Abstract
Abstract Kerr black holes, characterized solely by their mass and angular momentum, are considered the predominant type in the universe. Recent studies, however, suggest that black holes may possess additional parameters, known as “hair”. This paper investigates the quasinormal modes (QNMs) of rotating hairy black holes in asymptotically flat spacetimes using the continued fraction method to analyze their stability. Our results demonstrate that the introduction of hair parameters modifies the QNM frequencies, indicating a nuanced stability profile that reduces to the classical Kerr solution under specific conditions. These findings provide new insights into the dynamic properties of hairy black holes and their potential astrophysical implications.
Published Version
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