On the Goldberg-Sachs theorem in higher dimensions in the non-twisting case

TL;DR

This paper generalizes the Goldberg-Sachs theorem for higher-dimensional Einstein spacetimes with non-twisting multiple WANDs, analyzing the optical matrix's eigenvalue structure and providing explicit examples and restrictions.

Contribution

It extends the Goldberg-Sachs theorem to higher dimensions, characterizing the optical matrix of non-twisting multiple WANDs and exploring their geometric and algebraic properties.

Findings

Eigenvalue degeneracy of the optical matrix is constrained by algebraic specialness.

In certain cases, all eigenvalues of the optical matrix coincide, corresponding to Robinson-Trautman spacetimes.

Explicit examples include violations of the optical constraint and special forms in six dimensions.

Abstract

We study a generalization of the "shear-free part" of the Goldberg-Sachs theorem for Einstein spacetimes admitting a non-twisting multiple Weyl Aligned Null Direction (WAND) l in n>=6 spacetime dimensions. The form of the corresponding optical matrix ${\rho}$ is restricted by the algebraically special property in terms of the degeneracy of its eigenvalues. In particular, there necessarily exists at least one multiple eigenvalue and further constraints arise in various special cases. For example, when ${\rho}$ is non-degenerate and the Weyl components ${\Phi}_{ij}$ are non-zero, all eigenvalues of ${\rho}$ coincide and such spacetimes thus correspond to the Robinson-Trautman (RT) class. On the other hand, in certain degenerate cases all non-zero eigenvalues can be distinct. We also present explicit examples of Einstein spacetimes admitting some of the permitted forms of ${\rho}$, including examples violating the "optical constraint". The obtained restrictions on ${\rho}$ are, however, in general not sufficient for l to be a multiple WAND, as demonstrated by a few "counterexamples". We also discuss the geometrical meaning of these restrictions in terms of integrability properties of certain null distributions. Finally, we specialize our analysis to the six-dimensional case, where all the permitted forms of ${\rho}$ are given in terms of just two parameters. In the appendices some examples are given and certain results pertaining to (possibly) twisting mWANDs of Einstein spacetimes are presented.