Quantum corrected black holes: quasinormal modes, scattering, shadows. (arXiv:1912.10582v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Konoplya_R/0/1/0/all/0/1">R. A. Konoplya</a>
The spherically symmetric deformation of the Schwarzschild solution owing to
the quantum corrections to gravity is known as Kazakov-Solodukhin black-hole
metric. Neglecting non-spherical deformations of the background the problem was
solved non-perturbatively. Here we analyze the basic characteristics of this
geometry, such as: quasinormal modes and grey-body factors of fields of various
spin and shadow cast by this black hole. The WKB approach and time-domain
integration method, which we used for calculation of quasinormal modes, are in
a good concordance. The analytical formula for quasinormal modes is deduced in
the eikonal regime. The radius of shadow is decreasing when the quantum
deformation is turned on.
The spherically symmetric deformation of the Schwarzschild solution owing to
the quantum corrections to gravity is known as Kazakov-Solodukhin black-hole
metric. Neglecting non-spherical deformations of the background the problem was
solved non-perturbatively. Here we analyze the basic characteristics of this
geometry, such as: quasinormal modes and grey-body factors of fields of various
spin and shadow cast by this black hole. The WKB approach and time-domain
integration method, which we used for calculation of quasinormal modes, are in
a good concordance. The analytical formula for quasinormal modes is deduced in
the eikonal regime. The radius of shadow is decreasing when the quantum
deformation is turned on.
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