The gravitational wave echoes from the black hole with three-form fields

Abstract

In this work, we study of massless three-form black hole, where the three-form fields are higher $p$-form gauge fields with $p=3$. These give rise to the Schwarzschild-de Sitter (Sch-dS)-like solution through an effective cosmological constant represented by $a_1$. We analyze this solution under gravitational perturbations and find that it exhibits a single-peak potential. For this case, no echoes are produced. Furthermore, we consider the massive case of the three-form fields by introducing a Stueckelberg field to restore gauge invariance and to investigate its effect on GWs at late times. In this case, the potential exhibits a double-peak structure, with the modified potential appearing beside the gravitational perturbation potential. We also examine the impact of the relevant parameters as well as the influence of the parameter $c_0$, which arises from the equation of motion of the Stueckelberg field. For a large value of $a_1$, the two peaks of the potentials are close together, while $c_0$ affects the amplitude and decay rate of the time-domain waveform, resulting in no echoes. For small values of $a_1$, the peaks of the potentials are widely separated and $c_0$ influences both the phase and the amplitude of the echoes. In addition, the quasinormal frequencies of the black hole are also calculated using both the WKB and Prony methods. As results, these provide a potential avenue for testing deviations from GR and probing possible signatures of quantum gravity through future GWs observations.