### Kruskal–Szekeres coordinates

In general relativity **Kruskal–Szekeres coordinates**, named for Martin Kruskal and George Szekeres, are a coordinate system for the Schwarzschild geometry for a black hole. These coordinates have the advantage that they cover the entire spacetime manifold of the maximally extended Schwarzschild solution and are well-behaved everywhere outside the physical singularity.

## Contents

## Definition

Kruskal–Szekeres coordinates are defined, from the Schwarzschild coordinates $(t,r,\backslash theta,\backslash phi)$, by replacing *t* and *r* by a new time coordinate V and a new spatial coordinate U:

- $V\; =\; \backslash left(\backslash frac\{r\}\{2GM\}\; -\; 1\backslash right)^\{1/2\}e^\{r/4GM\}\backslash sinh\backslash left(\backslash frac\{t\}\{4GM\}\backslash right)$
- $U\; =\; \backslash left(\backslash frac\{r\}\{2GM\}\; -\; 1\backslash right)^\{1/2\}e^\{r/4GM\}\backslash cosh\backslash left(\backslash frac\{t\}\{4GM\}\backslash right)$

for the exterior region $r>2GM$, and:

- $V\; =\; \backslash left(1\; -\; \backslash frac\{r\}\{2GM\}\backslash right)^\{1/2\}e^\{r/4GM\}\backslash cosh\backslash left(\backslash frac\{t\}\{4GM\}\backslash right)$
- $U\; =\; \backslash left(1\; -\; \backslash frac\{r\}\{2GM\}\backslash right)^\{1/2\}e^\{r/4GM\}\backslash sinh\backslash left(\backslash frac\{t\}\{4GM\}\backslash right)$

for the interior region $02gm\; math>.\; Note$*GM* is the gravitational constant multiplied with the Schwarzschild mass parameter, and this article is using units where *c* = 1.

It follows that the Schwarzschild *r*, in terms of Kruskal–Szekeres coordinates, is implicitly given by:

- $V^2\; -\; U^2\; =\; \backslash left(1-\backslash frac\{r\}\{2GM\}\backslash right)e^\{r/2GM\}$

or using the Lambert W function as:

- $\backslash frac\{r\}\{2GM\}\; =\; 1\; +\; W\; \backslash left(\; \backslash frac\{U^2\; -\; V^2\}\{e\}\; \backslash right)$.

In these new coordinates the metric of the Schwarzschild black hole manifold is given by

- $ds^\{2\}\; =\; \backslash frac\{32G^3M^3\}\{r\}e^\{-r/2GM\}(-dV^2\; +\; dU^2)\; +\; r^2\; d\backslash Omega^2,$

written using the (− + + +) metric signature convention and where the angular component of the metric (the line element of the 2-sphere) is:

- $d\backslash Omega^2\backslash \; \backslash stackrel\{\backslash mathrm\{def\}\}\{=\}\backslash \; d\backslash theta^2+\backslash sin^2\backslash theta\backslash ,d\backslash phi^2$

The location of the event horizon (*r* = 2*GM*) in these coordinates is given by $V\; =\; \backslash plusmn\; U\backslash ,$. Note that the metric is perfectly well defined and non-singular at the event horizon.

## The maximally extended Schwarzschild solution

The transformation between Schwarzschild coordinates and Kruskal–Szekeres coordinates is defined for *r* > *2GM*, and −∞ < *t* < ∞, which is the range for which the Schwarzschild coordinates make sense. However in this region, *r* is an analytic function of *V* and *U* and can be extended, as an analytic function at least to the first singularity which occurs at *V^2-U^2=1*. Thus the above metric is a solution of Einstein's equations throughout this region. The allowed values are

- $-\backslash infty\; <\; U\; <\; \backslash infty\backslash ,$
- $V^2\; -\; U^2\; <\; 1.\backslash ,$

Note that this extension assumes that the solution is analytic everywhere.

In the maximally extended solution there are actually two singularities at *r* = 0, one for positive *V* and one for negative *V*. The negative *V* singularity is the time-reversed black hole, sometimes dubbed a *white hole*. Particles can escape from a white hole but they can never return.

The maximally extended Schwarzschild geometry can be divided into 4 regions each of which can be covered by a suitable set of Schwarzschild coordinates. The Kruskal–Szekeres coordinates, on the other hand, cover the entire spacetime manifold. The four regions are separated by event horizons.

I | exterior region | $V^2\; -\; U^2\; <\; 0$ and $U\; >\; 0$ | $2GM\; <\; r$ |
---|---|---|---|

II | interior black hole | $0\; <\; V^2\; -\; U^2\; <\; 1$ and $V\; >\; 0$ | $0\; <\; r\; <\; 2GM$ |

III | parallel exterior region | $V^2\; -\; U^2\; <\; 0$ and $U\; <\; 0$ | $2GM\; <\; r$ |

IV | interior white hole | $0\; <\; V^2\; -\; U^2\; <\; 1$ and $V\; <\; 0$ | $0\; <\; r\; <\; 2GM$ |

The transformation given above between Schwarzschild and Kruskal–Szekeres coordinates applies only in regions I and II. A similar transformation can be written down in the other two regions.

The Schwarzschild time coordinate *t* is given by

- $\backslash tanh\backslash left(\backslash frac\{t\}\{4GM\}\backslash right)\; =$

\begin{cases}V/U & \mbox{(in I and III)} \\ U/V & \mbox{(in II and IV)}\end{cases} In each region it runs from −∞ to +∞ with the infinities at the event horizons.

## Qualitative features of the Kruskal-Szekeres diagram

Kruskal–Szekeres coordinates have a number of useful features which make them helpful for building intuitions about the Schwarzschild spacetime. Chief among these is the fact that all radial light-like geodesics (the world lines of light rays moving in a radial direction) look like straight lines at a 45-degree angle when drawn in a Kruskal-Szekeres diagram (this can be derived from the metric equation given above, which guarantees that if $dU\; =\; \backslash plusmn\; dV\backslash ,$ then $ds\; =\; 0$).^{[1]} All timelike world lines of slower-than-light objects will at every point have a slope closer to the vertical time axis (the V coordinate) than 45 degrees. So, a light cone drawn in a Kruskal-Szekeres diagram will look just the same as a light cone in a Minkowski diagram in special relativity.

The event horizons bounding the black hole and white hole interior regions are also a pair of straight lines at 45 degrees, reflecting the fact that a light ray emitted at the horizon in a radial direction (aimed outward in the case of the black hole, inward in the case of the white hole) would remain on the horizon forever. Thus the two black hole horizons coincide with the boundaries of the future light cone of an event at the center of the diagram (at U=0 and V=0), while the two white hole horizons coincide with the boundaries of the past light cone of this same event. Any event inside the black hole interior region will have a future light cone that remains in this region (such that any world line within the event's future light cone will eventually hit the black hole singularity, which appears as a hyperbola bounded by the two black hole horizons), and any event inside the white hole interior region will have a past light cone that remains in this region (such that any world line within this past light cone must have originated in the white hole singularity, a hyperbola bounded by the two white hole horizons). Note that although the horizon looks as though it is an outward expanding cone, the area of this surface, given by *r* is just $16\backslash pi\; M^2$, a constant. Ie, these coordinates can be deceptive if care is not exercised.

It may be instructive to consider what curves of constant *Schwarzschild* coordinate would look like when plotted on a Kruskal-Szekeres diagram. It turns out that curves of constant r-coordinate in Schwarzschild coordinates always look like hyperbolas bounded by a pair of event horizons at 45 degrees, while lines of constant t-coordinate in Schwarzchild coordinates always look like straight lines at various angles passing through the center of the diagram. The black hole event horizon bordering exterior region I would coincide with a Schwarzschild t-coordinate of +∞ while the white hole event horizon bordering this region would coincide with a Schwarzschild t-coordinate of −∞, reflecting the fact that in Schwarzschild coordinates an infalling particle takes an infinite coordinate time to reach the horizon (i.e. the particle's distance from the horizon approaches zero as the Schwarzschild t-coordinate approaches infinity), and a particle traveling up away from the horizon must have crossed it an infinite coordinate time in the past. This is just an artifact of how Schwarzschild coordinates are defined; a free-falling particle will only take a finite proper time (time as measured by its own clock) to pass between an outside observer and an event horizon, and if the particle's world line is drawn in the Kruskal-Szekeres diagram this will also only take a finite coordinate time in Kruskal–Szekeres coordinates.

The Schwarzschild coordinate system can only cover a single exterior region and a single interior region, such as regions I and II in the Kruskal-Szekeres diagram. The Kruskal-Szekeres coordinate system, on the other hand, can cover a "maximally extended" spacetime which includes the region covered by Schwarzschild coordinates. Here, "maximally extended" refers to the idea that the spacetime should not have any "edges": any geodesic path can be extended arbitrarily far in either direction unless it runs into a gravitational singularity. Technically, this means that a maximally extended spacetime is either "geodesically complete" (meaning any geodesic can be extended to arbitrarily large positive or negative values of its 'affine parameter',^{[2]} which in the case of a timelike geodesic could just be the proper time), or if any geodesics are incomplete, it can only be because they end at a singularity.^{[3]}^{[4]} In order to satisfy this requirement, it was found that in addition to the black hole interior region (region II) which particles enter when they fall through the event horizon from the exterior (region I), there has to be a separate white hole interior region (region IV) which allows us to extend the trajectories of particles which an outside observer sees rising up *away* from the event horizon, along with a separate exterior region (region III) which allows us to extend some possible particle trajectories in the two interior regions. There are actually multiple possible ways to extend the exterior Schwarzschild solution into a maximally extended spacetime, but the Kruskal-Szekeres extension is unique in that it is a maximal, analytic, simply connected vacuum solution in which all maximally extended geodesics are either complete or else the curvature scalar diverges along them in finite affine time.^{[5]}

## Lightcone variant

In the literature the Kruskal–Szekeres coordinates sometimes also appear in their lightcone variant:

- $\backslash tilde\{U\}\; =\; V\; -\; U$
- $\backslash tilde\{V\}\; =\; V\; +\; U,$

in which the metric is given by

- $ds^\{2\}\; =\; -\backslash frac\{32G^3M^3\}\{r\}e^\{-r/2GM\}(d\backslash tilde\{U\}\; d\backslash tilde\{V\})\; +\; r^2\; d\backslash Omega^2,$

and *r* is defined implicitly by the equation

- $\backslash tilde\{U\}\; \backslash tilde\{V\}\; =\; \backslash left(1-\backslash frac\{r\}\{2GM\}\backslash right)e^\{r/2GM\}.$

(some sources use an alternate notation where the regular Kruskal–Szekeres coordinates are labeled T and R instead of V and U, and the Kruskal-Szekeres lightcone coordinates are labeled u and v rather than $\backslash tilde\{U\}$ and $\backslash tilde\{V\}$)^{[6]}

These lightcone coordinates have the useful feature that outgoing null geodesics are given by $\backslash tilde\{U\}\; =\; \backslash text\{constant\}$, while ingoing null geodesics are given by $\backslash tilde\{V\}\; =\; \backslash text\{constant\}$. Furthermore, the (future and past) event horizon(s) are given by the equation $\backslash tilde\{U\}\; \backslash tilde\{V\}\; =\; 0$, and curvature singularity is given by the equation $\backslash tilde\{U\}\; \backslash tilde\{V\}\; =\; 1$.

The lightcone coordinates derive closely from Eddington-Finkelstein coordinates.^{[7]}

## See also

- Schwarzschild coordinates
- Eddington-Finkelstein coordinates
- Isotropic coordinates
- Gullstrand-Painlevé coordinates