Perturbative Renormalisation Group Improved Black Hole Solution and its Quasinormal Modes

TL;DR

This paper constructs a perturbative black hole solution influenced by renormalization group effects and analyzes its quasinormal modes using various numerical methods, providing insights into black hole perturbations in different cosmological backgrounds.

Contribution

It introduces a novel RG-improved perturbative black hole solution and compares multiple methods for computing its quasinormal modes in SdS and SAdS spacetimes.

Findings

QNM frequencies depend on the free parameter of the solution.

Good agreement between different numerical methods for QNM calculation.

Waveform reconstruction matches time-domain profiles accurately.

Abstract

In this work, we construct a perturbative black hole (BH) solution motivated by renormalization group (RG) improvement and investigate the quasinormal modes (QNMs) of the BH under scalar field perturbations in both Schwarzschild-de Sitter (SdS) and Schwarzschild-anti-de Sitter (SAdS) backgrounds. To compute the QNMs in the SdS spacetime, we employ the 6th-order Pad\'e-averaged WKB approximation method, while for the SAdS background we utilize the direct shooting method. We examine the dependence of the QNM frequencies on the free parameter of the solution. Furthermore, we analyze the time evolution of a scalar field perturbation around the BH and present the corresponding time-domain profiles. The QNMs are also extracted from the time-domain data using the matrix pencil method. Using the extracted QNM frequencies, we reconstruct the waveform and compare it with the original time-domain profile, finding good agreement between the two. The QNM frequencies obtained from the 6th-order Pad\'e-averaged WKB method and the time-domain analysis in the SdS background, as well as those obtained from the direct shooting method and time-domain analysis in the SAdS spacetime, show very good consistency.