Tunneling method for Hawking radiation in the Nariai case

Abstract

Abstract. We revisit the tunneling picture for the Hawking effect in light of the charged Nariai manifold, because this general relativistic solution, which displays two horizons, provides the bonus to allow the knowledge of exact solutions of the field equations. We first perform a revisitation of the tunneling ansatz in the framework of particle creation in external fieldsà la Nikishov, which corroborates the interpretation of the semiclassical emission rate Γ emission as the conditional probability rate for the creation of a couple of particles from the vacuum. Then, particle creation associated with the Hawking effect on the Nariai manifold is calculated in two ways. On the one hand, we apply the Hamilton-Jacobi formalism for tunneling, in the case of a charged scalar field on the given background. On the other hand, the knowledge of the exact solutions for the Klein-Gordon equations on Nariai manifold, and their analytic properties on the extended manifold, allow us a direct computation of the flux of particles leaving the horizon, and, as a consequence, we obtain a further corroboration of the semiclassical tunneling picture from the side of S-matrix formalism.

Festina lente:1 EFT constraints from charged black hole evaporation in de Sitter

“…Previous studies of black hole evaporation in de Sitter [86,88,90,[92][93][94][95][96]118] concerned only the case where no charged particles are present, so the black hole can lose mass, but not charge (modulo non-perturbative effects). We have worked out how large de Sitter black holes evaporate, depending on the spectrum of charged particles in the theory.…”

“…The problem was worked out early on for neutral black holes [86][87][88][89] and charged ones in the absence of charged particles [90,91]. While there are some works that discuss emission of charged particles by black holes in de Sitter [92][93][94][95][96], we were unable to find a reference that described in detail how the mass and charge of the black hole deplete. We do this in the present paper, following an approach similar to [97], although the details are more complicated due to the lack of an asymptotically flat region.…”