Black hole perturbations in Maxwell-Horndeski theories

Abstract

We study the linear stability of black holes in Maxwell-Horndeski theories where a U (1) gaugeinvariant vector field is coupled to a scalar field with the Lagrangian of full Horndeski theories. The perturbations on a static and spherically symmetric background can be decomposed into oddand even-parity modes under the expansion of spherical harmonics with multipoles l. For l ≥ 2, the odd-parity sector contains two propagating degrees of freedom associated with the gravitational and vector field perturbations. In the even-parity sector, there are three dynamical perturbations arising from the scalar field besides the gravitational and vector field perturbations. For these five propagating degrees of freedom, we derive conditions for the absence of ghost/Laplacian stabilities along the radial and angular directions. We also discuss the stability of black holes for l = 0 and l = 1, in which case no additional conditions are imposed to those obtained for l ≥ 2. We apply our general results to Einstein-Maxwell-dilaton-Gauss-Bonnet theory and Einstein-Born-Infeld-dilaton gravity and show that hairy black hole solutions present in these theories can be consistent with all the linear stability conditions. In regularized four-dimensional Einstein-Gauss-Bonnet gravity with a Maxwell field, however, exact charged black hole solutions known in the literature are prone to instabilities of even-parity perturbations besides a strong coupling problem with a vanishing kinetic term of the radion mode.

Linear stability of vector Horndeski black holes

“…where the summation of Y l (θ) with respect to the multipoles l is omitted, and we use the notations Y l,θ = dY l /dθ and Y l,θθ = d 2 Y l /dθ 2 . The vector field A µ has the following perturbed components [85]…”