Weyl metrics explained

In general relativity, the Weyl metrics (named after the German-American mathematician Hermann Weyl)^[1] are a class of static and axisymmetric solutions to Einstein's field equation. Three members in the renowned Kerr–Newman family solutions, namely the Schwarzschild, nonextremal Reissner–Nordström and extremal Reissner–Nordström metrics, can be identified as Weyl-type metrics.

Standard Weyl metrics

The Weyl class of solutions has the generic form^{[2] [3]} where

\psi(\rho,z) and \gamma(\rho,z) are two metric potentials dependent on Weyl's canonical coordinates \{\rho,z \} . The coordinate system \{t,\rho,z,\phi\} serves best for symmetries of Weyl's spacetime (with two Killing vector fields being \xi ^{t = \partial} _{t} and \xi ^{\phi=} \partial _{\phi} ) and often acts like cylindrical coordinates, but is incomplete when describing a black hole as \{\rho,z \} only cover the horizon and its exteriors.T _{ab} , we just need to substitute the Weyl metric Eq(1) into Einstein's equation (with c=G=1):and work out the two functions \psi(\rho,z) and \gamma(\rho,z) .

Reduced field equations for electrovac Weyl solutions

One of the best investigated and most useful Weyl solutions is the electrovac case, where

T _{ab} comes from the existence of (Weyl-type) electromagnetic field (without matter and current flows). As we know, given the electromagnetic four-potential A _{a} , the anti-symmetric electromagnetic field F _{ab} and the trace-free stress–energy tensor T _{ab} (T = g ^{ab} T _{ab} =0 ) will be respectively determined bywhich respects the source-free covariant Maxwell equations:Eq(5.a) can be simplified to:in the calculations as \Gamma ^{a} _{bc} = \Gamma ^{a} _{cb} . Also, since R =-8 \pi T =0 for electrovacuum, Eq(2) reduces to

Now, suppose the Weyl-type axisymmetric electrostatic potential is

A _{a=\Phi(\rho,z)[dt]} _{a} (the component \Phi is actually the electromagnetic scalar potential), and together with the Weyl metric Eq(1), Eqs(3)(4)(5)(6) imply that

where

R =0 yields Eq(7.a), R _{tt} =8 \pi T _{tt} or R _{\varphi\varphi} =8 \pi T _{\varphi\varphi} yields Eq(7.b), R _{\rho\rho} =8 \pi T _{\rho\rho} or R _{zz} =8 \pi T _{zz} yields Eq(7.c), R _{\rho} =8 \pi T _{\rho} yields Eq(7.d), and Eq(5.b) yields Eq(7.e). Here \nabla ^{2} = \partial _{\rho\rho} + (1)/(\rho) \partial _{\rho} + \partial _{zz} and \nabla = \partial _{\rho} \hat{e} _{\rho} + \partial _{z} \hat{e} _{z} are respectively the Laplace and gradient operators. Moreover, if we suppose \psi = \psi(\Phi) in the sense of matter-geometry interplay and assume asymptotic flatness, we will find that Eqs(7.a-e) implies a characteristic relation that

Specifically in the simplest vacuum case with

\Phi =0 and T _{ab} =0 , Eqs(7.a-7.e) reduce to^[4]

We can firstly obtain

\psi(\rho,z) by solving Eq(8.b), and then integrate Eq(8.c) and Eq(8.d) for \gamma(\rho,z) . Practically, Eq(8.a) arising from R =0 just works as a consistency relation or integrability condition.

Unlike the nonlinear Poisson's equation Eq(7.b), Eq(8.b) is the linear Laplace equation; that is to say, superposition of given vacuum solutions to Eq(8.b) is still a solution. This fact has a widely application, such as to analytically distort a Schwarzschild black hole.

We employed the axisymmetric Laplace and gradient operators to write Eqs(7.a-7.e) and Eqs(8.a-8.d) in a compact way, which is very useful in the derivation of the characteristic relation Eq(7.f). In the literature, Eqs(7.a-7.e) and Eqs(8.a-8.d) are often written in the following forms as well:

and

Considering the interplay between spacetime geometry and energy-matter distributions, it is natural to assume that in Eqs(7.a-7.e) the metric function

\psi(\rho,z) relates with the electrostatic scalar potential \Phi(\rho,z) via a function \psi = \psi(\Phi) (which means geometry depends on energy), and it follows that

Eq(B.1) immediately turns Eq(7.b) and Eq(7.e) respectively intowhich give rise to

Now replace the variable

\psi by \zeta: = e ^{2\psi} , and Eq(B.4) is simplified to

Direct quadrature of Eq(B.5) yields

\zeta = e ^{2\psi} = \Phi ^{2+\tilde{C}\Phi+B} , with \{B, \tilde{C}\} being integral constants. To resume asymptotic flatness at spatial infinity, we need \lim _{\rho,z\toinfty} \Phi =0 and \lim _{\rho,z\toinfty} e ^{2\psi} =1 , so there should be B =1 . Also, rewrite the constant \tilde{C} as -2 C for mathematical convenience in subsequent calculations, and one finally obtains the characteristic relation implied by Eqs(7.a-7.e) that

This relation is important in linearize the Eqs(7.a-7.f) and superpose electrovac Weyl solutions.

Newtonian analogue of metric potential Ψ(ρ,z)

In Weyl's metric Eq(1), $e^=\backslash sum\_^\; \backslash frac$; thus in the approximation for weak field limit

\psi\to 0 , one hasand therefore

This is pretty analogous to the well-known approximate metric for static and weak gravitational fields generated by low-mass celestial bodies like the Sun and Earth,^[5] where

\Phi _{N} (\rho,z) is the usual Newtonian potential satisfying Poisson's equation \nabla ^{2} _{L} \Phi _{N} =4 \pi\varrho _{N} , just like Eq(3.a) or Eq(4.a) for the Weyl metric potential \psi(\rho,z) . The similarities between \psi(\rho,z) and \Phi _{N} (\rho,z) inspire people to find out the Newtonian analogue of \psi(\rho,z) when studying Weyl class of solutions; that is, to reproduce \psi(\rho,z) nonrelativistically by certain type of Newtonian sources. The Newtonian analogue of \psi(\rho,z) proves quite helpful in specifying particular Weyl-type solutions and extending existing Weyl-type solutions.

Schwarzschild solution

The Weyl potentials generating Schwarzschild's metric as solutions to the vacuum equations Eq are given bywhere

From the perspective of Newtonian analogue,

\psi _{SS} equals the gravitational potential produced by a rod of mass M and length 2 M placed symmetrically on the z -axis; that is, by a line mass of uniform density \sigma =1 / 2 embedded the interval z\in[ - M,M] . (Note: Based on this analogue, important extensions of the Schwarzschild metric have been developed, as discussed in ref.)

Given

\psi _{SS} and \gamma _{SS} , Weyl's metric Eq becomesand after substituting the following mutually consistent relationsone can obtain the common form of Schwarzschild metric in the usual \{t,r,\theta,\phi\} coordinates,

The metric Eq cannot be directly transformed into Eq by performing the standard cylindrical-spherical transformation

(t,\rho,z,\phi) = (t,r\sin\theta,r\cos\theta,\phi) , because \{t,r,\theta,\phi\} is complete while (t,\rho,z,\phi) is incomplete. This is why we call \{t,\rho,z,\phi\} in Eq as Weyl's canonical coordinates rather than cylindrical coordinates, although they have a lot in common; for example, the Laplacian \nabla ^{2:=} \partial _{\rho\rho} + (1)/(\rho) \partial _{\rho} + \partial _{zz} in Eq is exactly the two-dimensional geometric Laplacian in cylindrical coordinates.

Nonextremal Reissner–Nordström solution

The Weyl potentials generating the nonextremal Reissner–Nordström solution (

M>|Q| ) as solutions to Eqs are given bywhere

Thus, given

\psi _{RN} and \gamma _{RN} , Weyl's metric becomesand employing the following transformationsone can obtain the common form of non-extremal Reissner–Nordström metric in the usual \{t,r,\theta,\phi\} coordinates,

Extremal Reissner–Nordström solution

The potentials generating the extremal Reissner–Nordström solution (

M = |Q| ) as solutions to Eqs are given by (Note: We treat the extremal solution separately because it is much more than the degenerate state of the nonextremal counterpart.)

Thus, the extremal Reissner–Nordström metric readsand by substitutingwe obtain the extremal Reissner–Nordström metric in the usual

\{t,r,\theta,\phi\} coordinates,

Mathematically, the extremal Reissner–Nordström can be obtained by taking the limit

Q\to M of the corresponding nonextremal equation, and in the meantime we need to use the L'Hospital rule sometimes.

Remarks: Weyl's metrics Eq with the vanishing potential

\gamma(\rho,z) (like the extremal Reissner–Nordström metric) constitute a special subclass which have only one metric potential \psi(\rho,z) to be identified. Extending this subclass by canceling the restriction of axisymmetry, one obtains another useful class of solutions (still using Weyl's coordinates), namely the conformastatic metrics,^{[6] [7]} where we use λ in Eq as the single metric function in place of \psi in Eq to emphasize that they are different by axial symmetry (\phi -dependence).

Weyl vacuum solutions in spherical coordinates

Weyl's metric can also be expressed in spherical coordinates thatwhich equals Eq via the coordinate transformation

(t,\rho,z,\phi)\mapsto(t,r\sin\theta,r\cos\theta,\phi) (Note: As shown by Eqs, this transformation is not always applicable.) In the vacuum case, Eq for \psi(r,\theta) becomes

The asymptotically flat solutions to Eq iswhere

P _{n(\cos\theta)} represent Legendre polynomials, and a _{n} are multipole coefficients. The other metric potential \gamma(r,\theta) is given by

See also

• Schwarzschild metric
• Reissner–Nordström metric
• Distorted Schwarzschild metric

Notes and References

1. Weyl, H., "Zur Gravitationstheorie," Ann. der Physik 54 (1917), 117–145.
2. Jeremy Bransom Griffiths, Jiri Podolsky. Exact Space-Times in Einstein's General Relativity. Cambridge: Cambridge University Press, 2009. Chapter 10.
3. Hans Stephani, Dietrich Kramer, Malcolm MacCallum, Cornelius Hoenselaers, Eduard Herlt. Exact Solutions of Einstein's Field Equations. Cambridge: Cambridge University Press, 2003. Chapter 20.
4. R Gautreau, R B Hoffman, A Armenti. Static multiparticle systems in general relativity. IL NUOVO CIMENTO B, 1972, 7(1): 71-98.
5. James B Hartle. Gravity: An Introduction To Einstein's General Relativity. San Francisco: Addison Wesley, 2003. Eq(6.20) transformed into Lorentzian cylindrical coordinates
6. Guillermo A Gonzalez, Antonio C Gutierrez-Pineres, Paolo A Ospina. Finite axisymmetric charged dust disks in conformastatic spacetimes. Physical Review D, 2008, 78(6): 064058. arXiv:0806.4285v1
7. Antonio C Gutierrez-Pineres, Guillermo A Gonzalez, Hernando Quevedo. Conformastatic disk-haloes in Einstein-Maxwell gravity. Physical Review D, 2013, 87(4): 044010. https://arxiv.org/abs/1211.4941v2