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Distorted Schwarzschild metric

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In physics, the distorted Schwarzschild metric is the metric of a standard/isolated Schwarzschild spacetime exposed in external fields. In numerical simulation, the Schwarzschild metric can be distorted by almost arbitrary kinds of external energy–momentum distribution. However, in exact analysis, the mature method to distort the standard Schwarzschild metric is restricted to the framework of Weyl metrics.

Standard Schwarzschild as a vacuum Weyl metric

All static axisymmetric solutions of the Einstein–Maxwell equations can be written in the form of Weyl's metric,


( 1 ) 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 (1)\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}\,,}


From the Weyl perspective, the metric potentials generating the standard Schwarzschild solution are given by

( 2 ) ψ S S = 1 2 ln ⁡ L − M L + M , γ S S = 1 2 ln ⁡ L 2 − M 2 l + l − , {\displaystyle (2)\quad \psi _{SS}={\frac {1}{2}}\ln {\frac {L-M}{L+M}}\,,\quad \gamma _{SS}={\frac {1}{2}}\ln {\frac {L^{2}-M^{2}}{l_{+}l_{-}}}\,,}

where

( 3 ) L = 1 2 ( l + + l − ) , l + = ρ 2 + ( z + M ) 2 , l − = ρ 2 + ( z − M ) 2 , {\displaystyle (3)\quad L={\frac {1}{2}}{\big (}l_{+}+l_{-}{\big )}\,,\quad l_{+}={\sqrt {\rho ^{2}+(z+M)^{2}}}\,,\quad l_{-}={\sqrt {\rho ^{2}+(z-M)^{2}}}\,,}

which yields the Schwarzschild metric in Weyl's canonical coordinates that

( 4 ) d s 2 = − L − M L + M d t 2 + ( L + M ) 2 l + l − ( d ρ 2 + d z 2 ) + L + M L − M ρ 2 d ϕ 2 . {\displaystyle (4)\quad ds^{2}=-{\frac {L-M}{L+M}}dt^{2}+{\frac {(L+M)^{2}}{l_{+}l_{-}}}(d\rho ^{2}+dz^{2})+{\frac {L+M}{L-M}}\,\rho ^{2}d\phi ^{2}\,.}

Weyl-distortion of Schwarzschild's metric

Vacuum Weyl spacetimes (such as Schwarzschild) respect the following field equations,

( 5. a ) ∇ 2 ψ = 0 , {\displaystyle (5.a)\quad \nabla ^{2}\psi =0\,,}
( 5. b ) γ , ρ = ρ ( ψ , ρ 2 − ψ , z 2 ) , {\displaystyle (5.b)\quad \gamma _{,\,\rho }=\rho \,{\Big (}\psi _{,\,\rho }^{2}-\psi _{,\,z}^{2}{\Big )}\,,}
( 5. c ) γ , z = 2 ρ ψ , ρ ψ , z , {\displaystyle (5.c)\quad \gamma _{,\,z}=2\,\rho \,\psi _{,\,\rho }\psi _{,\,z}\,,}
( 5. d ) γ , ρ ρ + γ , z z = − ( ψ , ρ 2 + ψ , z 2 ) , {\displaystyle (5.d)\quad \gamma _{,\,\rho \rho }+\gamma _{,\,zz}=-{\big (}\psi _{,\,\rho }^{2}+\psi _{,\,z}^{2}{\big )}\,,}

where ∇ 2 := ∂ ρ ρ + 1 ρ ∂ ρ + ∂ z z {\displaystyle \nabla ^{2}:=\partial _{\rho \rho }+{\frac {1}{\rho }}\partial _{\rho }+\partial _{zz}} is the Laplace operator.

Derivation of vacuum field equations. The vacuum Einstein's equation reads R a b = 0 {\displaystyle R_{ab}=0} , which yields Eqs(5.a)-(5.c).

Moreover, the supplementary relation R = 0 {\displaystyle R=0} implies Eq(5.d). End derivation.

Eq(5.a) is the linear Laplace's equation; that is to say, linear combinations of given solutions are still its solutions. Given two solutions { ψ ⟨ 1 ⟩ , ψ ⟨ 2 ⟩ } {\displaystyle \{\psi ^{\langle 1\rangle },\psi ^{\langle 2\rangle }\}} to Eq(5.a), one can construct a new solution via

( 6 ) ψ ~ = ψ ⟨ 1 ⟩ + ψ ⟨ 2 ⟩ , {\displaystyle (6)\quad {\tilde {\psi }}\,=\,\psi ^{\langle 1\rangle }+\psi ^{\langle 2\rangle }\,,}

and the other metric potential can be obtained by

( 7 ) γ ~ = γ ⟨ 1 ⟩ + γ ⟨ 2 ⟩ + 2 ∫ ρ { ( ψ , ρ ⟨ 1 ⟩ ψ , ρ ⟨ 2 ⟩ − ψ , z ⟨ 1 ⟩ ψ , z ⟨ 2 ⟩ ) d ρ + ( ψ , ρ ⟨ 1 ⟩ ψ , z ⟨ 2 ⟩ + ψ , z ⟨ 1 ⟩ ψ , ρ ⟨ 2 ⟩ ) d z } . {\displaystyle (7)\quad {\tilde {\gamma }}\,=\,\gamma ^{\langle 1\rangle }+\gamma ^{\langle 2\rangle }+2\int \rho \,{\Big \{}\,{\Big (}\psi _{,\,\rho }^{\langle 1\rangle }\psi _{,\,\rho }^{\langle 2\rangle }-\psi _{,\,z}^{\langle 1\rangle }\psi _{,\,z}^{\langle 2\rangle }{\Big )}\,d\rho +{\Big (}\psi _{,\,\rho }^{\langle 1\rangle }\psi _{,\,z}^{\langle 2\rangle }+\psi _{,\,z}^{\langle 1\rangle }\psi _{,\,\rho }^{\langle 2\rangle }{\Big )}\,dz\,{\Big \}}\,.}

Let ψ ⟨ 1 ⟩ = ψ S S {\displaystyle \psi ^{\langle 1\rangle }=\psi _{SS}} and γ ⟨ 1 ⟩ = γ S S {\displaystyle \gamma ^{\langle 1\rangle }=\gamma _{SS}} , while ψ ⟨ 2 ⟩ = ψ {\displaystyle \psi ^{\langle 2\rangle }=\psi } and γ ⟨ 2 ⟩ = γ {\displaystyle \gamma ^{\langle 2\rangle }=\gamma } refer to a second set of Weyl metric potentials. Then, { ψ ~ , γ ~ } {\displaystyle \{{\tilde {\psi }},{\tilde {\gamma }}\}} constructed via Eqs(6)(7) leads to the superposed Schwarzschild-Weyl metric

( 8 ) d s 2 = − e 2 ψ ( ρ , z ) L − M L + M d t 2 + e 2 γ ( ρ , z ) − 2 ψ ( ρ , z ) ( L + M ) 2 l + l − ( d ρ 2 + d z 2 ) + e − 2 ψ ( ρ , z ) L + M L − M ρ 2 d ϕ 2 . {\displaystyle (8)\quad ds^{2}=-e^{2\psi (\rho ,z)}{\frac {L-M}{L+M}}dt^{2}+e^{2\gamma (\rho ,z)-2\psi (\rho ,z)}{\frac {(L+M)^{2}}{l_{+}l_{-}}}(d\rho ^{2}+dz^{2})+e^{-2\psi (\rho ,z)}{\frac {L+M}{L-M}}\,\rho ^{2}d\phi ^{2}\,.}

With the transformations

( 9 ) L + M = r , l + + l − = 2 M cos ⁡ θ , z = ( r − M ) cos ⁡ θ , {\displaystyle (9)\quad L+M=r\,,\quad l_{+}+l_{-}=2M\cos \theta \,,\quad z=(r-M)\cos \theta \,,}
ρ = r 2 − 2 M r sin ⁡ θ , l + l − = ( r − M ) 2 − M 2 cos 2 ⁡ θ , {\displaystyle \;\;\quad \rho ={\sqrt {r^{2}-2Mr}}\,\sin \theta \,,\quad l_{+}l_{-}=(r-M)^{2}-M^{2}\cos ^{2}\theta \,,}

one can obtain the superposed Schwarzschild metric in the usual { t , r , θ , ϕ } {\displaystyle \{t,r,\theta ,\phi \}} coordinates,

( 10 ) d s 2 = − e 2 ψ ( r , θ ) ( 1 − 2 M r ) d t 2 + e 2 γ ( r , θ ) − 2 ψ ( r , θ ) { ( 1 − 2 M r ) − 1 d r 2 + r 2 d θ 2 } + e − 2 ψ ( r , θ ) r 2 sin 2 ⁡ θ d ϕ 2 . {\displaystyle (10)\quad ds^{2}=-e^{2\psi (r,\theta )}\,{\Big (}1-{\frac {2M}{r}}{\Big )}\,dt^{2}+e^{2\gamma (r,\theta )-2\psi (r,\theta )}{\Big \{}\,{\Big (}1-{\frac {2M}{r}}{\Big )}^{-1}dr^{2}+r^{2}d\theta ^{2}\,{\Big \}}+e^{-2\psi (r,\theta )}r^{2}\sin ^{2}\theta \,d\phi ^{2}\,.}

The superposed metric Eq(10) can be regarded as the standard Schwarzschild metric distorted by external Weyl sources. In the absence of distortion potential { ψ ( ρ , z ) = 0 , γ ( ρ , z ) = 0 } {\displaystyle \{\psi (\rho ,z)=0,\gamma (\rho ,z)=0\}} , Eq(10) reduces to the standard Schwarzschild metric

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

Weyl-distorted Schwarzschild solution in spherical coordinates

Similar to the exact vacuum solutions to Weyl's metric in spherical coordinates, we also have series solutions to Eq(10). The distortion potential ψ ( r , θ ) {\displaystyle \psi (r,\theta )} in Eq(10) is given by the multipole expansion

( 12 ) ψ ( r , θ ) = − ∑ i = 1 ∞ a i ( R n ( cos ⁡ θ ) M ) P i {\displaystyle (12)\quad \psi (r,\theta )\,=-\sum _{i=1}^{\infty }a_{i}{\Big (}{\frac {R_{n}(\cos \theta )}{M}}{\Big )}P_{i}} with R := [ ( 1 − 2 M r ) r 2 + M 2 cos 2 ⁡ θ ] 1 / 2 {\displaystyle R:={\Big }^{1/2}}

where

( 13 ) P i := p i ( ( r − m ) cos ⁡ θ R ) {\displaystyle (13)\quad P_{i}:=p_{i}{\Big (}{\frac {(r-m)\cos \theta }{R}}{\Big )}}

denotes the Legendre polynomials and a i {\displaystyle a_{i}} are multipole coefficients. The other potential γ ( r , θ ) {\displaystyle \gamma (r,\theta )} is

( 14 ) γ ( r , θ ) = ∑ i = 1 ∞ ∑ j = 0 ∞ a i a j {\displaystyle (14)\quad \gamma (r,\theta )\,=\sum _{i=1}^{\infty }\sum _{j=0}^{\infty }a_{i}a_{j}} ( i j i + j ) {\displaystyle {\Big (}{\frac {ij}{i+j}}{\Big )}} ( R M ) i + j {\displaystyle {\Big (}{\frac {R}{M}}{\Big )}^{i+j}} ( P i P j − P i − 1 P j − 1 ) {\displaystyle (P_{i}P_{j}-P_{i-1}P_{j-1})} − 1 M ∑ i = 1 ∞ α i ∑ j = 0 i − 1 {\displaystyle -{\frac {1}{M}}\sum _{i=1}^{\infty }\alpha _{i}\sum _{j=0}^{i-1}} [ ( − 1 ) i + j ( r − M ( 1 − cos ⁡ θ ) ) + r − M ( 1 + cos ⁡ θ ) ] {\displaystyle {\Big }} ( R M ) j P j . {\displaystyle {\Big (}{\frac {R}{M}}{\Big )}^{j}P_{j}\,.}

See also

References

  1. ^ Jeremy Bransom Griffiths, Jiri Podolsky. Exact Space-Times in Einstein's General Relativity. Cambridge: Cambridge University Press, 2009. Chapter 10.
  2. ^ R Gautreau, R B Hoffman, A Armenti. Static multiparticle systems in general relativity. IL NUOVO CIMENTO B, 1972, 7(1): 71–98.
  3. Terry Pilkington, Alexandre Melanson, Joseph Fitzgerald, Ivan Booth. "Trapped and marginally trapped surfaces in Weyl-distorted Schwarzschild solutions". Classical and Quantum Gravity, 2011, 28(12): 125018. arXiv:1102.0999v2[gr-qc]
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