Quasi-normal Modes of Static Spherically Symmetric Black Holes in $f(R)$ Theory

Abstract

We study the quasi-normal modes (QNMs) of static, spherically symmetric black holes in $f(R)$ theories. We show how these modes in theories with non-trivial $f(R)$ are fundamentally different from those in General Relativity. In the special case of $f(R)=\alpha R^2$ theories, it has been recently argued that iso-spectrality between scalar and vector modes breaks down. Here, we show that such a break down is quite general across all $f(R)$ theories, as long as they satisfy $f^{\prime \prime }(0)/(1+f^{\prime \prime }(0))\ne 0$, where a prime denotes derivative of the function with respect to its argument. We specifically discuss the origin of the breaking of isospectrality. We also show that along with this breaking the QNMs receive a correction that arises when $f^{\prime \prime }(0)/(1+f^{\prime }(0))\ne 0$ owing to the inhomogeneous term that it introduces in the mode equation. We discuss how these differences affect the "ringdown" phase of binary black hole mergers and the possibility of constraining $f(R)$ models with gravitational-wave observations. We also find that even though the iso-spectrality is broken in $f(R)$ theories, in general, nevertheless in the corresponding scalar-tensor theories in the Einstein frame it is unbroken.

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