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Conformastatic spacetimes

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Class of solutions to Einstein's equation in general relativity

Conformastatic spacetimes refer to a special class of static solutions to Einstein's equation in general relativity.

Introduction

The line element for the conformastatic class of solutions in Weyl's canonical coordinates reads
( 1 ) d s 2 = − e 2 Ψ ( ρ , ϕ , z ) d t 2 + e − 2 Ψ ( ρ , ϕ , z ) ( d ρ 2 + d z 2 + ρ 2 d ϕ 2 ) , {\displaystyle (1)\qquad ds^{2}=-e^{2\Psi (\rho ,\phi ,z)}dt^{2}+e^{-2\Psi (\rho ,\phi ,z)}{\Big (}d\rho ^{2}+dz^{2}+\rho ^{2}d\phi ^{2}{\Big )}\;,}
as a solution to the field equation
( 2 ) R a b − 1 2 R g a b = 8 π T a b . {\displaystyle (2)\qquad R_{ab}-{\frac {1}{2}}Rg_{ab}=8\pi T_{ab}\;.}
Eq(1) has only one metric function Ψ ( ρ , ϕ , z ) {\displaystyle \Psi (\rho ,\phi ,z)} to be identified, and for each concrete Ψ ( ρ , ϕ , z ) {\displaystyle \Psi (\rho ,\phi ,z)} , Eq(1) would yields a specific conformastatic spacetime.

Reduced electrovac field equations

In consistency with the conformastatic geometry Eq(1), the electrostatic field would arise from an electrostatic potential A a {\displaystyle A_{a}} without spatial symmetry:
( 3 ) A a = Φ ( ρ , z , ϕ ) [ d t ] a , {\displaystyle (3)\qquad A_{a}=\Phi (\rho ,z,\phi )_{a}\;,}
which would yield the electromagnetic field tensor F a b {\displaystyle F_{ab}} by
( 4 ) F a b = A b ; a − A a ; b , {\displaystyle (4)\qquad F_{ab}=A_{b\,;a}-A_{a\,;b}\;,}
as well as the corresponding stress–energy tensor by
( 5 ) T a b ( E M ) = 1 4 π ( F a c F b c − 1 4 g a b F c d F c d ) . {\displaystyle (5)\qquad T_{ab}^{(EM)}={\frac {1}{4\pi }}{\Big (}F_{ac}F_{b}^{\;\;c}-{\frac {1}{4}}g_{ab}F_{cd}F^{cd}{\Big )}\;.}

Plug Eq(1) and Eqs(3)(4)(5) into "trace-free" (R=0) Einstein's field equation, and one could obtain the reduced field equations for the metric function Ψ ( ρ , ϕ , z ) {\displaystyle \Psi (\rho ,\phi ,z)} :

( 6 ) ∇ 2 Ψ = e − 2 Ψ ∇ Φ ∇ Φ {\displaystyle (6)\qquad \nabla ^{2}\Psi \,=\,e^{-2\Psi }\,\nabla \Phi \,\nabla \Phi }
( 7 ) Ψ i Ψ j = e − 2 Ψ Φ i Φ j {\displaystyle (7)\qquad \Psi _{i}\Psi _{j}=e^{-2\Psi }\Phi _{i}\Phi _{j}}

where ∇ 2 = ∂ ρ ρ + 1 ρ ∂ ρ + 1 ρ 2 ∂ ϕ ϕ + ∂ z z {\displaystyle \nabla ^{2}=\partial _{\rho \rho }+{\frac {1}{\rho }}\,\partial _{\rho }+{\frac {1}{\rho ^{2}}}\partial _{\phi \phi }+\partial _{zz}} and ∇ = ∂ ρ e ^ ρ + 1 ρ ∂ ϕ e ^ ϕ + ∂ z e ^ z {\displaystyle \nabla =\partial _{\rho }\,{\hat {e}}_{\rho }+{\frac {1}{\rho }}\partial _{\phi }\,{\hat {e}}_{\phi }+\partial _{z}\,{\hat {e}}_{z}} are respectively the generic Laplace and gradient operators. in Eq(7), i , j {\displaystyle i\,,j} run freely over the coordinates [ ρ , z , ϕ ] {\displaystyle } .

Examples

Extremal Reissner–Nordström spacetime

The extremal Reissner–Nordström spacetime is a typical conformastatic solution. In this case, the metric function is identified as

( 8 ) Ψ E R N = ln ⁡ L L + M , L = ρ 2 + z 2 , {\displaystyle (8)\qquad \Psi _{ERN}\,=\,\ln {\frac {L}{L+M}}\;,\quad L={\sqrt {\rho ^{2}+z^{2}}}\;,}

which put Eq(1) into the concrete form

( 9 ) d s 2 = − L 2 ( L + M ) 2 d t 2 + ( L + M ) 2 L 2 ( d ρ 2 + d z 2 + ρ 2 d φ 2 ) . {\displaystyle (9)\qquad ds^{2}=-{\frac {L^{2}}{(L+M)^{2}}}dt^{2}+{\frac {(L+M)^{2}}{L^{2}}}\,{\big (}d\rho ^{2}+dz^{2}+\rho ^{2}d\varphi ^{2}{\big )}\;.}

Applying the transformations

( 10 ) L = r − M , z = ( r − M ) cos ⁡ θ , ρ = ( r − M ) sin ⁡ θ , {\displaystyle (10)\;\;\quad L=r-M\;,\quad z=(r-M)\cos \theta \;,\quad \rho =(r-M)\sin \theta \;,}

one obtains the usual form of the line element of extremal Reissner–Nordström solution,

( 11 ) d s 2 = − ( 1 − M r ) 2 d t 2 + ( 1 − M r ) − 2 d r 2 + r 2 ( d θ 2 + sin 2 ⁡ θ d ϕ 2 ) . {\displaystyle (11)\;\;\quad ds^{2}=-{\Big (}1-{\frac {M}{r}}{\Big )}^{2}dt^{2}+{\Big (}1-{\frac {M}{r}}{\Big )}^{-2}dr^{2}+r^{2}{\Big (}d\theta ^{2}+\sin ^{2}\theta \,d\phi ^{2}{\Big )}\;.}

Charged dust disks

Some conformastatic solutions have been adopted to describe charged dust disks.

Comparison with Weyl spacetimes

Many solutions, such as the extremal Reissner–Nordström solution discussed above, can be treated as either a conformastatic metric or Weyl metric, so it would be helpful to make a comparison between them. The Weyl spacetimes refer to the static, axisymmetric class of solutions to Einstein's equation, whose line element takes the following form (still in Weyl's canonical coordinates):
( 12 ) d s 2 = − e 2 ψ ( ρ , z ) d t 2 + e 2 γ ( ρ , z ) − 2 ψ ( ρ , z ) ( d ρ 2 + d z 2 ) + e − 2 ψ ( ρ , z ) ρ 2 d ϕ 2 . {\displaystyle (12)\;\;\quad ds^{2}=-e^{2\psi (\rho ,z)}dt^{2}+e^{2\gamma (\rho ,z)-2\psi (\rho ,z)}(d\rho ^{2}+dz^{2})+e^{-2\psi (\rho ,z)}\rho ^{2}d\phi ^{2}\,.}
Hence, a Weyl solution become conformastatic if the metric function γ ( ρ , z ) {\displaystyle \gamma (\rho ,z)} vanishes, and the other metric function ψ ( ρ , z ) {\displaystyle \psi (\rho ,z)} drops the axial symmetry:
( 13 ) γ ( ρ , z ) ≡ 0 , ψ ( ρ , z ) ↦ Ψ ( ρ , ϕ , z ) . {\displaystyle (13)\;\;\quad \gamma (\rho ,z)\equiv 0\;,\quad \psi (\rho ,z)\mapsto \Psi (\rho ,\phi ,z)\,.}
The Weyl electrovac field equations would reduce to the following ones with γ ( ρ , z ) {\displaystyle \gamma (\rho ,z)} :

( 14. a ) ∇ 2 ψ = ( ∇ ψ ) 2 {\displaystyle (14.a)\quad \nabla ^{2}\psi =\,(\nabla \psi )^{2}}
( 14. b ) ∇ 2 ψ = e − 2 ψ ( ∇ Φ ) 2 {\displaystyle (14.b)\quad \nabla ^{2}\psi =\,e^{-2\psi }(\nabla \Phi )^{2}}
( 14. c ) ψ , ρ 2 − ψ , z 2 = e − 2 ψ ( Φ , ρ 2 − Φ , z 2 ) {\displaystyle (14.c)\quad \psi _{,\,\rho }^{2}-\psi _{,\,z}^{2}=e^{-2\psi }{\big (}\Phi _{,\,\rho }^{2}-\Phi _{,\,z}^{2}{\big )}}
( 14. d ) 2 ψ , ρ ψ , z = 2 e − 2 ψ Φ , ρ Φ , z {\displaystyle (14.d)\quad 2\psi _{,\,\rho }\psi _{,\,z}=2e^{-2\psi }\Phi _{,\,\rho }\Phi _{,\,z}}
( 14. e ) ∇ 2 Φ = 2 ∇ ψ ∇ Φ , {\displaystyle (14.e)\quad \nabla ^{2}\Phi =\,2\nabla \psi \nabla \Phi \,,}

where ∇ 2 = ∂ ρ ρ + 1 ρ ∂ ρ + ∂ z z {\displaystyle \nabla ^{2}=\partial _{\rho \rho }+{\frac {1}{\rho }}\,\partial _{\rho }+\partial _{zz}} and ∇ = ∂ ρ e ^ ρ + ∂ z e ^ z {\displaystyle \nabla =\partial _{\rho }\,{\hat {e}}_{\rho }+\partial _{z}\,{\hat {e}}_{z}} are respectively the reduced cylindrically symmetric Laplace and gradient operators.

It is also noticeable that, Eqs(14) for Weyl are consistent but not identical with the conformastatic Eqs(6)(7) above.

References

  1. John Lighton Synge. Relativity: The General Theory, Chapter VIII. Amsterdam: North-Holland Publishing Company (Interscience), 1960.
  2. Hans Stephani, Dietrich Kramer, Malcolm MacCallum, Cornelius Hoenselaers, Eduard Herlt . Exact Solutions of Einstein's Field Equations (2nd Edition), Chapter 18. Cambridge: Cambridge University Press, 2003.
  3. ^ Guillermo A Gonzalez, Antonio C Gutierrez-Pineres, Paolo A Ospina. Finite axisymmetric charged dust disks in conformastatic spacetimes. Physical Review D 78 (2008): 064058. arXiv:0806.4285[gr-qc]
  4. ^ F D Lora-Clavijo, P A Ospina-Henao, J F Pedraza. Charged annular disks and Reissner–Nordström type black holes from extremal dust. Physical Review D 82 (2010): 084005. arXiv:1009.1005[gr-qc]
  5. ^ Ivan Booth, David Wenjie Tian. Some spacetimes containing non-rotating extremal isolated horizons. Accepted by Classical and Quantum Gravity. arXiv:1210.6889[gr-qc]
  6. Antonio C Gutierrez-Pineres, Guillermo A Gonzalez, Hernando Quevedo. Conformastatic disk-haloes in Einstein-Maxwell gravity. Physical Review D 87 (2013): 044010. arXiv:1211.4941[gr-qc]

See also

Category: