Long-lived resonances of massive scalar fields in the Reissner-Nordstr"om black-hole spacetime: Analytic treatment in the large-mass regime
gr-qc, astro-ph.HE, hep-th
Submitted: 2025-11-13
Updated: 2025-11-13
Comments: 9 pages
Journal ref: Phys. Lett. B 874, 140228 (2026)
License: http://creativecommons.org/licenses/by/4.0/
The gist: The physical and mathematical properties of the composed Reissner-Nordström-black-hole-massive-scalar-field system are studied analytically in the dimensionless large-mass Mμ 1 regime [here M,μ
Terminology
Abstract
The physical and mathematical properties of the composed Reissner-Nordström-black-hole-massive-scalar-field system are studied analytically in the dimensionless large-mass Mμ 1 regime [here M,μ are respectively the mass of the central black hole and the proper mass of the scalar field]. It is proved that, for a given value Q Q/M of the dimensionless charge parameter of the central black hole, the system is characterized by the presence of quasi-resonances, linearized perturbation modes with arbitrarily long lifetimes. In particular, using analytical techniques, we determine the black-hole-field critical mass spectrum Mμ crit(Q) which characterizes the long-lived resonances of the composed physical system.
Sources
- Bohr's Correspondence Principle and The Area Spectrum of Quantum Black Holes
- Kerr black hole quasinormal frequencies
- Intermediate Asymptotics of the Kerr Quasinormal Spectrum
- Selection Rules for Black-Hole Quantum Transitions
- Analytic Study of Rotating Black-Hole Quasinormal Modes
- Near-Extreme Black Holes and the Universal Relaxation Bound
- Purely imaginary polar resonances of rapidly-rotating Kerr black holes
- Hairy Black Holes and Null Circular Geodesics
- Stationary Scalar Clouds Around Rotating Black Holes
- Stationary resonances of rapidly-rotating Kerr black holes
- Kerr-Newman black holes with stationary charged scalar clouds
- Rotating black holes can have short bristles
- Analytic treatment of the black-hole bomb
- On the instability regime of the rotating Kerr spacetime to massive scalar perturbations
- A no-short scalar hair theorem for rotating Kerr black holes
- Spinning Kerr black holes with stationary massive scalar clouds: The large-coupling regime
- Spinning boson stars and Kerr black holes with scalar hair: the effect of self-interactions
- Quantum and classical aspects of scalar and vector fields around black holes
- Late-Time Tails in Gravitational Collapse of a Self-Interacting (Massive) Scalar-Field and Decay of a Self-Interacting Scalar Hair
- Late-Time Evolution of Realistic Rotating Collapse and The No-Hair Theorem
Related papers
- Listening to the Horizon: Probing Near-Horizon Reflectivity with GW250114
- A Pairwise Surrogate for Gravitational-Wave Spectra from Highly Relativistic Vacuum Bubble Collisions
- Tests of General Relativity with Einstein Telescope
- A weakly modelled view of the joint compact-binary mass plane: population structure and spectral-siren cosmology
- Unitary quantum matter-bounce in a universe with a positive cosmological constant
- Nonreciprocal black holes with primary hair in beyond Horndeski gravity: Exact solutions and stability