Proper length or rest length is the length of an object in the object's rest frame. The measurement of lengths is more complicated in the theory of relativity than in classical mechanics. In classical mechanics, lengths are measured based on the assumption that the locations of all points involved are measured simultaneously. But in the theory of relativity, the notion of simultaneity is dependent on the observer. A different term, proper distance, provides an invariant measure whose value is the same for all observers. Proper distance is analogous to proper time. The difference is that the proper distance is defined between two spacelike-separated events, while the proper time is defined between two timelike-separated events.
Proper length or rest length
The proper length or rest length of an object is the length of the object measured by an observer which is at rest relative to it, by applying standard measuring rods on the object. The measurement of the object's endpoints doesn't have to be simultaneous, since the endpoints are constantly at rest at the same positions in the object's rest frame, so it is independent of Δt. This length is thus given by: However, in relatively moving frames the object's endpoints have to be measured simultaneously, since they are constantly changing their position. The resulting length is shorter than the rest length, and is given by the formula for length contraction : In comparison, the invariant proper distance between two arbitrary events happening at the endpoints of the same object is given by: So Δσ depends on Δt, whereas the object's rest length L0 can be measured independently of Δt. It follows that Δσ and L0, measured at the endpoints of the same object, only agree with each other when the measurement events were simultaneous in the object's rest frame so that Δt is zero. As explained by Fayngold:
In special relativity, the proper distance between two spacelike-separated events is the distance between the two events, as measured in an inertial frame of reference in which the events are simultaneous. In such a specific frame, the distance is given by where
The two formulae are equivalent because of the invariance of spacetime intervals, and since Δt = 0 exactly when the events are simultaneous in the given frame. Two events are spacelike-separated if and only if the above formula gives a real, non-zero value for Δσ.
The above formula for the proper distance between two events assumes that the spacetime in which the two events occur is flat. Hence, the above formula cannot in general be used in general relativity, in which curved spacetimes are considered. It is, however, possible to define the proper distance along a path in any spacetime, curved or flat. In a flat spacetime, the proper distance between two events is the proper distance along a straight path between the two events. In a curved spacetime, there may be more than one straight path between two events, so the proper distance along a straight path between two events would not uniquely define the proper distance between the two events. Along an arbitrary spacelike path P, the proper distance is given in tensor syntax by the line integral where
dxμ is the coordinate separation between neighboring events along the path P.
In the equation above, the metric tensor is assumed to use the +−−−metric signature, and is assumed to be normalized to return a time instead of a distance. The − sign in the equation should be dropped with a metric tensor that instead uses the −+++ metric signature. Also, the should be dropped with a metric tensor that is normalized to use a distance, or that uses geometrized units.
