# Kruskal-Szekeres coordinates

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.

Definition

"Conventions": In this article we will take the metric signature to be (− + + +) and we will work in units where "c" = 1. The gravitational constant "G" will be kept explicit. We will denote the characteristic mass of the Schwarzschild geometry by "M".

Recall that in Schwarzschild coordinates $\left(t,r, heta,phi\right)$, the Schwarzschild metric is given by:$ds^\left\{2\right\} = -left\left(1-frac\left\{2GM\right\}\left\{r\right\} ight\right) dt^2 + left\left(1-frac\left\{2GM\right\}\left\{r\right\} ight\right)^\left\{-1\right\}dr^2+ r^2 dOmega^2$,where:$dOmega^2 stackrel\left\{mathrm\left\{def\left\{=\right\} d heta^2+sin^2 heta,dphi^2$is the line element of the 2-sphere $S^2.$

Kruskal-Szekeres coordinates are defined by replacing "t" and "r" by new time and radial coordinates::$T = left\left(frac\left\{r\right\}\left\{2GM\right\} - 1 ight\right)^\left\{1/2\right\}e^\left\{r/4GM\right\}sinhleft\left(frac\left\{t\right\}\left\{4GM\right\} ight\right)$:$R = left\left(frac\left\{r\right\}\left\{2GM\right\} - 1 ight\right)^\left\{1/2\right\}e^\left\{r/4GM\right\}coshleft\left(frac\left\{t\right\}\left\{4GM\right\} ight\right)$for the exterior region $r>2GM$, and::$T = left\left(1 - frac\left\{r\right\}\left\{2GM\right\} ight\right)^\left\{1/2\right\}e^\left\{r/4GM\right\}coshleft\left(frac\left\{t\right\}\left\{4GM\right\} ight\right)$:$R = left\left(1 - frac\left\{r\right\}\left\{2GM\right\} ight\right)^\left\{1/2\right\}e^\left\{r/4GM\right\}sinhleft\left(frac\left\{t\right\}\left\{4GM\right\} ight\right)$for the interior region

In these coordinates the metric is given by:$ds^\left\{2\right\} = frac\left\{32G^3M^3\right\}\left\{r\right\}e^\left\{-r/2GM\right\}\left(-dT^2 + dR^2\right) + r^2 dOmega^2,$where "r" is defined implicitly by the equation:$T^2 - R^2 = left\left(1-frac\left\{r\right\}\left\{2GM\right\} ight\right)e^\left\{r/2GM\right\}$or equivalently by:$frac\left\{r\right\}\left\{2GM\right\} = 1 + W left\left( frac\left\{R^2 - T^2\right\}\left\{e\right\} ight\right)$where "W" is the Lambert W function.

The location of the event horizon ("r" = 2"GM") in these coordinates is given by:$T = plusmn R,$Note that the metric is perfectly well-defined and non-singular at the event horizon.

In the literature the Kruskal-Szekers coordinates sometimes also appear in their lightcone variant:: $U = T - R$: $V = T + R,$in which the metric is given by:$ds^\left\{2\right\} = -frac\left\{32G^3M^3\right\}\left\{r\right\}e^\left\{-r/2GM\right\}\left(dU dV\right) + r^2 dOmega^2,$and "r" is defined implicitly by the equation:$U V = left\left(1-frac\left\{r\right\}\left\{2GM\right\} ight\right)e^\left\{r/2GM\right\}.$These coordinates have the useful feature that outgoing null geodesics are given by $U = constant$, while ingoing null geodesics are given by $V = constant$. Furthermore, the (future and past) eventhorizon(s) are given by the equation $U V = 0$, and curvature singularity is given by the equation $U V = 1$.

The maximally extended Schwarzschild solution

The transformation between Schwarzschild coordinates and Kruskal-Szekeres coordinates is defined for "r" &gt; 0, "r" ≠ 2"GM", and −∞ &lt; "t" &lt; ∞, which is the range for which the Schwarzschild coordinates make sense. However, the coordinates ("T", "R") can be extended over every value possible without hitting the physical singularity. The allowed values are:$-infty < R < infty,$:$T^2 - R^2 < 1.,$

In the maximally extended solution there are actually two singularites at "r" = 0, one for positive "T" and one for negative "T". The negative "T" 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. TheKruskal-Szekeres coordinates, on the other hand, cover the entire spacetime manifold. The four regions are separated by event horizons.

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:In each region it runs from −∞ to +∞ with the infinities at the event horizons.

ee also

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

Wikimedia Foundation. 2010.

### Look at other dictionaries:

• George Szekeres — Infobox Scientist name = George Szekeres |300px image width = 300px caption = George Szekeres, 2001 birth date = birth date|1911|5|29|mf=y birth place = Budapest, Hungary death date = death date and age|2005|8|28|1911|5|29|mf=y death place =… …   Wikipedia

• Martin David Kruskal — Born September 28, 1925(1925 09 28) New York City …   Wikipedia

• Gullstrand-Painlevé coordinates — GullStrand Painlevé (GP) coordinates were proposed by Paul Painlevé [Paul Painlevé, “La mécanique classique et la théorie de la relativité”, C. R. Acad. Sci. (Paris) 173, 677–680 (1921). ] and Allvar Gullstrand [Allvar Gullstrand, “Allgemeine… …   Wikipedia

• Eddington-Finkelstein coordinates — In general relativity Eddington Finkelstein coordinates, named for Arthur Stanley Eddington and David Finkelstein, are a pair of coordinate systems for a Schwarzschild geometry which are adapted to radial null geodesics (i.e. the worldlines of… …   Wikipedia

• Schwarzschild coordinates — In the theory of Lorentzian manifolds, spherically symmetric spacetimes admit a family of nested round spheres . In such a spacetime, a particularly important kind of coordinate chart is the Schwarzschild chart, a kind of polar spherical… …   Wikipedia

• Golden age of general relativity — The Golden Age of General Relativity is the period roughly from 1960 to 1975 during which the study of general relativity, which had previously been regarded as something of a curiosity, entered the mainstream of theoretical physics. During this… …   Wikipedia

• Schwarzschild metric — In Einstein s theory of general relativity, the Schwarzschild solution (or the Schwarzschild vacuum) describes the gravitational field outside a spherical, non rotating mass such as a (non rotating) star, planet, or black hole. It is also a good… …   Wikipedia

• Black hole — For other uses, see Black hole (disambiguation). Simulated view of a black hole (center) in front of the Large Magellanic Cloud. Note the gravitat …   Wikipedia

• Metric tensor (general relativity) — This article is about metrics in general relativity. For a discussion of metrics in general, see metric tensor. Metric tensor of spacetime in general relativity written as a matrix. In general relativity, the metric tensor (or simply, the metric) …   Wikipedia

• Penrose diagram — For the tensor diagram notation, see Penrose graphical notation. In theoretical physics, a Penrose diagram (named for mathematical physicist Roger Penrose) is a two dimensional diagram that captures the causal relations between different points… …   Wikipedia