vector before rotation  by the relation

.

The inverse  of  is defined by

,

which yields

.

Here  is the Kronecker delta.

A simple rotation matrix that rotates the coordinate axis through an angle  about the -axis is

.

This is a rotation in the y-z plane. The inverse is obtained by switching the sign of .

If the rotation matrix does not depend on time then the geodesic equation becomes, upon rotation

where

.

The curvature in the new coordinate system is non-diagonal. The inverse problem of transforming an arbitrary coordinate system into a diagonal system can be performed mathematically with the process of diagonalization.

Time dependent rotation of the local frame: Christoffel symbols

The space craft may tumble about its center of mass. In that case the rotation matrix is time dependent. If the rotation matrix is time dependent, then it does not commute with the time derivative.

In that case, the rotation of the separation velocity can be written

which becomes

where

is known as a Christoffel symbol.

The geodesic equation becomes

,

which is the same as before with the exception that the derivatives have been generalized.

Arbitrariness in the curvature

The velocity in the frame of the spacecraft can be written

.

The geodesic equation becomes

.

.

In an arbitrarily rotating spacecraft, the curvature of space is due to two terms, one due to the mass density and one due to the arbitrary rotation of the spacecraft. The arbitrary rotation is non-physical and must be eliminated in any real physical theory of gravitation. In General Relativity this is done with a process called Fermi–Walker transport. In a Euclidean sense, Fermi–Walker transport is simply a statement that the spacecraft is not allowed to tumble

for all i and j. The only time-dependent rotations allowed are those generated by the mass density.

General geodesic and field equations in a Newtonian setting

Geodesic equation

where

and  is a Christoffel symbol.

Field equation

where  is a rotation matrix and the curvature tensor is

.

The curvature is proportional to the mass density

.

Overview of the Newtonian picture

The geodesic and field equations simply are a restatement of Newton's Law of Gravitation as seen from a local frame of reference co-moving with the mass within the local frame. This picture contains many of the elements of General Relativity, including the concept that particles travel along geodesics in a curved space (spacetime in the relativistic case) and that the curvature is due to the presence of mass density (mass/energy density in the relativistic case). This picture also contains some of the mathematical machinery of General Relativity such as tensors, Christoffel symbols, and Fermi–Walker transport.

Relativistic generalization

General relativity generalizes the geodesic equation and the field equation to the relativistic realm in which trajectories in space are replaced with world lines in spacetime. The equations are also generalized to more complicated curvatures.

See also

Biographies
Albert Einstein
Élie Cartan
Bernhard Riemann
Enrico Fermi

Related mathematics
Mathematics of general relativity
Basic introduction to the mathematics of curved spacetime
Tidal tensor
Frame fields in general relativity

References

[1] 

[2] 

[3] 

[4] 

General relativity