# 3.2: Affine Notions and Parallel Transport

### The Affine Parameter in Curved Spacetime: A Rough Sketch

We want to be able to measure things in curved spacetime. There turn out to be two complementary systems of measurement we can apply: *affine measure* and *metric measure*. Affine measure in a flat geometry was introduced in Section 2.1. Surprisingly, it turns out to be quite easy to generalize this to the curved case. Our construction of the affine parameter with a scaffolding of parallelograms depended on the existence and uniqueness of parallels expressed by axiom A1, so we might imagine that there was no point in trying to generalize the construction to curved spacetime. But the equivalence principle tells us that spacetime is locally affine to some approximation. Concretely, clock-time is one example of an affine parameter, and the curvature of spacetime clearly can’t prevent us from building a clock and releasing it on a free-fall trajectory.

More generally, we can use the fact that every segment of a geodesic is geometrically similar to every other segment. For example, consider an arc of the earth’s equator spanning one degree of longitude. That arc could be slid along the equator to a different location, then expanded to cover 3 degrees of longitude. The two arcs are similar.

Example 2: Geodesics are special

The following three non-examples show that this is a special property of geodesics.

The property is not enjoyed by a non-geodesic curve. A segment of a pentagon that encompasses one of the vertices is not similar to some other segment that is straight.

Another non-example involving non-geodesics is the curve that we get in 1+1-dimensional spacetime by joining together the positive x axis and the positive t axis. We can never take a one-year segment of the t axis and, through any combination of boosts and rotations, make it coincide with a one-light-year piece of the x axis. The original segment is timelike, and any boost or rotation will preserve its timelike character.

Furthermore, it is not true in general, when curvature exists, that we can take any geometrical figure, transport it wherever we like, and also scale it as we like. For example, Euclidean geometry is a good approximation on small portions of the Earth’s spherical surface, so a roadmap can be made in the shape of a rectangle with four right-angle corners. However, it is not possible to scale up such a rectangle; to map a large portion of the world, we have to introduce distortions of the type used in map projections.

Because geodesics have this special property, we can slide any portion of a geodesic to anywhere else on the geodesic and employ it as a standard of measure. This gives us a complete system of measurement along that geodesic, and it works regardless of whether the geodesic is timelike, lightlike, or spacelike. But as in flat geometry, affine measurement does not allow us to compare lengths along one geodesic to lengths along another.

### The Affine Parameter in More Detail

When we originally defined affine measure in Section 2.1, for a flat space, we did it through the explicit construction of a scaffolding. An important example of the differential, i.e., local, nature of our geometry is the generalization of the scaffolding construction from to a context broader than affine geometry.

To generalize the recipe for the construction (Figure 3.2.1), the first obstacle is the ambiguity of the instruction to construct parallelogram \((0,1,q_0,q_1)\), which requires us to draw 1q_{1} parallel to 0q_{0}. Suppose we construe this as an instruction to make the two segments initially parallel, i.e., parallel as they depart the line at 0 and 1. By the time they get to q_{0} and q_{1}, they may be converging or diverging.

**Figure \(\PageIndex{1}\)** - Construction of an affine parameter in curved spacetime.

Because parallelism is only approximate here, there will be a certain amount of error in the construction of the affine parameter. One way of detecting such an error is that lattices constructed with different initial distances will get out of step with one another. For example, we can define \(\frac{1}{2}\) as before by requiring that the lattice constructed with initial segment 0 \(\frac{1}{2}\) line up with the original lattice at 1. We will find, however, that they do *not *quite line up at other points, such as 2. Let’s use this discrepancy \(\epsilon\) = 2 − 2' as a numerical measure of the error. It will depend on both \(\delta_{1}\), the distance 01, and on \(\delta_{2}\), the distance between 0 and q_{0}. Since \(\epsilon\) vanishes for either \(\delta_{1}\) = 0 or \(\delta_{2}\) = 0, and since the equivalence principle guarantees smooth behavior on small scales, the leading term in the error will in general be proportional to the product \(\delta_{1} \delta_{2}\). In the language of infinitesimals, we can replace \(\delta_{1}\) and \(\delta_{2}\) with infinitesimally short distances, which for simplicity we assume to be equal, and which we call d\(\lambda\). Then the affine parameter \(\lambda\) is defined as \(\lambda = \int d \lambda\), where the error of order d\(\lambda^{2}\) is, as usual, interpreted as the negligible discrepancy between the integral and its approximation as a Riemann sum.

### Parallel Transport

If you were alert, you may have realized that I cheated you at a crucial point in this construction. We were to make 1q_{1} and 0q_{0} “initially parallel” as they left 01. How should we even define this idea of “initially parallel?” We could try to do it by making angles q_{0}01 and q_{1}12 equal, but this doesn’t quite work, because it doesn’t specify whether the angle is to the left or the right on the two-dimensional plane of the page. In three or more dimensions, the issue becomes even more serious. The construction workers building the lattice need to keep it all in one plane, but how do they do that in curved spacetime?

A mathematician’s answer would be that our geometry lacks some additional structure called a *connection*, which is a rule that specifies how one locally flat neighborhood is to be joined seamlessly onto another locally flat neighborhood nearby. If you’ve ever bought two maps and tried to tape them together to make a big map, you’ve formed a connection. If the maps were on a large enough scale, you also probably noticed that this was impossible to do perfectly, because of the curvature of the earth.

Physically, the idea is that in flat spacetime, it is possible to construct inertial guidance systems like the ones discussed earlier. Since they are possible in flat spacetime, they are also possible in locally flat neighborhoods of spacetime, and they can then be carried from one neighborhood to another. In three space dimensions, a gyroscope’s angular momentum vector maintains its direction, and we can orient other vectors, such as 1q_{1}, relative to it. Suppose for concreteness that the construction of the affine parameter above is being carried out in three space dimensions. We place a gyroscope at 0, orient its axis along 0q_{0}_{ }, slide it along the line to 1, and then construct 1q_{1} along that axis.

In 3+1 dimensions, a gyroscope only does part of the job. We now have to maintain the direction of a four-dimensional vector. Four-vectors will not be discussed in detail until section 4.2, but similar devices can be used to maintain their orientations in spacetime. These physical devices are ways of defining a mathematical notion known as *parallel transport*, which allows us to take a vector from one point to another in space. In general, specifying a notion of parallel transport is equivalent to specifying a connection.

Parallel transport is path-dependent, as shown in Figure 3.2.2.

**Figure \(\PageIndex{2}\)** - Parallel transport is path-dependent. On the surface of this sphere, parallel-transporting a vector along ABC gives a different answer than transporting it along AC.

##### Affine Parameters Defined Only along Geodesics

In the context of flat spacetime, the affine parameter was defined only along lines, not arbitrary curves, and could not be compared between lines running in different directions. In curved spacetime, the same limitation is present, but with “along lines” replaced by “along geodesics.” Figure 3.2.3 shows what goes wrong if we try to apply the construction to a world-line that isn’t a geodesic. One definition of a geodesic is that it’s the course we’ll end up following if we navigate by keeping a fixed bearing relative to an inertial guidance device such as gyroscope; that is, the tangent to a geodesic, when parallel-transported farther along the geodesic, is still tangent. A non-geodesic curve lacks this property, and the effect on the construction of the affine parameter is that the segments nq_{n} drift more and more out of alignment with the curve.

**Figure \(\PageIndex{3}\)** - Bad things happen if we try to construct an affine parameter along a curve that isn’t a geodesic. This curve is similar to path ABC in Figure 3.2.2. Parallel transport doesn’t preserve the vectors’ angle relative to the curve, as it would with a geodesic. The errors in the construction blow up in a way that wouldn’t happen if the curve had been a geodesic. The fourth dashed parallel flies off wildly around the back of the sphere, wrapping around and meeting the curve at a point, 4, that is essentially random.

### Contributors

- Benjamin Crowell (Fullerton College). General Relativity is copyrighted with a CC-BY-SA license.