Abstract
It is known that the nonstrictly thermal character of the Hawking radiation spectrum harmonizes Hawking radiation with black hole (BH) quasi-normal modes (QNM). This paramount issue has been recently analyzed in the framework of both Schwarzschild BHs (SBH) and Kerr BHs (KBH). In this assignment, we generalize the analysis to the framework ofnonextremalReissner-Nordström BHs (RNBH). Such a generalization is important because in both Schwarzschild and Kerr BHs an absorbed (emitted) particle has only mass. Instead, in RNBH the particle has charge as well as mass. In doing so, we expose that, for the RNBH, QNMs can be naturally interpreted in terms of quantum levels for both particle emission and absorption. Conjointly, we generalize some concepts concerning the RNBH's “effective states.”
Highlights
A Reissner-Nordstrom black hole (BH) (RNBH) of mass M is identical to a Schwarzschild BHs (SBH) of mass M except that a RNBH has the nonzero charge quantity Q
It is known that the countable character of successive emissions of Hawking quanta which is a consequence of Advances in High Energy Physics the nonstrictly thermal character of the Hawking radiation spectrum generates a natural correspondence between Hawking radiation and BH quasi-normal modes (QNM) [3,4,5,6,7]
We began our paper by summarizing some basic similarities and differences between SBHs and RNBHs in terms of charge and horizon radii
Summary
A RNBH of mass M is identical to a SBH of mass M except that a RNBH has the nonzero charge quantity Q.
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