Abstract
The quasinormal resonance frequency of the higher-dimensional Reissner–Nordström (RN) black hole due to charged massive scalar field perturbation is deduced analytically in the eikonal regime. The characteristic decay timescale of the charged massive scalar perturbation in the background of the higher-dimensional RN spacetime is then obtained. The result reveals that longlived charged massive scalar field can exist in higher-dimensional RN spacetime under a certain condition.
Highlights
The dynamics of the perturbation field in a spherically symmetric background spacetime is typically governed by a Schrodinger-like equation together with proper boundary conditons at the horizon and the spatial infinity [1]
The quasinormal modes (QNMs), which is described as oscillations of the form e−iωt, where ω is the quasinormal frequency, can be viewed as slowly decaying [2, 3] or highly damped [4, 5, 6] waves travelling around the black hole
Motivated by the uniqueness theorem, it is stated that static matter field cannot be hold by the asymptotically flat black hole in Einstein’s theory of gravitation by Wheeler’s no-hair conjecture [18] and the dynamic purturbation around a static black hole will go to be vanished [19, 20, 21]; in particular, the scalar [22], massive vector [23], and spinor [24] will be absorbed by the black hole or be scattered away from the black hole
Summary
The dynamics of the perturbation field in a spherically symmetric background spacetime is typically governed by a Schrodinger-like equation together with proper boundary conditons at the horizon and the spatial infinity [1]. Motivated by the uniqueness theorem, it is stated that static matter field cannot be hold by the asymptotically flat black hole in Einstein’s theory of gravitation by Wheeler’s no-hair conjecture [18] and the dynamic purturbation around a static black hole will go to be vanished [19, 20, 21]; in particular, the scalar [22], massive vector [23], and spinor [24] will be absorbed by the black hole or be scattered away from the black hole. Preprint submitted to Elsevier tions of the decaying timescale that the black hole takes to absorb or scatter the purturbations To this point, it has been analytically verified that the charged massive scalar field can be longlived (though vanished ) outside the fourdimensional Reissner–Nordstrom (RN) black hole, as the relaxation time will be infinity under a certain condition Mμ/qQ → 1− [28], where M(μ), Q(q) are respectively the mass and charge of the black hole (scalar field).
Published Version
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