- Source: Weyl metrics
In general relativity, the Weyl metrics (named after the German-American mathematician Hermann Weyl) 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
where
ψ
(
ρ
,
z
)
{\displaystyle \psi (\rho ,z)}
and
γ
(
ρ
,
z
)
{\displaystyle \gamma (\rho ,z)}
are two metric potentials dependent on Weyl's canonical coordinates
{
ρ
,
z
}
{\displaystyle \{\rho \,,z\}}
. The coordinate system
{
t
,
ρ
,
z
,
ϕ
}
{\displaystyle \{t,\rho ,z,\phi \}}
serves best for symmetries of Weyl's spacetime (with two Killing vector fields being
ξ
t
=
∂
t
{\displaystyle \xi ^{t}=\partial _{t}}
and
ξ
ϕ
=
∂
ϕ
{\displaystyle \xi ^{\phi }=\partial _{\phi }}
) and often acts like cylindrical coordinates, but is incomplete when describing a black hole as
{
ρ
,
z
}
{\displaystyle \{\rho \,,z\}}
only cover the horizon and its exteriors.
Hence, to determine a static axisymmetric solution corresponding to a specific stress–energy tensor
T
a
b
{\displaystyle 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
ψ
(
ρ
,
z
)
{\displaystyle \psi (\rho ,z)}
and
γ
(
ρ
,
z
)
{\displaystyle \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
a
b
{\displaystyle 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
{\displaystyle A_{a}}
, the anti-symmetric electromagnetic field
F
a
b
{\displaystyle F_{ab}}
and the trace-free stress–energy tensor
T
a
b
{\displaystyle T_{ab}}
(
T
=
g
a
b
T
a
b
=
0
)
{\displaystyle (T=g^{ab}T_{ab}=0)}
will be respectively determined by
which respects the source-free covariant Maxwell equations:
Eq(5.a) can be simplified to:
in the calculations as
Γ
b
c
a
=
Γ
c
b
a
{\displaystyle \Gamma _{bc}^{a}=\Gamma _{cb}^{a}}
. Also, since
R
=
−
8
π
T
=
0
{\displaystyle R=-8\pi T=0}
for electrovacuum, Eq(2) reduces to
Now, suppose the Weyl-type axisymmetric electrostatic potential is
A
a
=
Φ
(
ρ
,
z
)
[
d
t
]
a
{\displaystyle A_{a}=\Phi (\rho ,z)[dt]_{a}}
(the component
Φ
{\displaystyle \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
{\displaystyle R=0}
yields Eq(7.a),
R
t
t
=
8
π
T
t
t
{\displaystyle R_{tt}=8\pi T_{tt}}
or
R
φ
φ
=
8
π
T
φ
φ
{\displaystyle R_{\varphi \varphi }=8\pi T_{\varphi \varphi }}
yields Eq(7.b),
R
ρ
ρ
=
8
π
T
ρ
ρ
{\displaystyle R_{\rho \rho }=8\pi T_{\rho \rho }}
or
R
z
z
=
8
π
T
z
z
{\displaystyle R_{zz}=8\pi T_{zz}}
yields Eq(7.c),
R
ρ
z
=
8
π
T
ρ
z
{\displaystyle R_{\rho z}=8\pi T_{\rho z}}
yields Eq(7.d), and Eq(5.b) yields Eq(7.e). Here
∇
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 Laplace and gradient operators. Moreover, if we suppose
ψ
=
ψ
(
Φ
)
{\displaystyle \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
Φ
=
0
{\displaystyle \Phi =0}
and
T
a
b
=
0
{\displaystyle T_{ab}=0}
, Eqs(7.a-7.e) reduce to
We can firstly obtain
ψ
(
ρ
,
z
)
{\displaystyle \psi (\rho ,z)}
by solving Eq(8.b), and then integrate Eq(8.c) and Eq(8.d) for
γ
(
ρ
,
z
)
{\displaystyle \gamma (\rho ,z)}
. Practically, Eq(8.a) arising from
R
=
0
{\displaystyle 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
ψ
(
ρ
,
z
)
{\displaystyle \psi (\rho ,z)}
relates with the electrostatic scalar potential
Φ
(
ρ
,
z
)
{\displaystyle \Phi (\rho ,z)}
via a function
ψ
=
ψ
(
Φ
)
{\displaystyle \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 into
which give rise to
Now replace the variable
ψ
{\displaystyle \psi }
by
ζ
:=
e
2
ψ
{\displaystyle \zeta :=e^{2\psi }}
, and Eq(B.4) is simplified to
Direct quadrature of Eq(B.5) yields
ζ
=
e
2
ψ
=
Φ
2
+
C
~
Φ
+
B
{\displaystyle \zeta =e^{2\psi }=\Phi ^{2}+{\tilde {C}}\Phi +B}
, with
{
B
,
C
~
}
{\displaystyle \{B,{\tilde {C}}\}}
being integral constants. To resume asymptotic flatness at spatial infinity, we need
lim
ρ
,
z
→
∞
Φ
=
0
{\displaystyle \lim _{\rho ,z\to \infty }\Phi =0}
and
lim
ρ
,
z
→
∞
e
2
ψ
=
1
{\displaystyle \lim _{\rho ,z\to \infty }e^{2\psi }=1}
, so there should be
B
=
1
{\displaystyle B=1}
. Also, rewrite the constant
C
~
{\displaystyle {\tilde {C}}}
as
−
2
C
{\displaystyle -2C}
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
±
2
ψ
=
∑
n
=
0
∞
(
±
2
ψ
)
n
n
!
{\textstyle e^{\pm 2\psi }=\sum _{n=0}^{\infty }{\frac {(\pm 2\psi )^{n}}{n!}}}
; thus in the approximation for weak field limit
ψ
→
0
{\displaystyle \psi \to 0}
, one has
and 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,
where
Φ
N
(
ρ
,
z
)
{\displaystyle \Phi _{N}(\rho ,z)}
is the usual Newtonian potential satisfying Poisson's equation
∇
L
2
Φ
N
=
4
π
ϱ
N
{\displaystyle \nabla _{L}^{2}\Phi _{N}=4\pi \varrho _{N}}
, just like Eq(3.a) or Eq(4.a) for the Weyl metric potential
ψ
(
ρ
,
z
)
{\displaystyle \psi (\rho ,z)}
. The similarities between
ψ
(
ρ
,
z
)
{\displaystyle \psi (\rho ,z)}
and
Φ
N
(
ρ
,
z
)
{\displaystyle \Phi _{N}(\rho ,z)}
inspire people to find out the Newtonian analogue of
ψ
(
ρ
,
z
)
{\displaystyle \psi (\rho ,z)}
when studying Weyl class of solutions; that is, to reproduce
ψ
(
ρ
,
z
)
{\displaystyle \psi (\rho ,z)}
nonrelativistically by certain type of Newtonian sources. The Newtonian analogue of
ψ
(
ρ
,
z
)
{\displaystyle \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(8) are given by
where
From the perspective of Newtonian analogue,
ψ
S
S
{\displaystyle \psi _{SS}}
equals the gravitational potential produced by a rod of mass
M
{\displaystyle M}
and length
2
M
{\displaystyle 2M}
placed symmetrically on the
z
{\displaystyle z}
-axis; that is, by a line mass of uniform density
σ
=
1
/
2
{\displaystyle \sigma =1/2}
embedded the interval
z
∈
[
−
M
,
M
]
{\displaystyle z\in [-M,M]}
. (Note: Based on this analogue, important extensions of the Schwarzschild metric have been developed, as discussed in ref.)
Given
ψ
S
S
{\displaystyle \psi _{SS}}
and
γ
S
S
{\displaystyle \gamma _{SS}}
, Weyl's metric Eq(1) becomes
and after substituting the following mutually consistent relations
one can obtain the common form of Schwarzschild metric in the usual
{
t
,
r
,
θ
,
ϕ
}
{\displaystyle \{t,r,\theta ,\phi \}}
coordinates,
The metric Eq(14) cannot be directly transformed into Eq(16) by performing the standard cylindrical-spherical transformation
(
t
,
ρ
,
z
,
ϕ
)
=
(
t
,
r
sin
θ
,
r
cos
θ
,
ϕ
)
{\displaystyle (t,\rho ,z,\phi )=(t,r\sin \theta ,r\cos \theta ,\phi )}
, because
{
t
,
r
,
θ
,
ϕ
}
{\displaystyle \{t,r,\theta ,\phi \}}
is complete while
(
t
,
ρ
,
z
,
ϕ
)
{\displaystyle (t,\rho ,z,\phi )}
is incomplete. This is why we call
{
t
,
ρ
,
z
,
ϕ
}
{\displaystyle \{t,\rho ,z,\phi \}}
in Eq(1) as Weyl's canonical coordinates rather than cylindrical coordinates, although they have a lot in common; for example, the Laplacian
∇
2
:=
∂
ρ
ρ
+
1
ρ
∂
ρ
+
∂
z
z
{\displaystyle \nabla ^{2}:=\partial _{\rho \rho }+{\frac {1}{\rho }}\partial _{\rho }+\partial _{zz}}
in Eq(7) 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
|
{\displaystyle M>|Q|}
) as solutions to Eqs(7) are given by
where
Thus, given
ψ
R
N
{\displaystyle \psi _{RN}}
and
γ
R
N
{\displaystyle \gamma _{RN}}
, Weyl's metric becomes
and employing the following transformations
one can obtain the common form of non-extremal Reissner–Nordström metric in the usual
{
t
,
r
,
θ
,
ϕ
}
{\displaystyle \{t,r,\theta ,\phi \}}
coordinates,
Extremal Reissner–Nordström solution
The potentials generating the extremal Reissner–Nordström solution (
M
=
|
Q
|
{\displaystyle M=|Q|}
) as solutions to Eqs(7) 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 reads
and by substituting
we obtain the extremal Reissner–Nordström metric in the usual
{
t
,
r
,
θ
,
ϕ
}
{\displaystyle \{t,r,\theta ,\phi \}}
coordinates,
Mathematically, the extremal Reissner–Nordström can be obtained by taking the limit
Q
→
M
{\displaystyle 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(1) with the vanishing potential
γ
(
ρ
,
z
)
{\displaystyle \gamma (\rho ,z)}
(like the extremal Reissner–Nordström metric) constitute a special subclass which have only one metric potential
ψ
(
ρ
,
z
)
{\displaystyle \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,
where we use
λ
{\displaystyle \lambda }
in Eq(22) as the single metric function in place of
ψ
{\displaystyle \psi }
in Eq(1) to emphasize that they are different by axial symmetry (
ϕ
{\displaystyle \phi }
-dependence).
Weyl vacuum solutions in spherical coordinates
Weyl's metric can also be expressed in spherical coordinates that
which equals Eq(1) via the coordinate transformation
(
t
,
ρ
,
z
,
ϕ
)
↦
(
t
,
r
sin
θ
,
r
cos
θ
,
ϕ
)
{\displaystyle (t,\rho ,z,\phi )\mapsto (t,r\sin \theta ,r\cos \theta ,\phi )}
(Note: As shown by Eqs(15)(21)(24), this transformation is not always applicable.) In the vacuum case, Eq(8.b) for
ψ
(
r
,
θ
)
{\displaystyle \psi (r,\theta )}
becomes
The asymptotically flat solutions to Eq(28) is
where
P
n
(
cos
θ
)
{\displaystyle P_{n}(\cos \theta )}
represent Legendre polynomials, and
a
n
{\displaystyle a_{n}}
are multipole coefficients. The other metric potential
γ
(
r
,
θ
)
{\displaystyle \gamma (r,\theta )}
is given by
See also
Schwarzschild metric
Reissner–Nordström metric
Distorted Schwarzschild metric
References
Kata Kunci Pencarian:
- Weyl metrics
- Weyl tensor
- List of things named after Hermann Weyl
- Weyl–Lewis–Papapetrou coordinates
- Spinor
- Weyl transformation
- Reissner–Nordström metric
- Distorted Schwarzschild metric
- Equidistributed sequence
- Weyl equation
