Quasinormal modes of Kerr-like black bounce spacetime
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arXiv
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| Autori principali: | , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2022
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| _version_ | 1866915695211577344 |
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| author | Yang, Yi Liu, Dong Övgün, Ali Long, Zheng-Wen Xu, Zhaoyi |
| author_facet | Yang, Yi Liu, Dong Övgün, Ali Long, Zheng-Wen Xu, Zhaoyi |
| contents | We investigate the quasinormal mode (QNM) spectrum of a Kerr-like black-bounce spacetime under massive scalar-field perturbations. Starting from the Kerr-like deformation of the Simpson--Visser black-bounce geometry, we derive the corresponding radial and angular equations and obtain the effective potential governing scalar perturbations. We show that the Kerr-like black-bounce spacetime inherits a characteristic double-peaked effective potential, analogous to the Schwarzschild-like black-bounce case, which is known to be associated with late-time echo signals. The QNM frequencies are computed by means of the Pöschl--Teller potential approximation and the semi-analytic WKB method (up to sixth order), and we demonstrate good agreement between these two approaches. We then analyze in detail how the QNM spectrum depends on the spin parameter $a$, the bounce parameter $p$ that interpolates between black-hole and wormhole geometries, and the scalar-field mass $μ$. Our results indicate that increasing either $a$ or $p$ lowers both the real frequency and the magnitude of the imaginary part, leading to longer-lived modes. Moreover, the mass of the scalar field has a non-negligible impact on the ringdown spectrum. These features suggest that rotating black-bounce geometries may leave distinct imprints in the ringdown phase of gravitational-wave signals, and motivate future studies of echoes and parameter estimation in the context of present and upcoming detectors. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2205_07530 |
| institution | arXiv |
| publishDate | 2022 |
| record_format | arxiv |
| spellingShingle | Quasinormal modes of Kerr-like black bounce spacetime Yang, Yi Liu, Dong Övgün, Ali Long, Zheng-Wen Xu, Zhaoyi General Relativity and Quantum Cosmology We investigate the quasinormal mode (QNM) spectrum of a Kerr-like black-bounce spacetime under massive scalar-field perturbations. Starting from the Kerr-like deformation of the Simpson--Visser black-bounce geometry, we derive the corresponding radial and angular equations and obtain the effective potential governing scalar perturbations. We show that the Kerr-like black-bounce spacetime inherits a characteristic double-peaked effective potential, analogous to the Schwarzschild-like black-bounce case, which is known to be associated with late-time echo signals. The QNM frequencies are computed by means of the Pöschl--Teller potential approximation and the semi-analytic WKB method (up to sixth order), and we demonstrate good agreement between these two approaches. We then analyze in detail how the QNM spectrum depends on the spin parameter $a$, the bounce parameter $p$ that interpolates between black-hole and wormhole geometries, and the scalar-field mass $μ$. Our results indicate that increasing either $a$ or $p$ lowers both the real frequency and the magnitude of the imaginary part, leading to longer-lived modes. Moreover, the mass of the scalar field has a non-negligible impact on the ringdown spectrum. These features suggest that rotating black-bounce geometries may leave distinct imprints in the ringdown phase of gravitational-wave signals, and motivate future studies of echoes and parameter estimation in the context of present and upcoming detectors. |
| title | Quasinormal modes of Kerr-like black bounce spacetime |
| topic | General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2205.07530 |