Quasinormal Modes of Black holes in the generalized Schwarzschild-de Sitter solution of $f(R)$ gravity

Abstract

We analyze scalar, vector, and {axial} tensor perturbations in a Schwarzschild-type static spherically symmetric solution of modified $f(R)$ gravity. This solution differs from the Schwarzschild metric of general relativity through the presence of a linearly growing term and a logarithmic correction, and it depends on four integration constants. Using the higher-order Wentzel-Kramers-Brillouin (WKB) approximation and an analytical method, we calculate the quasinormal modes (QNMs) for all three types of perturbations. Our results show that, for appropriately chosen parameter values, the QNMs closely match those of the Schwarzschild black hole. In particular, the model parameter $A$ produces a nonlinear increase in both the oscillation frequency and damping rate of ringdown gravitational waves. A similar effect arises for the parameter $\eta$ when $A$ is small, while for larger $A$ values the effects are opposite, where the scalar perturbations display a distinct deviation compared to the vector and {axial} tensor cases. Contour plots of QNMs in the parameter space support these findings. Finally, time-domain profiles are obtained to illustrate the dynamical evolution of the gravitational wave signal.

arXiv comment25 pages, 22 figures, published in Physical Review D

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