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 Kähler–Einstein manifold has a self-dual Riemann tensor.
* Equivalently, a 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 Kahler 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 $\mathbb^4$, the torus $\mathbb^4$ and the Euclidean de Sitter space $\mathbb^4$, ''i.e.'' the standard metric on the 4-sphere.
* The product of spheres $S^2\times S^2$.
* The Schwarzschild metric $\mathbb^2\times S^2$ and the Kerr metric $\mathbb^2\times S^2$
* The Eguchi–Hanson instanton $T^*\mathbb(1)$, given below.
* The Taub–NUT solution, given below.
* The Fubini–Study metric on the complex projective plane $\mathbb(2).$ 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.
* Page space, a rotating compact metric on the direct sum of two complex projective planes $\mathbb(2)\oplus\overline(2)$.
* The Gibbons–Hawking multi-center metrics, given below.
* The Taub-bolt metric $\mathbb(2)\setminus \$ 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 asymptotically locally Euclidean self-dual manifolds, including the lens spaces $L(k + 1, 1)$, the double-coverings of the dihedral groups, the tetrahedral group, the octahedral group, and the icosahedral group. Note that $L(2, 1)$ corresponds to the Eguchi–Hanson instanton, while for higher ''k'', the $L(2, 1)$ corresponds to the Gibbons–Hawking multi-center metrics.
This is an incomplete list; there are others.

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

:$\begin \sigma_1 &= \sin \psi \, d \theta - \cos \psi \sin \theta \, d \phi \\ \sigma_2 &= \cos \psi \, d \theta + \sin \psi \sin \theta \, d \phi \\ \sigma_3 &= d \psi + \cos \theta \, d \phi. \\ \end$

Note that $d\sigma_i + \sigma_j \wedge \sigma_k=0$ for $i,j,k=1,2,3$ cyclic.

Taub–NUT metric

:$ds^2 = \frac \frac dr^2 + \frac n^2 ^2 + \frac(r^2 - n^2)(^2 + ^2)$

Eguchi–Hanson metric

The Eguchi–Hanson space is defined by a metric the cotangent bundle of the 2-sphere $T^*\mathbb(1)=T^*S^2$. This metric is

:$ds^2 = \left( 1 - \frac \right) ^ dr^2 + \frac \left( 1 - \frac \right) ^2 + \frac (\sigma_1^2 + \sigma_2^2).$

where $r \ge a^$. This metric is smooth everywhere if it has no conical singularity at $r \rightarrow a^$, $\theta = 0, \pi$. For $a = 0$ this happens if $\psi$ has a period of $4\pi$, which gives a flat metric on R⁴; However, for $a \ne 0$ this happens if $\psi$ has a period of $2\pi$.

Asymptotically (i.e., in the limit $r \rightarrow \infty$) the metric looks like
:$ds^2 = dr^2 + \frac \sigma_3^2 + \frac (\sigma_1^2 + \sigma_2^2)$
which naively seems as the flat metric on R⁴. However, for $a \ne 0$, $\psi$ has only half the usual periodicity, as we have seen. Thus the metric is asymptotically R⁴ with the identification $\psi\, \, \psi + 2\pi$, 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
:$ds^2 = \frac ( d \psi + \boldsymbol \cdot d \mathbf)^2 + V(\mathbf) d \mathbf \cdot d \mathbf,$
where
$\nabla V = \pm \nabla \times \boldsymbol, \quad V = \sum_^2 \frac.$
:(For a = 0, $V = \frac$, and the new coordinates are defined as follows: one first defines $\rho=r^2/4$ and then parametrizes $\rho$, $\theta$ and $\phi$ by the R³ coordinates $\mathbf$, i.e. $\mathbf=(\rho \sin \theta \cos \phi, \rho \sin \theta \sin \phi,\rho \cos\theta)$).

In the new coordinates, $\psi$ has the usual periodicity $\psi\ \ \psi + 4\pi.$

One may replace V by
:$\quad V = \sum_^n \frac.$
For some ''n'' points $\mathbf_i$, ''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 ($r\rightarrow \infty$) is equivalent to taking all $\mathbf_i$ to zero, and by changing coordinates back to r, $\theta$ and $\phi$, and redefining $r\rightarrow r/\sqrt$, we get the asymptotic metric

: ds^2 = dr^2 + \frac \left( + \cos \theta \, d\phi\right)^2 + \frac \sigma_1^L)^2 + (\sigma_2^L)^2

This is R⁴/Z_''n'' = C²/Z_n, because it is R⁴ with the angular coordinate $\psi$ replaced by $\psi/n$, which has the wrong periodicity ($4\pi/n$ instead of $4\pi$). In other words, it is R⁴ identified under $\psi\ \ \psi + 4\pi k/n$, or, equivalently, C² identified under ''z''_''i'' ~ $e^$ ''z''_''i'' for ''i'' = 1, 2.

To conclude, the multi-center Eguchi–Hanson geometry is a Kähler Ricci flat geometry which is asymptotically C²/Z_n. According to Yau's theorem this is the only geometry satisfying these properties. Therefore, this is also the geometry of a C²/Z_n 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

:$ds^2 = \frac ( d \tau + \boldsymbol \cdot d \mathbf)^2 + V(\mathbf) d \mathbf \cdot d \mathbf,$

where

:$\nabla V = \pm \nabla \times \boldsymbol, \quad V = \varepsilon + 2M \sum_^ \frac.$

Here, $\epsilon = 1$ corresponds to multi-Taub–NUT, $\epsilon = 0$ and $k = 1$ is flat space, and $\epsilon = 0$ and $k = 2$ is the Eguchi–Hanson solution (in different coordinates).

FLRW-metrics as gravitational instantons

In 2021 it was found J.Hristov;. Quantum theory of $k(\phi)$-metrics its connection to Chern–Simons models and the theta vacuum structure of quantum gravity https://doi.org/10.1140/epjc/s10052-021-09315-1 that if one views the curvature parameter of a foliated maximally symmetric space as a continues 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

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*{{cite journal, last1=Kronheimer, first1=P. B., title=The construction of ALE spaces as hyper-Kähler quotients, journal=Journal of Differential Geometry, date=1989, volume=29, issue=3, pages=665–683, doi=10.4310/jdg/1214443066, doi-access=free

Riemannian manifolds
Quantum gravity
Mathematical physics
4-manifolds