Abstract
This study investigates the stability of higher-dimensional singly rotating Myers-Perry–de Sitter (MP–dS) black holes against scalar field perturbations. The phase spaces of MP-dS black holes with one spin parameter are discussed. Additionally, the quasinormal modes (QNMs) of MP-dS black holes are calculated via the asymptotic iteration method and sixth-order Wentzel–Kramers–Brillouin approximation. For near-extremal MP-dS black holes, the event horizon may be considerably close to the cosmological horizon. In such cases, the Pöschl–Teller technique yields an accurate analytic formula for the QNMs. It is found that when the spin parameter of a black hole increases, the scalar perturbation modes oscillate at higher frequencies and decay faster. Furthermore, the MP-dS black hole with a single rotation is found to be stable under perturbation.
Highlights
Black holes are compact objects that describe the final state of massive stellar bodies in our universe
Our numerical scheme is based on the improved asymptotic iteration method (AIM) discussed in the previous section
The quasinormal modes (QNMs) will be computed by solving the radial equation with the analytic formula for the angular eigenvalue Ak j m
Summary
Black holes are compact objects that describe the final state of massive stellar bodies in our universe. With non-vanishing cosmological constants, multidimensional black holes are shown to be stable [11], including the RN-AdS under gravitational perturbations [12]. It is extended to a version that includes the posknown study of classical stability of higher-dimensional itive cosmological constant [28,29] Through this positive rotating bodies focuses on the Myers-Perry (MP) black cosmological constant, the asymptotic geometry of the black hole. For a positive cosmological constant, the Kerr-dS black holes in general relativity are gravitationally stable [25], while their counterparts in scalar tensor theory suffer from. The black hole phase spaces are determined by the cosmological constant and spin parameter.
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