Abstract
We find a new class of exact solutions in the Einstein–Maxwell theory by employing the Ernst magnetization process to the Kerr–Newman–Taub-NUT spacetimes. We study the solutions and find that they are regular everywhere. We also find the quasilocal conserved quantities for the spacetimes, the corresponding Smarr formula and the first law of thermodynamics.
Highlights
Finding the exact solutions to the Einstein–Maxwell theory is always fascinating, as it opens a door to explore the new aspects of the gravitational physics
Ernst magnetization is a transformation acting on a set of Ernst potentials which can be defined by using some functions appearing in the seed spacetime solution and the accompanying vector field in Einstein–Maxwell theory
We have constructed a new class of the exact solutions to the Einstein–Maxwell theory in four dimensions which describes the immersion of the Kerr–Newman–TaubNUT spacetimes in an external magnetic field
Summary
Finding the exact solutions to the Einstein–Maxwell theory is always fascinating, as it opens a door to explore the new aspects of the gravitational physics. The exact solutions to the aforementioned theory contain the black hole solutions, such as the Kerr–Newman family, to a more general spacetime solutions of Plebanski–Demianski [1] Different aspects of those solutions have been studied and reported, in which, some can be related to the real astrophysical phenomena, and others are still in vague. The superradiant instability in this weakly magnetized black hole had been investigated in [19], and this type of magnetization for Kerr-NUT-AdS spacetime had been performed in [20] This Ernst magnetization itself can be viewed as a type of Harrison transformation [21] which maps an old solution to a new one in the theory.
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