2008/01/31 by R. A. Konoplya · 2 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Pulsars and Gravitational Waves Research #astro-ph #gr-qc #hep-th
paper · pdf · doi:10.1016/j.physletb.2008.07.079
published as Phys.Lett.B666:283-287,2008; Phys.Lett.B670:459,2009 · 10 pages, Latex, 5 figures, corrected version
openalex publication_date 2008/07/27 · arxiv created 2008/11/22 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We consider the bound states of the massive scalar field around a rotating black hole immersed in the asymptotically uniform magnetic field. In the regime of slow black hole rotation, the Klein-Gordon equation allows separation of variables. We show that the growth rate of the instability can be amplified a few times by the magnetic field. The effect occurs because the magnetic field adds the "effective mass" term B |m| to the scalar field potential for a Kerr black hole. In addition, and as a by-product, we discuss the behavior of the quasinormal modes for the magnetized rotating black holes.