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Quasinormal modes, scattering, and Hawking radiation of Kerr-Newman black holes in a magnetic field

K. D. Kokkotas and R. A. Konoplya^*

A. Zhidenko^†

Theoretical Astrophysics, Eberhard-Karls University of Tübingen, Tübingen 72076, Germany

Centro de Matemática, Computação e Cognição, Universidade Federal do ABC, Rua Santa Adélia, 166, 09210-170, Santo André, São Paulo, Brazil

^*konoplya_roma@yahoo.com
^†olexandr.zhydenko@ufabc.edu.br

Phys. Rev. D 83, 024031 – Published 26 January, 2011

DOI: https://doi.org/10.1103/PhysRevD.83.024031

Abstract

We perform a comprehensive analysis of the spectrum of proper oscillations (quasinormal modes), transmission/reflection coefficients, and Hawking radiation for a massive charged scalar field in the background of the Kerr-Newman black hole immersed in an asymptotically homogeneous magnetic field. There are two main effects: the Zeeman shift of the particle energy in the magnetic field and the difference of values of an electromagnetic potential between the horizon and infinity, i.e. the Faraday induction. We have shown that “turning on” the magnetic field induces a stronger energy-emission rate and leads to “recharging” of the black hole. Thus, a black hole immersed in a magnetic field evaporates much quicker, achieving thereby an extremal state in a shorter period of time. Quasinormal modes are moderately affected by the presence of a magnetic field which is assumed to be relatively small compared to the gravitational field of the black hole.

Article Text

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