Quasinormal modes for a non-minimally coupled scalar field in a five-dimensional Einstein-power-Maxwell background

Abstract

We study the propagation of massless scalar fields non-minimally coupled to gravity in the background of five-dimensional Einsteinpower-Maxwell black holes, and by using the WKB and the pseudospectral Chebyshev methods we obtain the quasinormal frequencies (QNFs), which allow to show the existence of stable and unstable QNFs depending on the exponent k of the nonlinearity electrodynamics. Thus, for k < 1, there are stables and unstables QNFs depending on the size of the black hole and on the angular number, while that for k > 1, the QNFs are complex and stable, and also the longest-lived modes are the ones with higher angular number.

Regular Charged Black Holes, Energy Conditions, and Quasinormal Modes

“…Now, taking advantage of the Klein-Gordon equation (see Refs. [37][38][39][40][41][42][43] and references therein)…”

Orbits of light rays in (1＋2)-dimensional Einstein–power–Maxwell gravity: Exact analytical solution to the null geodesic equations

“…This is to be contrasted to what happens in the case of the standard Reissner-Nordström solution [48]. Finally, a toy model that generalizes Maxwell's theory in a straightforward manner leads to the so called Einstein-power-Maxwell (EpM) theory [49][50][51][52][53][54][55][56][57][58][59][60][61][62], described by a Lagrangian density of the form L(F ) ∼ F k , where F is the Maxwell invariant, and k is an arbitrary rational number. One of the advantages of EpM theory is that the nice conformal properties of the four-dimensional Maxwell's theory are preserved in any number of space-time dimensionality D, provided that the power k is chosen to be k = D/4, as it is easy to verify that for this particular value the electromagnetic stress-energy tensor becomes traceless.…”

Construction of a traversable wormhole from a suitable embedding function

“…The response of a wormhole to perturbations is dominated by damped oscillations called quasi-normal modes. The computation of the QNM modes can be performed through a variety of methods (for an incomplete list see [26][27][28][29][30][31][32][33][34][35][36][37][38][39][40][41][42] and references therein, for example). However, in this work, we shall use the recently developed WKB approximation to the 13th order which has brought the attention of the community [43].…”