Page d'accueil de |
version française |
pdf version of this document | |

Please help me ! Could a nice person correct my english? |

in General Relativity

**Christian Magnan**

The deviation of light rays near the Sun is one of the most dramatic predictions of general relativity and the verification of this effect by Eddington in 1919 brought a spectacular confirmation of Einstein's theory. But it is quite difficult to provide the reader with the details of the calculation as there is no simple way to do it. In fact, to get the result it is necessary to dive into the full theory of general relativity. Here is a good opportunity to discover this theory while illustrating it on an example!

The derivation of the equations given here closely follows the presentation of Edwin F. Taylor and John Archibald Wheeler in their delightful work "Exploring Black Holes, Introduction to General Relativity" (Addison Wesley Longman, 2000).

- Principle of the calculation
- Metrics for curved spacetime around a massive object
- The equations of a geodesic
- Energy of the particle
- Angular momentum of the particle
- Computing the orbit
- The trajectory of light
- Determination of the deflection angle
- Approximations and integration

- About this document...

General relativity teaches us that by propagating into space a photon follows what is called a "geodesic" of spacetime. Thus we have to examine the following points:

- what is a "geodesic"?
- which equations govern a geodesic?
- find the solutions of those equations and thus discover the trajectory of light through space
- compute the angle between the initial and final directions of light.

Newtonian mechanics describes the motion of a particle in an absolute space with respect to an absolute time. The position of the moving object is located by its coordinates with respect to some frame of reference and is given as a function of time . General relativity affirms that there exists no absolute time ant that time cannot be dissociated from space. The theory bases its reasoning on *events*, each event being characterized by a point M (where it happens!) and a time (when it happens!). The events attached to a moving particle constitute what is called a *worldline*.

Let us consider for example a spaceship moving freely through space, which means that all his motors are turned off. Let us imagine that regular flashes are emitted in accordance with a clock located inside the rocket and beating the time. The time interval between two successive flashes will be denoted by (this quantity is thus measured with respect to the proper time of the spaceship). Think now of another frame of reference as constituted by an ensemble of space beacons, also free from acceleration, at constant mutual distances from one another (each free beacon stays at the same distance from its neighbours). Every signal bears the indication of its position in space (for instance by showing its distance from some origin) and holds its own clock. The clocks of this second frame are synchronized between them. Then in that frame the interval between two flashes (i.e. two events) is characterized by two numbers: the space interval and the time interval . To determine those two quantities it suffices to record which beacon faces Flash #1 and which beacon faces Flash #2 while noting the times of those events.

Special relativity is based on the following principle. The proper time interval between Event #1 et Event #2 is given by the formula

(1) |

Be careful: unless otherwise indicated, distances will be measured in units of time, as is often done in astronomy. We have chosen to do so in writing Equation (1). On the contrary if distances *s* are expressed in conventional units, for instance in centimeters, then one should pass from the latter to our distance *s* expressed in seconds via the formula *s* (in seconds) = *s* (in centimeters)/*c**c* is the speed of light in conventional units, namely
cm/s. (Expressing distances and times with the same unit would amount to taking the speed of light equal to unity.)

In general relativity the property of invariance of the proper interval with respect to a change of the coordinates remains valid but only locally, i.e. under the condition of staying in a sufficiently small region of spacetime (its size depends on the accuracy of the measurements). The main novelty concerns the expression of the proper time as given by Formula (1). The coefficients entering this formula depend now on the point of spacetime under consideration and the resulting expression takes the name of *metrics*. In fact the whole structure of spacetime, and especially its curvature, is included in the local expression of and in the form of its coefficients.

We are interested here in the structure of spacetime around the sun. In order to describe the physics locally we consider two nearby events separated by infinitesimal amounts of the time and space coordinates , , and . If space were flat, the metrics would have the form

which is usually written (and a little sloppily) by convention as

(2) |

where *r* denotes the distance to the center and an azimutal angle in the plane of the orbit (see the figure below).

But spacetime around a center of attraction of mass (for instance a black hole or the vicinity of the sun) is not flat. It is characterized by the *Schwarzschild metric*

(3) |

The story is really fantastic: the *whole* structure of spacetime is embodied in this "simple" formula (3).Even the famous black hole lurks behind those apparently innocuous symbols.

One question: in which units is expressed the mass in that formula? It is seen that has the dimension of a length, a quantity that we measure here in seconds. Therefore will also be measured in seconds. The formula allowing to transform grams in seconds is

where .

The metric, that is (exactly) the formula expressing at a givent point of spacetime the temporal interval between two nearby events, reveals the presence of curvature as soon as the expression deviates from Formula (2) corresponding to flat euclidian space. That metric will allow us to find the properties of the motion of a test particle free from acceleration. Actually both special and general relativity teach us that between two given events and a freely moving body follows the path for which the time interval is maximum. Equivalently one can say that a freely moving particle follows a geodesic of spacetime as a geodesic is precisely defined by this property of maximazing the time interval.

Definition of a geodesic:the geodesic between two events and is the wordline for which the interval of proper time between and is maximum.

That property of maximazing the proper time will allow us to derive the equations of a geodesic. It will also yield the expressions of the energy and angular momentum of a particle in orbit around the center of attraction.

(4) |

In order to avoid varying all quantities at the same time, we assume in this experiment that the locations of the radii
,
and
are fixed and that only the time
, at which the second flash is emitted, is allowed to change. According to Formula (3) the interval of proper time over the first segment is given by its square

(5) |

(6) |

The lapse of time over Segment
between the events
and
is
, and therefore the proper time duration
is given by

(7) |

(8) |

To make the total time interval
maximum with respect to a variation
of the time
,
we write

(9) |

(10) |

We have discovered in Equation (10) a quantity that is the same for both segment. This quantity is thus a constant of the motion for the free particle under consideration. For good physical reasons (especially to recover the formulae of special relativity), one is led to identify that constant of motion as the ratio of the energy of the particle to its mass. We write this very important result under the form

(11) |

Incidentally we may notice that with the units we have chosen, energy and mass are expressed in the same unit (for instance the centimeter).

We have applied the principle of maximazing the proper time interval by varying the time of the intermediate event **E**_{2}. We now perform the same operation but this time we vary the angle
of that intermediate event. We recall that measures the direction of the moving particle with respect to some direction chosen as the origin. We call it the *azimuth*.

We consider again three events consisting in the emission of flashes inside a spaceship floating freely in space. The first segment connects Event to Event . The second segment connects to . The azimutal angle of the first event is fixed at . The angle of the last one is fixed at . The intermediate azimuth is taken as the variable . Again in order not to vary everything at the same time, we assume that the radius at which the second flash is emitted stays constant.

We follow the same chain of reasoning as in the previous section. From the metric (3), the time interval
over the first segment is given by its square

(12) |

(13) |

(14) | |||

(15) |

By writing one easily obtains, similarly to Formula (10)

(16) |

(17) |

Technically speaking in order to determine the trajectory of a moving body free from acceleration we apply the following strategy. Knowing the energy
and the angular momentum
of the particle of mass
( and
depend on the initial conditions) we can follow the position of that particle by computing the increments of its spacetime coordinates
,
and
as the proper time
itself advances. Algebraically for each increment
of the proper time we compute (or the computer calculates) the corresponding increments
,
and
of the coordinate of the mobile body. The squares of the increments
and
are extracted from Equations (11) and (17) in the following form:

(18) | |||

(19) |

We notice that the expression of
is missing. We get it by transporting the values of
and
into the metric equation (3) and solving it for
. This yields

(20) |

By dividing both sides of Equations (20) and (19) we directly arrive to the equation of the orbit in polar coordinates as

(21) |

Nevertheless it happens that by letting the mass of the particle tend towards zero, one arrives at the right results. Thus for
our equation (21) takes the form

(22) |

That equation will allow us to determine the deviation of ligth rays passing near the sun.

It is necessary to specify the parameters found in the formulae. First the angular momentum of the moving particle at infinity is equal by definition to the product of its linear momentum
by what is called the *impact parameter*
, which represents the distance between the center of attraction (the sun in the present case) and the initial direction of the velocity of the particle (see the figure).

In other words

(23) |

In addition it is known that the momentum
of a photon is equal to its energy
(with the units that were chosen). It results at once from this formula that

(24) |

(25) |

Formula (25) will allow us to determine the change in the direction of a light pulse caused by the gravitational field of the sun. To achieve this aim we have to sum up the successive infinitesimal increments
of the azimuthal angle
along the path. This means that we have to carry out the integration of
when *r* varies from the minimum distance denoted
( is the radius of the sun if the light ray grazes its surface). We should still multiply that quantity par 2 to account for both symmetrical "legs" of the trajectory (the photon first approaches the Sun then recedes from it).

It is necessary to stipulate a further point, namely the relation existing between the two quantities
and
that we have introduced and that are not independent. The point
corresponds to the place where the light photon is closest to the sun. There the photon moves tangentially. Since at that point there is no radial component, we can write that the derivative vanishes. It suffices to take the element from Equation (25) to find immediately

(26) |

(27) |

The form of the expression dictates to us to pose

where varies between 1 and 0. The last equation (27) then becomes

or | |||

(28) |

Consequently the infinitesimal variation of the azimuth is given in terms of the variation of
by

(29) |

The presence of the term
in Expression (29) encourages us to make the change of variable

which leads to

(30) |

By observing that

we end up with the final equation of the trajectory under the form

(31) |

It is interesting to emphasize that so far there have been no approximation. This is quite rewarding.

In Equation (31) we can thus use the classical approximation
to arrive at

(32) |

(33) | |||

(34) | |||

(35) |

The first term gives the total change in the azimuthal angle of the photon where there is no Sun present, since in that case the photon follows a straight path. But the second term gives the additional angle of deflection
with respect to this straight line (see the figure)

(36) | |||

or in conventional units | |||

(37) |

Numerically at the surface of the sun (with the values of the mass and the radius given above) one finds
radian, or ( knowing that
radians equal 180 degrees and that there are 60 minutes of arc in one degree and 60 seconds of arc in one minute of arc)

in General Relativity

This document was generated using the
**LaTeX2 HTML** translator Version 2002 (1.67)

Copyright © 1993, 1994, 1995, 1996,
Nikos Drakos,
Computer Based Learning Unit, University of Leeds.

Copyright © 1997, 1998, 1999,
Ross Moore,
Mathematics Department, Macquarie University, Sydney.

The command line arguments were:

**latex2html** `DeviationLumiere`

The translation was initiated by Christian Magnan on 2007-01-09

Christian Magnan 2007-01-09 | Page d'accueil |