Born coordinates

To motivate the Born chart, we first consider the family of Langevin observers represented in an ordinary cylindrical coordinate chart for Minkowski spacetime. The world lines of these observers form a timelike congruence which is rigid in the sense of having a vanishing expansion tensor. They represent observers who rotate rigidly around an axis of cylindrical symmetry.

Fig. 1: Part of the helical world line of a typical Langevin observer (red curve), depicted in the cylindrical chart, with some future pointing light cones (gold) with the frame vectors assigned by the Langevin frame (black rods). In this figure, the Z coordinate is inessential and has been suppressed. The white cylinder shows a locus of constant radius; the dashed green line represents the symmetry axis R=0. The blue curve is an integral curve of the azimuthal unit vector ${\displaystyle {\vec {p}}_{3}}$.

From the line element

${\displaystyle {\begin{aligned}&\mathrm {d} s^{2}=-\mathrm {d} T^{2}+\mathrm {d} Z^{2}+\mathrm {d} R^{2}+R^{2}\,\mathrm {d} \Phi ^{2},\;\;\\&-\infty <T,\,Z<\infty ,\;0<R<\infty ,\;-\pi <\Phi <\pi \end{aligned}}}$

we can immediately read off a frame field representing the local Lorentz frames of stationary (inertial) observers

${\displaystyle {\vec {e}}_{0}=\partial _{T},\;\;{\vec {e}}_{1}=\partial _{Z},\;\;{\vec {e}}_{2}=\partial _{R},\;\;{\vec {e}}_{3}={\frac {1}{R}}\,\partial _{\Phi }}$

Here, ${\displaystyle {\vec {e}}_{0}}$ is a timelike unit vector field while the others are spacelike unit vector fields; at each event, all four are mutually orthogonal and determine the infinitesimal Lorentz frame of the static observer whose world line passes through that event.

Simultaneously boosting these frame fields in the ${\displaystyle {\vec {e}}_{3}}$ direction, we obtain the desired frame field describing the physical experience of the Langevin observers, namely

${\displaystyle {\vec {p}}_{0}={\frac {1}{\sqrt {1-\omega ^{2}\,R^{2}}}}\,\partial _{T}+{\frac {\omega \,R}{\sqrt {1-\omega ^{2}\,R^{2}}}}\;{\frac {1}{R}}\partial _{\Phi }}$

${\displaystyle {\vec {p}}_{1}=\partial _{Z},\;\;{\vec {p}}_{2}=\partial _{R}}$

${\displaystyle {\vec {p}}_{3}={\frac {1}{\sqrt {1-\omega ^{2}\,R^{2}}}}\;{\frac {1}{R}}\,\partial _{\Phi }+{\frac {\omega \,R}{\sqrt {1-\omega ^{2}\,R^{2}}}}\,\partial _{T}}$

This frame was apparently first introduced (implicitly) by Paul Langevin in 1935; its first explicit use appears to have been by T. A. Weber, as recently as 1997! It is defined on the region 0 < R < 1/ω; this limitation is fundamental, since near the outer boundary, the velocity of the Langevin observers approaches the speed of light.

Fig. 2: This figure shows the world lines of a fiducial Langevin observer (red curve) and his nearest neighbors (dashed navy blue curves). It shows one quarter of one orbit by the fiducial observer about the axis of symmetry (vertical green line).

Each integral curve of the timelike unit vector field ${\displaystyle {\vec {p}}_{0}}$ appears in the cylindrical chart as a helix with constant radius (such as the red curve in Fig. 1). Suppose we choose one Langevin observer and consider the other observers who ride on a ring of radius R which is rigidly rotating with angular velocity ω. Then if we take an integral curve (blue helical curve in Fig. 1) of the spacelike basis vector ${\displaystyle {\vec {p}}_{3}}$, we obtain a curve which we might hope can be interpreted as a "line of simultaneity" for the ring-riding observers. But as we see from Fig. 1, ideal clocks carried by these ring-riding observers cannot be synchronized. This is our first hint that it is not as easy as one might expect to define a satisfactory notion of spatial geometry even for a rotating ring, much less a rotating disk!

Computing the kinematic decomposition of the Langevin congruence, we find that the acceleration vector is

${\displaystyle \nabla _{{\vec {p}}_{0}}{\vec {p}}_{0}={\frac {-\omega ^{2}\,R}{1-\omega ^{2}\,R^{2}}}\;{\vec {p}}_{2}}$

This points radially inward and it depends only on the (constant) radius of each helical world line. The expansion tensor vanishes identically, which means that nearby Langevin observers maintain constant distance from each other. The vorticity vector is

${\displaystyle {\vec {\Omega }}={\frac {\omega }{1-\omega ^{2}\,R^{2}}}\;{\vec {p}}_{1}}$

which is parallel to the axis of symmetry. This means that the world lines of the nearest neighbors of each Langevin observer are twisting about its own world line, as suggested by Fig. 2. This is a kind of local notion of "swirling" or vorticity.

In contrast, note that projecting the helices onto any one of the spatial hyperslices ${\displaystyle T=T_{0}}$ orthogonal to the world lines of the static observers gives a circle, which is of course a closed curve. Even better, the coordinate basis vector ${\displaystyle \partial _{\Phi }}$ is a spacelike Killing vector field whose integral curves are closed spacelike curves (circles, in fact), which moreover degenerate to zero length closed curves on the axis R = 0. This expresses the fact that our spacetime exhibits cylindrical symmetry, and also exhibits a kind of global notion of the rotation of our Langevin observers.

In Fig. 2, the magenta curve shows how the spatial vectors ${\displaystyle {\vec {p}}_{2},\;{\vec {p}}_{3}}$ are spinning about ${\displaystyle {\vec {p}}_{1}}$ (which is suppressed in the figure since the Z coordinate is inessential). That is, the vectors ${\displaystyle {\vec {p}}_{2},\;{\vec {p}}_{3}}$ are not Fermi–Walker transported along the world line, so the Langevin frame is spinning as well as non-inertial. In other words, in our straightforward derivation of the Langevin frame, we kept the frame aligned with the radial coordinate basis vector ${\displaystyle \partial _{R}}$. By introducing a constant rate rotation of the frame carried by each Langevin observer about ${\displaystyle {\vec {p}}_{1}}$, we could, if we wished "despin" our frame to obtain a gyrostabilized version.

Fig. 3: An attempt to define a notion of "space at a time" for our Langevin observers, depicted in the Born chart. This attempt is doomed to fail for at least two reasons! This figure depicts the region 0 < r < 1 when ω = 1/5, with a discontinuity at ϕ = π. The radial ray from which we have "grown" the integral curves to make the surface is at ϕ = 0 (on the far side in this image).

To obtain the Born chart, we straighten out the helical world lines of the Langevin observers using the simple coordinate transformation

${\displaystyle t=T,\;\;z=Z,\;\;r=R,\;\;\phi =\Phi -\omega \,T}$

The new line element is

${\displaystyle \mathrm {d} s^{2}=-\left(1-\omega ^{2}r^{2}\right)\mathrm {d} t^{2}+2\omega r^{2}\mathrm {d} t\,\mathrm {d} \phi +\mathrm {d} z^{2}+\mathrm {d} r^{2}+r^{2}\mathrm {d} \phi ^{2},}$

${\displaystyle -\infty <t,\,z<\infty ,0<r<{\frac {1}{\omega }},\;-\pi <\phi <\pi }$

Notice the "cross-terms" involving ${\displaystyle \mathrm {d} t\,\mathrm {d} \phi }$, which show that the Born chart is not an orthogonal coordinate chart. The Born coordinates are also sometimes referred to as rotating cylindrical coordinates.

In the new chart, the world lines of the Langevin observers appear as vertical straight lines. Indeed, we can easily transform the four vector fields making up the Langevin frame into the new chart. We obtain

${\displaystyle {\vec {p}}_{0}={\frac {1}{\sqrt {1-\omega ^{2}\,r^{2}}}}\,\partial _{t}}$

${\displaystyle {\vec {p}}_{1}=\partial _{z},\;\;{\vec {p}}_{2}=\partial _{r}}$

${\displaystyle {\vec {p}}_{3}={\frac {\sqrt {1-\omega ^{2}\,r^{2}}}{r}}\,\partial _{\phi }+{\frac {\omega \,r}{\sqrt {1-\omega ^{2}\,r^{2}}}}\,\partial _{t}}$

These are exactly the same vector fields as before – they are now simply represented in a different coordinate chart!

Needless to say, in the process of "unwinding" the world lines of the Langevin observers, which appear as helices in the cylindrical chart, we "wound up" the world lines of the static observers, which now appear as helices in the Born chart! Note too that, like the Langevin frame, the Born chart is only defined on the region 0 < r < 1/ω.

If we recompute the kinematic decomposition of the Langevin observers, that is of the timelike congruence ${\displaystyle {\vec {p}}_{0}={\frac {1}{\sqrt {1-\omega ^{2}\,r^{2}}}}\,\partial _{t}}$, we will of course obtain the same answer that we did before, only expressed in terms of the new chart. Specifically, the acceleration vector is

${\displaystyle \nabla _{{\vec {p}}_{0}}\,{\vec {p}}_{0}={\frac {-\omega ^{2}\,r}{1-\omega ^{2}\,r^{2}}}\,{\vec {p}}_{2}}$

the expansion tensor vanishes, and the vorticity vector is

${\displaystyle {\vec {\Omega }}={\frac {\omega }{1-\omega ^{2}\,r^{2}}}\;{\vec {p}}_{1}}$

The dual covector field of the timelike unit vector field in any frame field represents infinitesimal spatial hyperslices. However, the Frobenius integrability theorem gives a strong restriction on whether or not these spatial hyperplane elements can be "knit together" to form a family of spatial hypersurfaces which are everywhere orthogonal to the world lines of the congruence. Indeed, it turns out that this is possible, in which case we say the congruence is hypersurface orthogonal, if and only if the vorticity vector vanishes identically. Thus, while the static observers in the cylindrical chart admits a unique family of orthogonal hyperslices ${\displaystyle T=T_{0}}$, the Langevin observers admit no such hyperslices. In particular, the spatial surfaces ${\displaystyle t=t_{0}}$ in the Born chart are orthogonal to the static observers, not to the Langevin observers. This is our second (and much more pointed) indication that defining "the spatial geometry of a rotating disk" is not as simple as one might expect.

To better understand this crucial point, consider integral curves of the third Langevin frame vector

${\displaystyle {\vec {p}}_{3}={\sqrt {1-\omega ^{2}\,r^{2}}}\,{\frac {1}{r}}\,\partial _{\phi }+{\frac {\omega \,r}{\sqrt {1-\omega ^{2}\,r^{2}}}}\,\partial _{t}}$

which pass through the radius ${\displaystyle \phi =0,\,t=0}$. (For convenience, we will suppress the inessential coordinate z from our discussion.) These curves lie in the surface

${\displaystyle \phi +\omega \,t-{\frac {t}{\omega \,r^{2}}}=0,\;\;-\pi <\phi <\pi }$

shown in Fig. 3. We would like to regard this as a "space at a time" for our Langevin observers. But two things go wrong.

First, the Frobenius theorem tells us that ${\displaystyle {\vec {p}}_{2},\,{\vec {p}}_{3}}$ are tangent to no spatial hyperslice whatever. Indeed, except on the initial radius, the vectors ${\displaystyle {\vec {p}}_{2}}$ do not lie in our slice. Thus, while we found a spatial hypersurface, it is orthogonal to the world lines of only some our Langevin observers. Because the obstruction from the Frobenius theorem can be understood in terms of the failure of the vector fields ${\displaystyle {\vec {p}}_{2},\,{\vec {p}}_{3}}$ to form a Lie algebra, this obstruction is differential, in fact Lie theoretic. That is, it is a kind of infinitesimal obstruction to the existence of a satisfactory notion of spatial hyperslices for our rotating observers.

Second, as Fig. 3 shows, our attempted hyperslice would lead to a discontinuous notion of "time" due to the "jumps" in the integral curves (shown as a blue colored grid discontinuity). Alternatively, we could try to use a multivalued time. Neither of these alternatives seems very attractive! This is evidently a global obstruction. It is of course a consequence of our inability to synchronize the clocks of the Langevin observers riding even a single ring – say the rim of a disk – much less an entire disk.

Imagine that we have fastened a fiber-optic cable around the circumference of a ring of radius ${\displaystyle r_{0}}$ which is rotating with steady angular velocity ω. We wish to compute the round trip travel time, as measured by a ring-riding observer, for a laser pulse sent clockwise and counterclockwise around the cable. For simplicity, we will ignore the fact that light travels through a fiber optic cable at somewhat less than the speed of light in vacuum, and will pretend that the world line of our laser pulse is a null curve (but certainly not a null geodesic!).

In the Born line element, let us put ${\displaystyle \mathrm {d} s=\mathrm {d} z=\mathrm {d} r=0}$. This gives

${\displaystyle (1-\omega ^{2}\,r_{0}^{2})\,\mathrm {d} t^{2}=2\omega \,r_{0}^{2}\,\mathrm {d} t\,\mathrm {d} \phi +r_{0}^{2}\,\mathrm {d} \phi ^{2}}$

or

${\displaystyle \mathrm {d} t_{+}={\frac {r_{0}\,\mathrm {d} \phi }{1-\omega \,r_{0}}},\quad \mathrm {d} t_{-}=-{\frac {r_{0}\,\mathrm {d} \phi }{1+\omega \,r_{0}}}}$

We obtain for the round trip travel time

${\displaystyle \Delta t_{+}=\int _{0}^{2\pi }{\frac {r_{0}\,\mathrm {d} \phi }{1-\omega \,r_{0}}}={\frac {2\pi r_{0}}{1-\omega \,r_{0}}},\quad \Delta t_{-}=\int _{0}^{-2\pi }-{\frac {r_{0}\,\mathrm {d} \phi }{1+\omega \,r_{0}}}={\frac {2\pi r_{0}}{1+\omega \,r_{0}}}}$

Putting ${\displaystyle \delta ={\frac {\Delta t_{+}-\Delta t_{-}}{2\,\pi \,r_{0}}}}$, we find ${\displaystyle \omega _{+,-}={\frac {-1\pm {\sqrt {1+\delta ^{2}}}}{r_{0}\,\delta }}}$ (positive ω means counter-clockwise rotation, negative ω means clockwise rotation) so that the ring-riding observers can determine the angular velocity of the ring (as measured by a static observer) from the difference between clockwise and counterclockwise travel times. This is known as the Sagnac effect. It is evidently a global effect.

Fig. 4: Two radial null geodesic tracks (green curve: outward bound, red curve: inward bound) depicted in the Born chart. The track of a Langevin observer L orbiting counter-clockwise at radius R = R₀, i.e. riding a counter-clockwise rotating ring, is also shown (navy blue circle). Parameters: ω = +0.2, R₀=r₀=1

We wish to compare the appearance of null geodesics in the cylindrical chart and the Born chart.

In the cylindrical chart, the geodesic equations read

${\displaystyle {\ddot {T}}=0,\;\;{\ddot {Z}}=0,\;\;{\ddot {R}}-R\,{\dot {\Phi }}^{2}=0,\;\;{\ddot {\Phi }}+{\frac {2}{R}}\,{\dot {\Phi }}\,{\dot {R}}=0.}$

We immediately obtain the first integrals

${\displaystyle {\dot {T}}=E,\;\;{\dot {Z}}=P,\;\;{\dot {\Phi }}={\frac {L}{R^{2}}}.}$

Plugging these into the expression obtained from the line element by setting ${\displaystyle \mathrm {d} s^{2}=0}$, we obtain

${\displaystyle {\dot {R}}^{2}=E^{2}-P^{2}-{\frac {L^{2}}{R^{2}}}\geq 0}$

from which we see that the minimal radius of a null geodesic is given by

${\displaystyle E^{2}-P^{2}-{\frac {L^{2}}{R_{\mathrm {min} }^{2}}}=0\quad }$ i.e., ${\displaystyle \quad R_{\mathrm {min} }={\frac {|L|}{\sqrt {E^{2}-P^{2}}}}}$

hence

${\displaystyle {\dot {R}}^{2}=L^{2}\left({\frac {1}{R_{\mathrm {min} }^{2}}}-{\frac {1}{R^{2}}}\right).}$

Fig. 5: Null geodesics depicted in the Born chart between ring riding Langevin observers (r = r₀ = 1). Null geodesics propagating with the rotation are bent inward (green curve), null geodesics propagating against the rotation are bent outward (red curve). The proper light-travel time from L₁ to L₂ Δt₁₂ is 1.311, from L₂ to L₁ Δt₂₁ is 1.510, the proper light-travel times are not symmetrical but the radar distance (Δt₁₂ + Δt₂₁)/2 is. For ω → 0 both proper light-travel times tend toward √2 = 1.414. Null geodesics between opposite Langevin observers (L₁ and L₃) bend symmetrically around the center of rotation. Parameters: ω = +0.1, R₀=r₀=1, Δϕ(L₁,L₂)=π/2, Δϕ(L₁,L₃)=π

We can now solve to obtain the null geodesics as curves parameterized by an affine parameter, as follows:

${\displaystyle {\begin{aligned}R&={\sqrt {(E^{2}-P^{2})\,s^{2}+L^{2}/(E^{2}-P^{2})}}=\\&={\sqrt {(E^{2}-P^{2})\,s^{2}+R_{\mathrm {min} }^{2}}},\\T&=T_{0}+E\,s,\\[1em]Z&=Z_{0}+P\,s,\\\Phi &=\Phi _{0}+\operatorname {arctan} \left({\frac {E^{2}-P^{2}}{L}}\,s\right)=\\&=\Phi _{0}+\operatorname {arctan} \left({\frac {\sqrt {E^{2}-P^{2}}}{R_{\mathrm {min} }\,\operatorname {sgn} {(L)}}}\,s\right).\end{aligned}}}$

More useful for our purposes is the observation that the trajectory of a null geodesic (its projection into any spatial hyperslice ${\displaystyle T=T_{0}}$) is of course a straight line, given by

${\displaystyle R=R_{\mathrm {min} }\,\sec(\Phi -\Phi _{0}).}$

To obtain the minimal radius of the line through two points (on the same side of the point of closest approach to the origin), we solve

${\displaystyle R_{1}=R_{\mathrm {min} }\,\sec(\Phi _{1}-\Phi _{0}),\;\;R_{2}=R_{\mathrm {min} }\,\sec(\Phi _{2}-\Phi _{0})}$

which gives

${\displaystyle R_{\mathrm {min} }={\frac {R_{1}\,R_{2}\,|\sin(\Phi _{2}-\Phi _{1})|}{\sqrt {R_{1}^{2}-2\,R_{1}\,R_{2}\,\cos(\Phi _{2}-\Phi _{1})+R_{2}^{2}}}}.}$

Now consider the simplest case, the radial null geodesics (R_min = L = 0, E = 1, P = 0). An outward bound radial null geodesic may be written in the form

${\displaystyle T=s,\;Z=Z_{0},\;R=s,}$

${\displaystyle \Phi =\mathrm {const.} =\omega \,R_{0}}$

with the radius R₀ of the ring riding Langevin observer (see Fig. 4). Transforming to the Born chart, we find that the trajectory can be written as

${\displaystyle r=r_{0}-{\frac {\phi }{\omega }}.}$

The tracks turn out to appear slightly bent in the Born chart (see green curve in Fig. 4). From section Transforming to the Born chart we see, that in the Born chart we cannot properly refer to these "tracks" as "projections" as for the Langevin observer an orthogonal hyperslice for t = t₀ does not exist (see Fig. 3).

Similarly for inward bound radial null geodesics we get

${\displaystyle r={\frac {\phi }{\omega }}}$

depicted as red curve in Fig. 4.

Notice that to send a laser pulse toward the stationary observer S at R = 0, the Langevin observer L has to aim slightly behind to correct for its own motion. Turning things around, just as a duck hunter would expect, to send a laser pulse toward the Langevin observer riding a counterclockwise rotating ring, the central observer has to aim, not at this observer's current position, but at the position at which he will arrive just in time to intercept the signal. These families of inward and outward bound radial null geodesics represent very different curves in spacetime and their projections do not agree for ω > 0.

Fig. 6: A null geodesic arc, depicted in the Born chart, which models a signal sent from one ring-riding observer to another. The world lines of these observers are shown as blue vertical lines; the center of symmetry as a green vertical line. Notice that our null geodesic (amber arc) appears to bend slightly inward (see also green curve in Fig. 5).

Similarly, null geodesics between ring-riding Langevin observers appear slightly bent inward in the Born chart, if the geodesics propagate with the direction of the rotation (see green curve in Fig. 5). To see this, write the equation of a null geodesic in the cylindrical chart in the form

${\displaystyle T=R_{\mathrm {min} }\,\tan(\Phi ),}$

${\displaystyle R=R_{\mathrm {min} }\,\sec(\Phi ).}$

Transforming to Born coordinates, we obtain the equations

${\displaystyle t=r_{\mathrm {min} }\,\tan(\phi +\omega \,t),}$

${\displaystyle r=r_{\mathrm {min} }\,\sec(\phi +\omega \,t).}$

Eliminating ϕ gives

${\displaystyle r={\sqrt {r_{\mathrm {min} }^{2}+t^{2}}}}$

which shows that the geodesic does indeed appear to bend inward (see Fig. 6). We also find that

${\displaystyle \phi =-\omega \,t+\operatorname {arctan} (t/r_{\mathrm {min} }).}$

For null geodesics propagating against the rotation (red curve in Fig. 5) we get

${\displaystyle r={\sqrt {r_{\mathrm {min} }^{2}+t^{2}}},}$

${\displaystyle \phi =-\omega \,t-\operatorname {arctan} (t/r_{\mathrm {min} })}$

and the geodesic bends slightly outward. This completes the description of the appearance of null geodesics in the Born chart, since every null geodesic is either radial or else has some point of closest approach to the axis of cylindrical symmetry.

Note (see Fig. 5) that a ring-riding observer trying to send a laser pulse to another ring-riding observer must aim slightly ahead or behind of his angular coordinate as given in the Born chart, in order to compensate for the rotational motion of the target. Note too that the picture presented here is fully compatible with our expectation (see appearance of the night sky) that a moving observer will see the apparent position of other objects on his celestial sphere to be displaced toward the direction of his motion.

Fig. 7: This schematic figure illustrates the notion of radar distance between a ring-riding observer and a static central observer (with the same Z coordinate).

Even in flat spacetime, it turns out that accelerating observers (even linearly accelerating observers; see Rindler coordinates) can employ various distinct but operationally significant notions of distance. Perhaps the simplest of these is radar distance.

Consider how a static observer at R=0 might determine his distance to a ring riding observer at R = R₀. At event C he sends a radar pulse toward the ring, which strikes the world line of a ring-riding observer at A′ and then returns to the central observer at event C″. (See the right hand diagram in Fig. 7.) He then divides the elapsed time (as measured by an ideal clock he carries) by two. It is not hard to see that he obtains for this distance simply R₀ (in the cylindrical chart), or r₀ (in the Born chart).

Similarly, a ring-riding observer can determine his distance to the central observer by sending a radar pulse, at event A toward the central observer, which strikes his world line at event C′ and returns to the ring-riding observer at event A″. (See the left hand diagram in Fig. 7.) It is not hard to see that he obtains for this distance ${\displaystyle R_{0}{\sqrt {1-\omega ^{2}\,R_{0}^{2}}}}$ (in the cylindrical chart) or ${\displaystyle r_{0}{\sqrt {1-\omega ^{2}\,r_{0}^{2}}}}$ (in the Born chart), a result which is somewhat smaller than the one obtained by the central observer. This is a consequence of time dilation: the elapsed time for a ring riding observer is smaller by the factor ${\displaystyle {\sqrt {1-\omega ^{2}\,r_{0}^{2}}}}$ than the time for the central observer. Thus, while radar distance has a simple operational significance, it is not even symmetric.

Fig. 8: This schematic figure illustrates the notion of radar distance between two Langevin observers riding a ring with radius R₀ which is rotating with angular velocity ω. In the left hand diagram, the ring is rotating counter-clockwise; in the right hand diagram, it is rotating clockwise.

To drive home this crucial point, compare the radar distances obtained by two ring-riding observers with radial coordinate R = R₀. In the left hand diagram at Fig. 8, we can write the coordinates of event A as

${\displaystyle T=0,\;Z=0,\;X=R_{0},Y=0}$

and we can write the coordinates of event B′ as

${\displaystyle T=2\,R_{0}\,\sin \left({\frac {\Phi }{2}}\right),\;Z=0,}$

${\displaystyle X=R_{0}\cos(\Phi ),\;Y=R_{0}\sin(\Phi )}$

Writing the unknown elapsed proper time as ${\displaystyle \Delta s}$, we now write the coordinates of event A″ as

${\displaystyle T={\frac {\Delta s}{\sqrt {1-\omega ^{2}\,R_{0}^{2}}}},\;Z=0}$

${\displaystyle X=R_{0}\cos \left({\frac {\omega \,\Delta s}{\sqrt {1-\omega ^{2}\,R_{0}^{2}}}}\right),\;Y=R_{0}\sin \left({\frac {\omega \,\Delta s}{\sqrt {1-\omega ^{2}\,R_{0}^{2}}}}\right)}$

By requiring that the line segments connecting these events be null, we obtain an equation which in principle we can solve for Δ s. It turns out that this procedure gives a rather complicated nonlinear equation, so we simply present some representative numerical results. With R₀ = 1, Φ = π/2, and ω = 1/10, we find that the radar distance from A to B is about 1.311, while the distance from B to A is about 1.510. As ω tends to zero, both results tend toward √2 = 1.414 (see also Fig. 5).

Despite these possibly discouraging discrepancies, it is by no means impossible to devise a coordinate chart which is adapted to describing the physical experience of a single Langevin observer, or even a single arbitrarily accelerating observer in Minkowski spacetime. Pauri and Vallisneri have adapted the Märzke-Wheeler clock synchronization procedure to devise adapted coordinates they call Märzke-Wheeler coordinates (see the paper cited below). In the case of steady circular motion, this chart is in fact very closely related to the notion of radar distance "in the large" from a given Langevin observer.

As was mentioned above, for various reasons the family of Langevin observers admits no family of orthogonal hyperslices. Therefore, these observers simply cannot be associated with any slicing of spacetime into a family of successive "constant time slices".

However, because the Langevin congruence is stationary, we can imagine replacing each world line in this congruence by a point. That is, we can consider the quotient space of Minkowski spacetime (or rather, the region 0 < R < 1/ω) by the Langevin congruence, which is a three-dimensional topological manifold. Even better, we can place a Riemannian metric on this quotient manifold, turning it into a three-dimensional Riemannian manifold, in such a way that the metric has a simple operational significance.

To see this, consider the Born line element

${\displaystyle \mathrm {d} s^{2}=-(1-\omega ^{2}\,r^{2})\,\mathrm {d} t^{2}+2\,\omega \,r^{2}\,\mathrm {d} t\,\mathrm {d} \phi +\mathrm {d} z^{2}+\mathrm {d} r^{2}+r^{2}\,\mathrm {d} \phi ^{2},}$

${\displaystyle -\infty <t,z<\infty ,\;\;0<r<{\frac {1}{\omega }},\;\;-\pi <\phi <\pi .}$

Setting ds² = 0 and solving for dt we obtain

${\displaystyle \mathrm {d} t_{+}={\frac {\omega \,r^{2}\,\mathrm {d} \phi +{\sqrt {(1-\omega ^{2}\,r^{2})\;(\mathrm {d} z^{2}+\mathrm {d} r^{2})+r^{2}\,\mathrm {d} \phi ^{2}}}}{1-\omega ^{2}\,r^{2}}},}$

${\displaystyle \mathrm {d} t_{-}={\frac {\omega \,r^{2}\,\mathrm {d} \phi -{\sqrt {(1-\omega ^{2}\,r^{2})\;(\mathrm {d} z^{2}+\mathrm {d} r^{2})+r^{2}\,\mathrm {d} \phi ^{2}}}}{1-\omega ^{2}\,r^{2}}}.}$

The elapsed proper time for a roundtrip radar blip emitted by a Langevin observer is then

${\displaystyle {\sqrt {1-\omega ^{2}\,r^{2}}}\;{\frac {\mathrm {d} t_{+}-\mathrm {d} t_{-}}{2}}={\sqrt {\mathrm {d} z^{2}+\mathrm {d} r^{2}+{\frac {r^{2}\,\mathrm {d} \phi ^{2}}{1-\omega ^{2}\,r^{2}}}}}.}$

Therefore, in our quotient manifold, the Riemannian line element

${\displaystyle \mathrm {d} \sigma ^{2}=\mathrm {d} z^{2}+\mathrm {d} r^{2}+{\frac {r^{2}\,\mathrm {d} \phi ^{2}}{1-\omega ^{2}\,r^{2}}},}$

${\displaystyle -\infty <t<\infty ,\;\;0<r<{\frac {1}{\omega }},\;\;-\pi <\phi <\pi }$

corresponds to distance between infinitesimally nearby Langevin observers. We will call it the Langevin-Landau-Lifschitz metric, and we can call this notion of distance radar distance "in the small".

This metric was first given by Langevin, but the interpretation in terms of radar distance "in the small" is due to Lev Landau and Evgeny Lifshitz, who generalized the construction to work for the quotient of any Lorentzian manifold by a stationary timelike congruence.

If we adopt the coframe

${\displaystyle \theta ^{\hat {1}}=\mathrm {d} z,\;\;\theta ^{\hat {2}}=\mathrm {d} r,\;\;\theta ^{\hat {3}}={\frac {r\,\mathrm {d} \phi }{\sqrt {1-\omega ^{2}\,r^{2}}}}}$

we can easily compute the Riemannian curvature tensor of our three-dimensional quotient manifold. It has only two independent nontrivial components,

${\displaystyle {R^{\hat {2}}}_{{\hat {3}}{\hat {2}}{\hat {3}}}={\frac {-3\,\omega ^{2}}{(1-\omega ^{2}r^{2})^{2}}}=-3\,\omega ^{2}+O(\omega ^{4}\,r^{2}),}$

${\displaystyle {R^{\hat {3}}}_{{\hat {2}}{\hat {3}}{\hat {2}}}={\frac {-3\,\omega ^{2}\,r^{2}}{(1-\omega ^{2}r^{2})^{3}}}=-3\,\omega ^{2}\,r^{2}+O(\omega ^{4}\,r^{4}).}$

Thus, in some sense, the geometry of a rotating disk is curved, as Theodor Kaluza claimed (without proof) as early as 1910. In fact, to second order in ω it has the geometry of the hyperbolic plane, just as Kaluza claimed.

Warning: as we have seen, there are many possible notions of distance which can be employed by Langevin observers riding on a rigidly rotating disk, so statements referring to "the geometry of a rotating disk" always require careful qualification.

To drive home this important point, let us use the Landau-Lifschitz metric to compute the distance between a Langevin observer riding a ring with radius R₀ and a central static observer. To do this, we need only integrate our line element over the appropriate null geodesic track. From our earlier work, we see that we must plug

${\displaystyle \mathrm {d} r={\frac {\mathrm {d} \phi }{\omega }},\,\mathrm {d} z=0}$

into our line element and integrate

${\displaystyle \int _{0}^{\Delta }\mathrm {d} \sigma =\int \limits _{0}^{r_{0}}{\left(1+{\frac {\omega ^{2}r^{2}}{1-\omega ^{2}r^{2}}}\right)^{\frac {1}{2}}}\,\mathrm {d} r.}$

This gives

${\displaystyle \Delta =\int _{0}^{r_{0}}{\frac {\mathrm {d} r}{\sqrt {1-\omega ^{2}\,r^{2}}}}={\frac {\arcsin(\omega r_{0})}{\omega }}=r_{0}+{\frac {\omega ^{2}\,r_{0}^{3}}{6}}+O(r_{0}^{5}).}$

Because we are now dealing with a Riemannian metric, this notion of distance is of course symmetric under interchanging the two observers, unlike radar distance "in the large". The values given by this notion are in contradiction to the radar distances "in the large" computed in the previous section. Also, because up to second order the Landau-Lifschitz metric agrees with the Einstein synchronization convention, we see that the curvature tensor we just computed does have operational significance: while radar distance "in the large" between pairs of Langevin observers is certainly not a Riemannian notion of distance, the distance between pairs of nearby Langevin observers does correspond to a Riemannian distance, given by the Langevin-Landau-Lifschitz metric. (In the felicitous phrase of Howard Percy Robertson, this is kinematics im Kleinen.)

One way to see that all reasonable notions of spatial distance for our Langevin observers agree for nearby observers is to show, following Nathan Rosen, that for any one Langevin observer, an instantaneously co-moving inertial observer will also obtain the distances given by the Langevin-Landau-Lifschitz metric, for very small distances.

• Ehrenfest paradox, for a sometimes controversial topic often studied using the Born chart.
• Fibre optic gyroscope
• Rindler coordinates, for another useful coordinate chart adapted to another important family of accelerated observers in Minkowski spacetime; this article also emphasizes the existence of distinct notions of distance which may be employed by such observers.
• Sagnac effect

A few papers of historical interest:

• Born, M. (1909). "Die Theorie des starren Elektrons in der Kinematik des Relativitäts-Prinzipes". Ann. Phys. 30 (11): 1–56. Bibcode:1909AnP...335....1B. doi:10.1002/andp.19093351102.
  • Wikisource translation: The Theory of the Rigid Electron in the Kinematics of the Principle of Relativity
• Ehrenfest, P. (1909). "Gleichförmige Rotation starrer Körper und Relativitätstheorie". Phys. Z. 10: 918. Bibcode:1909PhyZ...10..918E.
  • Wikisource translation: Uniform Rotation of Rigid Bodies and the Theory of Relativity
• Langevin, P. (1935). "Remarques au sujet de la Note de Prunier". C. R. Acad. Sci. Paris. 200: 48.

A few classic references:

• Grøn, Ø. (1975). "Relativistic description of a rotating disk". Am. J. Phys. 43 (10): 869–876. Bibcode:1975AmJPh..43..869G. doi:10.1119/1.9969.
• Landau, L. D. & Lifschitz, E. M. (1980). The Classical Theory of Fields (4th ed.). London: Butterworth-Heinemann. ISBN 0-7506-2768-9. See Section 84 for the Landau-Lifschitz metric on the quotient of a Lorentzian manifold by a stationary congruence; see the problem at the end of Section 89 for the application to Langevin observers.

Selected recent sources:

• Rizzi, G. & Ruggiero, M. L. (2004). Relativity in Rotating Frames. Dordrecht: Kluwer. ISBN 1-4020-1805-3. This book contains a valuable historical survey by Øyvind Grøn and some other papers on the Ehrenfest paradox and related controversies and a paper by Lluis Bel discussing the Langevin congruence. Hundreds of additional references may be found in this book.
• Pauri, Massimo & Vallisneri, Michele (2000). "Märzke-Wheeler coordinates for accelerated observers in special relativity". Found. Phys. Lett. 13 (5): 401–425. Bibcode:2000gr.qc.....6095P. doi:10.1023/A:1007861914639. S2CID 15097773. Studies a coordinate chart constructed using radar distance "in the large" from a single Langevin observer. See also the eprint version.

• The Rigid Rotating Disk in Relativity, by Michael Weiss (1995), from the sci.physics FAQ.