Greybody radiation and quasinormal modes of Kerr-like black hole in Bumblebee gravity model

Abstract

In the framework of the Lorentz symmetry breaking (LSB), we investigate the quasinormal modes (QNMs) and the greybody factors (GFs) of the Kerr-like black hole spacetime obtained from the bumblebee gravity model. In particular, we analyze the scalar and fermionic perturbations of the black hole within the framework of both semi-analytic WKB method and the time domain approach. The impacts of the LSB on the bosonic/fermionic QNMs and GFs of the Kerr-like black hole are investigated in detail. The obtained results are graphically depicted and discussed.

Comment on “Greybody radiation and quasinormal modes of Kerr-like black hole in Bumblebee gravity model”

“…Firstly, the complete rotational Kerr-like black hole solution used in [1] does not satisfy the equation of motion for the bumblebee field, as it already was discussed in Ref. [2], although that has not been shown explicitly.…”

“…The paper "Greybody radiation and quasinormal modes of Kerr-like black hole in Bumblebee gravity model" [1] is an interesting work that seeks to establish a significant relationship between two important realms of the current research on astrophysics and high energy physics, namely, semi-classical gravitation associated to rotating black holes and Lorentz symmetry breakdown. This latter embodies features that are beyond the standard model of elementary particles and fundamental interactions.…”

Superradiant instability of the Kerr-like black hole in Einstein-bumblebee gravity

“…As a more practical scenario, axial symmetry in Einsteinbumblebee gravity is investigated and an exact Kerr-like black hole is obtained by C. Ding et al [17]. The studies related to this solution have been extended to the effects of the matter and light around it [18][19][20]. Furthermore, a Kerr-Sen-like black hole has also been found [21].…”

Quasinormal Frequencies of a Two-Dimensional Asymptotically Anti-de Sitter Black Hole of the Dilaton Gravity Theory

“…Furthermore, in 2D spacetimes the equations of motion for classical fields simplify and we can study in more detail several physical phenomena, for example, the way in which a 2D black hole reacts when it is perturbed. The QNFs of 2D spacetimes have been studied in recent times (Li et al, 2001;Kettner et al, 2004;Becar et al, 2007;Zelnikov, 2008;López-ortega, 2009;Becar et al, 2010;López-ortega, 2011;López-Ortega and Vega-Acevedo, 2011;Cordero et al, 2012;Myung and Moon, 2012;Estrada-Jiménez et al, 2013;Stetsko, 2017;Jusufi et al, 2018;Sakallı et al, 2018;Mirbabayi, 2020;Bhattacharjee et al, 2021;Kanzi and Sakallı, 2021;Sakalli and Tokgöz Hyusein, 2021). Exact results for the QNFs have previously found (Li et al, 2001;Kettner et al, 2004;Becar et al, 2007;Zelnikov, 2008;López-ortega, 2009;Becar et al, 2010;López-ortega, 2011;López-Ortega and Vega-Acevedo, 2011;Cordero et al, 2012;Myung and Moon, 2012;Estrada-Jiménez et al, 2013;Stetsko, 2017;Jusufi et al, 2018;Sakallı et al, 2018;Mirbabayi, 2020;Bhattacharjee et al, 2021;Kanzi and Sakallı, 2021;Sakalli and Tokgöz Hyusein, 2021), but for some asymptotically adS 2D backgrounds a numerical calculation is necessary (Corder...…”