• Source: Gravitational instanton

In mathematical physics and differential geometry, a gravitational instanton is a four-dimensional complete Riemannian manifold satisfying the vacuum Einstein equations. They are so named because they are analogues in quantum theories of gravity of instantons in Yang–Mills theory. In accordance with this analogy with self-dual Yang–Mills instantons, gravitational instantons are usually assumed to look like four dimensional Euclidean space at large distances, and to have a self-dual Riemann tensor. Mathematically, this means that they are asymptotically locally Euclidean (or perhaps asymptotically locally flat) hyperkähler 4-manifolds, and in this sense, they are special examples of Einstein manifolds. From a physical point of view, a gravitational instanton is a non-singular solution of the vacuum Einstein equations with positive-definite, as opposed to Lorentzian, metric.
There are many possible generalizations of the original conception of a gravitational instanton: for example one can allow gravitational instantons to have a nonzero cosmological constant or a Riemann tensor which is not self-dual. One can also relax the boundary condition that the metric is asymptotically Euclidean.
There are many methods for constructing gravitational instantons, including the Gibbons–Hawking Ansatz, twistor theory, and the hyperkähler quotient construction.




Introduction


Gravitational instantons are interesting, as they offer insights into the quantization of gravity. For example, positive definite asymptotically locally Euclidean metrics are needed as they obey the positive-action conjecture; actions that are unbounded below create divergence in the quantum path integral.

A four-dimensional Ricci-flat Kähler manifold has anti-self-dual Riemann tensor with respect to the complex orientation.
Consequently, a simply-connected anti-self-dual gravitational instanton is a four-dimensional complete hyperkähler manifold.
Gravitational instantons are analogous to self-dual Yang–Mills instantons.
Several distinctions can be made with respect to the structure of the Riemann curvature tensor, pertaining to flatness and self-duality. These include:

Einstein (non-zero cosmological constant)
Ricci flatness (vanishing Ricci tensor)
Conformal flatness (vanishing Weyl tensor)
Self-duality
Anti-self-duality
Conformally self-dual
Conformally anti-self-dual




Taxonomy


By specifying the 'boundary conditions', i.e. the asymptotics of the metric 'at infinity' on a noncompact Riemannian manifold, gravitational instantons are divided into a few classes, such as asymptotically locally Euclidean spaces (ALE spaces), asymptotically locally flat spaces (ALF spaces).
They can be further characterized by whether the Riemann tensor is self-dual, whether the Weyl tensor is self-dual, or neither; whether or not they are Kähler manifolds; and various characteristic classes, such as Euler characteristic, the Hirzebruch signature (Pontryagin class), the Rarita–Schwinger index (spin-3/2 index), or generally the Chern class. The ability to support a spin structure (i.e. to allow consistent Dirac spinors) is another appealing feature.




List of examples


Eguchi et al. list a number of examples of gravitational instantons. These include, among others:

Flat space





R


4




{\displaystyle \mathbb {R} ^{4}}

, the torus





T


4




{\displaystyle \mathbb {T} ^{4}}

and the Euclidean de Sitter space





S


4




{\displaystyle \mathbb {S} ^{4}}

, i.e. the standard metric on the 4-sphere.
The product of spheres




S

2


×

S

2




{\displaystyle S^{2}\times S^{2}}

.
The Schwarzschild metric





R


2


×

S

2




{\displaystyle \mathbb {R} ^{2}\times S^{2}}

and the Kerr metric





R


2


×

S

2




{\displaystyle \mathbb {R} ^{2}\times S^{2}}

.
The Eguchi–Hanson instanton




T

∗



C
P

(
1
)


{\displaystyle T^{*}\mathbb {CP} (1)}

, given below.
The Taub–NUT solution, given below.
The Fubini–Study metric on the complex projective plane




C
P

(
2
)
.


{\displaystyle \mathbb {CP} (2).}

Note that the complex projective plane does not support well-defined Dirac spinors. That is, it is not a spin structure. It can be given a spinc structure, however.
The Page space, which exhibits an explicit Einstein metric on the connected sum of two oppositely oriented complex projective planes




C
P

(
2
)
#



C
P

¯


(
2
)


{\displaystyle \mathbb {CP} (2)\#{\overline {\mathbb {CP} }}(2)}

.
The Gibbons–Hawking multi-center metrics, given below.
The Taub-bolt metric




C
P

(
2
)
∖
{
0
}


{\displaystyle \mathbb {CP} (2)\setminus \{0\}}

and the rotating Taub-bolt metric. The "bolt" metrics have a cylindrical-type coordinate singularity at the origin, as compared to the "nut" metrics, which have a sphere coordinate singularity. In both cases, the coordinate singularity can be removed by switching to Euclidean coordinates at the origin.
The K3 surfaces.
The ALE (asymptotically locally Euclidean) anti-self-dual manifolds. Among these, the simply connected ones are all hyper-Kähler, and each one is asymptotic to a flat cone over




S

3


=
S
U
(
2
)


{\displaystyle S^{3}=SU(2)}

modulo a finite subgroup. Each finite sub-group of



S
U
(
2
)


{\displaystyle SU(2)}

actually occurs. The complete list of possibilities consists of the cyclic groups





Z


k
+
1




{\displaystyle \mathbb {Z} _{k+1}}

together with the inverse images of the dihedral groups, the tetrahedral group, the octahedral group, and the icosahedral group under the double cover



S
U
(
2
)
→
S
O
(
3
)


{\displaystyle SU(2)\to SO(3)}

. Note that





Z


2




{\displaystyle \mathbb {Z} _{2}}

corresponds to the Eguchi–Hanson instanton, while for higher k, the cyclic group





Z


k
+
1




{\displaystyle \mathbb {Z} _{k+1}}

corresponds to the Gibbons–Hawking multi-center metrics, each of which diffeomorphic to the space obtained from the disjoint union of k copies of




T

∗



S

2




{\displaystyle T^{*}S^{2}}

by using the Dynkin diagram




A

k




{\displaystyle A_{k}}

as a plumbing diagram.
This is a very incomplete list; there are many other possibilities, not all of which have been classified.




Examples


It will be convenient to write the gravitational instanton solutions below using left-invariant 1-forms on the three-sphere S3 (viewed as the group Sp(1) or SU(2)). These can be defined in terms of Euler angles by









σ

1





=
sin
⁡
ψ

d
θ
−
cos
⁡
ψ
sin
⁡
θ

d
ϕ





σ

2





=
cos
⁡
ψ

d
θ
+
sin
⁡
ψ
sin
⁡
θ

d
ϕ





σ

3





=
d
ψ
+
cos
⁡
θ

d
ϕ
.






{\displaystyle {\begin{aligned}\sigma _{1}&=\sin \psi \,d\theta -\cos \psi \sin \theta \,d\phi \\\sigma _{2}&=\cos \psi \,d\theta +\sin \psi \sin \theta \,d\phi \\\sigma _{3}&=d\psi +\cos \theta \,d\phi .\\\end{aligned}}}


Note that



d

σ

i


+

σ

j


∧

σ

k


=
0


{\displaystyle d\sigma _{i}+\sigma _{j}\wedge \sigma _{k}=0}

for



i
,
j
,
k
=
1
,
2
,
3


{\displaystyle i,j,k=1,2,3}

cyclic.




= Taub–NUT metric

=




d

s

2


=


1
4





r
+
n


r
−
n



d

r

2


+



r
−
n


r
+
n




n

2





σ

3




2


+


1
4


(

r

2


−

n

2


)
(



σ

1




2


+



σ

2




2


)


{\displaystyle ds^{2}={\frac {1}{4}}{\frac {r+n}{r-n}}dr^{2}+{\frac {r-n}{r+n}}n^{2}{\sigma _{3}}^{2}+{\frac {1}{4}}(r^{2}-n^{2})({\sigma _{1}}^{2}+{\sigma _{2}}^{2})}





= Eguchi–Hanson metric

=
The Eguchi–Hanson space is defined by a metric the cotangent bundle of the 2-sphere




T

∗



C
P

(
1
)
=

T

∗



S

2




{\displaystyle T^{*}\mathbb {CP} (1)=T^{*}S^{2}}

. This metric is




d

s

2


=


(

1
−


a

r

4





)


−
1


d

r

2


+



r

2


4



(

1
−


a

r

4





)




σ

3




2


+



r

2


4


(

σ

1


2


+

σ

2


2


)
.


{\displaystyle ds^{2}=\left(1-{\frac {a}{r^{4}}}\right)^{-1}dr^{2}+{\frac {r^{2}}{4}}\left(1-{\frac {a}{r^{4}}}\right){\sigma _{3}}^{2}+{\frac {r^{2}}{4}}(\sigma _{1}^{2}+\sigma _{2}^{2}).}


where



r
≥

a

1

/

4




{\displaystyle r\geq a^{1/4}}

. This metric is smooth everywhere if it has no conical singularity at



r
→

a

1

/

4




{\displaystyle r\rightarrow a^{1/4}}

,



θ
=
0
,
π


{\displaystyle \theta =0,\pi }

. For



a
=
0


{\displaystyle a=0}

this happens if



ψ


{\displaystyle \psi }

has a period of



4
π


{\displaystyle 4\pi }

, which gives a flat metric on R4; However, for



a
≠
0


{\displaystyle a\neq 0}

this happens if



ψ


{\displaystyle \psi }

has a period of



2
π


{\displaystyle 2\pi }

.
Asymptotically (i.e., in the limit



r
→
∞


{\displaystyle r\rightarrow \infty }

) the metric looks like




d

s

2


=
d

r

2


+



r

2


4



σ

3


2


+



r

2


4


(

σ

1


2


+

σ

2


2


)


{\displaystyle ds^{2}=dr^{2}+{\frac {r^{2}}{4}}\sigma _{3}^{2}+{\frac {r^{2}}{4}}(\sigma _{1}^{2}+\sigma _{2}^{2})}


which naively seems as the flat metric on R4. However, for



a
≠
0


{\displaystyle a\neq 0}

,



ψ


{\displaystyle \psi }

has only half the usual periodicity, as we have seen. Thus the metric is asymptotically R4 with the identification



ψ


∼


ψ
+
2
π


{\displaystyle \psi \,{\sim }\,\psi +2\pi }

, which is a Z2 subgroup of SO(4), the rotation group of R4. Therefore, the metric is said to be asymptotically
R4/Z2.
There is a transformation to another coordinate system, in which the metric looks like




d

s

2


=


1

V
(

x

)



(
d
ψ
+

ω

⋅
d

x


)

2


+
V
(

x

)
d

x

⋅
d

x

,


{\displaystyle ds^{2}={\frac {1}{V(\mathbf {x} )}}(d\psi +{\boldsymbol {\omega }}\cdot d\mathbf {x} )^{2}+V(\mathbf {x} )d\mathbf {x} \cdot d\mathbf {x} ,}


where




∇
V
=
±
∇
×

ω

,

V
=

∑

i
=
1


2




1


|


x

−


x


i



|




.


{\displaystyle \nabla V=\pm \nabla \times {\boldsymbol {\omega }},\quad V=\sum _{i=1}^{2}{\frac {1}{|\mathbf {x} -\mathbf {x} _{i}|}}.}


(For a = 0,



V
=


1


|


x


|






{\displaystyle V={\frac {1}{|\mathbf {x} |}}}

, and the new coordinates are defined as follows: one first defines



ρ
=

r

2



/

4


{\displaystyle \rho =r^{2}/4}

and then parametrizes



ρ


{\displaystyle \rho }

,



θ


{\displaystyle \theta }

and



ϕ


{\displaystyle \phi }

by the R3 coordinates




x



{\displaystyle \mathbf {x} }

, i.e.




x

=
(
ρ
sin
⁡
θ
cos
⁡
ϕ
,
ρ
sin
⁡
θ
sin
⁡
ϕ
,
ρ
cos
⁡
θ
)


{\displaystyle \mathbf {x} =(\rho \sin \theta \cos \phi ,\rho \sin \theta \sin \phi ,\rho \cos \theta )}

).
In the new coordinates,



ψ


{\displaystyle \psi }

has the usual periodicity



ψ


∼


ψ
+
4
π
.


{\displaystyle \psi \ {\sim }\ \psi +4\pi .}


One may replace V by





V
=

∑

i
=
1


n




1


|


x

−


x


i



|




.


{\displaystyle \quad V=\sum _{i=1}^{n}{\frac {1}{|\mathbf {x} -\mathbf {x} _{i}|}}.}


For some n points





x


i




{\displaystyle \mathbf {x} _{i}}

, i = 1, 2..., n.
This gives a multi-center Eguchi–Hanson gravitational instanton, which is again smooth everywhere if the angular coordinates have the usual periodicities (to avoid conical singularities). The asymptotic limit (



r
→
∞


{\displaystyle r\rightarrow \infty }

) is equivalent to taking all





x


i




{\displaystyle \mathbf {x} _{i}}

to zero, and by changing coordinates back to r,



θ


{\displaystyle \theta }

and



ϕ


{\displaystyle \phi }

, and redefining



r
→
r

/



n




{\displaystyle r\rightarrow r/{\sqrt {n}}}

, we get the asymptotic metric




d

s

2


=
d

r

2


+



r

2


4




(




d
ψ

n


+
cos
⁡
θ

d
ϕ

)


2


+



r

2


4


[
(

σ

1


L



)

2


+
(

σ

2


L



)

2


]
.


{\displaystyle ds^{2}=dr^{2}+{\frac {r^{2}}{4}}\left({d\psi \over n}+\cos \theta \,d\phi \right)^{2}+{\frac {r^{2}}{4}}[(\sigma _{1}^{L})^{2}+(\sigma _{2}^{L})^{2}].}


This is R4/Zn = C2/Zn, because it is R4 with the angular coordinate



ψ


{\displaystyle \psi }

replaced by



ψ

/

n


{\displaystyle \psi /n}

, which has the wrong periodicity (



4
π

/

n


{\displaystyle 4\pi /n}

instead of



4
π


{\displaystyle 4\pi }

). In other words, it is R4 identified under



ψ


∼


ψ
+
4
π
k

/

n


{\displaystyle \psi \ {\sim }\ \psi +4\pi k/n}

, or, equivalently, C2 identified under zi ~




e

2
π
i
k

/

n




{\displaystyle e^{2\pi ik/n}}

zi for i = 1, 2.
To conclude, the multi-center Eguchi–Hanson geometry is a Kähler Ricci flat geometry which is asymptotically C2/Zn. According to Yau's theorem this is the only geometry satisfying these properties. Therefore, this is also the geometry of a C2/Zn orbifold in string theory after its conical singularity has been smoothed away by its "blow up" (i.e., deformation).




= Gibbons–Hawking multi-centre metrics

=
The Gibbons–Hawking multi-center metrics are given by




d

s

2


=


1

V
(

x

)



(
d
τ
+

ω

⋅
d

x


)

2


+
V
(

x

)
d

x

⋅
d

x

,


{\displaystyle ds^{2}={\frac {1}{V(\mathbf {x} )}}(d\tau +{\boldsymbol {\omega }}\cdot d\mathbf {x} )^{2}+V(\mathbf {x} )d\mathbf {x} \cdot d\mathbf {x} ,}


where




∇
V
=
±
∇
×

ω

,

V
=
ε
+
2
M

∑

i
=
1


k




1


|


x

−


x


i



|




.


{\displaystyle \nabla V=\pm \nabla \times {\boldsymbol {\omega }},\quad V=\varepsilon +2M\sum _{i=1}^{k}{\frac {1}{|\mathbf {x} -\mathbf {x} _{i}|}}.}


Here,



ϵ
=
1


{\displaystyle \epsilon =1}

corresponds to multi-Taub–NUT,



ϵ
=
0


{\displaystyle \epsilon =0}

and



k
=
1


{\displaystyle k=1}

is flat space, and



ϵ
=
0


{\displaystyle \epsilon =0}

and



k
=
2


{\displaystyle k=2}

is the Eguchi–Hanson solution (in different coordinates).




= FLRW-metrics as gravitational instantons

=
In 2021 it was found that if one views the curvature parameter of a foliated maximally symmetric space as a continuous function, the gravitational action, as a sum of the Einstein–Hilbert action and the Gibbons–Hawking–York boundary term, becomes that of a point particle. Then the trajectory is the scale factor and the curvature parameter is viewed as the potential. For the solutions restricted like this, general relativity takes the form of a topological Yang–Mills theory.




See also


Gravitational anomaly
Hyperkähler manifold




References



Gibbons, G.W.; Hawking, S.W. (October 1978). "Gravitational multi-instantons". Physics Letters B. 78 (4): 430–432. Bibcode:1978PhLB...78..430G. doi:10.1016/0370-2693(78)90478-1.
Gibbons, G. W.; Hawking, S. W. (October 1979). "Classification of Gravitational Instanton symmetries". Communications in Mathematical Physics. 66 (3): 291–310. Bibcode:1979CMaPh..66..291G. doi:10.1007/BF01197189. S2CID 123183399.
Eguchi, Tohru; Hanson, Andrew J. (April 1978). "Asymptotically flat self-dual solutions to euclidean gravity". Physics Letters B. 74 (3): 249–251. Bibcode:1978PhLB...74..249E. doi:10.1016/0370-2693(78)90566-X. OSTI 1446816. S2CID 16380482.
Eguchi, Tohru; Hanson, Andrew J (July 1979). "Self-dual solutions to euclidean gravity". Annals of Physics. 120 (1): 82–106. Bibcode:1979AnPhy.120...82E. doi:10.1016/0003-4916(79)90282-3. OSTI 1447072. S2CID 48866858.
Eguchi, Tohru; Hanson, Andrew J. (December 1979). "Gravitational instantons". General Relativity and Gravitation. 11 (5): 315–320. Bibcode:1979GReGr..11..315E. doi:10.1007/BF00759271. S2CID 123806150.
Kronheimer, P. B. (1989). "The construction of ALE spaces as hyper-Kähler quotients". Journal of Differential Geometry. 29 (3): 665–683. doi:10.4310/jdg/1214443066.

Kata Kunci Pencarian:

• Gravitational instanton
• Instanton
• Gravitational anomaly
• Einstein manifold
• Ale (disambiguation)
• Andrew J. Hanson
• Monstrous moonshine
• Gibbons–Hawking ansatz
• Nuts and bolts (general relativity)
• Hyperkähler manifold