The superradiant stability of Kerr-Newman black holes

Abstract

In this article, the superradiation stability of Kerr-Newman black holes is discussed by introducing the condition used in Kerr black holes y into them. Moreover, the motion equation of the minimal coupled scalar perturbation in a Kerr-Newman black hole is divided into angular and radial parts. Hod proved\cite{12} that the Kerr black hole should be superradiantly stable under massive scalar perturbation when $\mu \ge \sqrt{2}m{\Omega }_H$, where $\mu$ is the mass. In this article, a new variable y is added here to expand the results of the above article. When $\sqrt{2(a^2+Q^2)}/r_{+}^2<\omega <m{\Omega }_H+q{\Phi }_H$,particularly $\mu \ge \sqrt{2}(m{\Omega }_H+q{\Phi }_H)$,so the Kerr-Newman black hole is superradiantly stable at that time.

arXiv admin note: substantial text overlap with arXiv:2105.05394

References in corpus (2)

• Superradiant instability of charged massive scalar field in Kerr-Newman-anti-de Sitter black hole
• Analytic treatment of the system of a Kerr-Newman black hole and a charged massive scalar field