The Carter tensor and the physical-space analysis in perturbations of Kerr–Newman spacetime

Abstract

The Carter tensor is a Killing tensor of the Kerr–Newman spacetime, and its existence implies the separability of the wave equation. Nevertheless, the Carter operator is known to commute with the D’Alembertian only in the case of a Ricci-flat metric. We show that, even though the Kerr–Newman spacetime satisfies the non-vacuum Einstein-Maxwell equations, its curvature and electromagnetic tensors satisfy peculiar properties which imply that the Carter operator still commutes with the wave equation. This feature allows to adapt to Kerr–Newman the physical-space analysis of the wave equation in Kerr by Andersson–Blue $\href{https://www.jstor.org/stable/24523010}{[4]}$, which avoids frequency decomposition of the solution by precisely making use of the commutation with the Carter operator. We also extend the mathematical framework of physical-space analysis to the case of the Einstein–Maxwell equations on Kerr–Newman spacetime, representing coupled electromagnetic-gravitational perturbations of the rotating charged black hole. The physical-space analysis is crucial in this setting as the coupling of spin‑1 and spin‑2 fields in the axially symmetric background prevents the separation in modes as observed by Chandrasekhar $\href{https://doi.org/10.1007/978-94-009-6469-3_2}{[19]}$, and therefore represents an important step towards an analytical proof of the stability of the Kerr–Newman black hole.