2013/01/16 by G. W. Gibbons, Gibbons, G. W., Abid H. Mujtaba +3 · 6 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #High Energy Astrophysical Phenomena (astro-ph.HE) #High Energy Physics - Theory (hep-th)
paper · pdf · doi:10.48550/arxiv.1301.3927
openalex publication_date 2013/01/16 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The spacetimes obtained by Ernst's procedure for appending an external magnetic field B to a seed Kerr-Newman black hole are commonly believed to be asymptotic to the static Melvin solution. We show that this is not in general true. Unless the electric charge of the black hole satisfies Q= jB(1+ 1/4 j2 B4), where j is the angular momentum of the original seed solution, an ergoregion extends all the way from the black hole horizon to infinity. We give a self-contained account of the solution-generating procedure, including including explicit formulae for the metric and the vector potential. In the case when Q= jB(1+ 1/4 j2 B4), we show that there is an arbitrariness in the choice of asymptotically timelike Killing field KΩ= ∂/∂ t+ Ω∂/∂ ϕ, because there is no canonical choice of Ω. For one choice, Ω=Ωs, the metric is asymptotically static, and there is an ergoregion confined to the neighbourhood of the horizon. On the other hand, by choosing Ω=ΩH, so that KΩH is co-rotating with the horizon, then for sufficiently large B numerical studies indicate there is no ergoregion at all. For smaller values, in a range B-<b></b>