Quasinormal mode and spectroscopy of a Schwarzschild black hole surrounded by a cloud of strings in Rastall gravity

TL;DR

This paper investigates a Schwarzschild black hole with a string cloud in Rastall gravity, analyzing its quasinormal modes, thermodynamics, and potential dark energy implications, revealing how Rastall parameters influence these properties.

Contribution

It provides a new exact solution for a black hole with a string cloud in Rastall gravity and explores its quasinormal modes, thermodynamics, and dark energy connection.

Findings

Increased string parameter $a$ slows gravitational wave decay.

Area spectrum is equally spaced, matching Einstein gravity.

Entropy spectrum depends on Rastall parameter $eta$.

Abstract

We obtain the solution of a static spherically symmetric black hole surrounded by a cloud of strings in Rastall gravity and study the influence of the parameter $a$ associated with strings on the event horizon and the Hawking temperature. Through analyzing the black hole metric, we find that the static spherically symmetric black hole solution surrounded by a cloud of strings in Rastall gravity can be transformed into the static spherically symmetric black hole solution surrounded by quintessence in Einstein gravity when the parameter $\beta$ of Rastall gravity is positive, which provides a possibility for the string fluid to be a candidate of dark energy. We use the method of Regge and Wheeler together with the high order WKB-Pad\'{e} approximation to calculate the quasinormal mode frequencies of the odd parity gravitational perturbation and simultaneously apply the unstable null geodesics of black holes to compute the quasinormal mode frequencies at the eikonal limit for this black hole model. The results show that the increase of the parameter $a$ makes the gravitational wave decay slowly in Rastall gravity. In addition, we utilize two methods, which are based on the adiabatic invariant integral and the periodic property of outgoing waves, respectively, to derive the area spectrum and entropy spectrum of the black hole model. The results show that the area spectrum and entropy spectrum are equidistant spaced. The former is same as the case of Einstein gravity, while the latter is different, depending on the Rastall parameter $\beta$.